diff --git a/.github/workflows/validate.yml b/.github/workflows/validate.yml new file mode 100644 index 0000000..d20838d --- /dev/null +++ b/.github/workflows/validate.yml @@ -0,0 +1,18 @@ +name: validate + +on: + push: + branches: [main] + pull_request: + +jobs: + validate: + runs-on: ubuntu-latest + steps: + - uses: actions/checkout@v4 + - uses: actions/setup-python@v5 + with: + python-version: "3.11" + - run: pip install pytest + - run: make validate + - run: make test diff --git a/.gitignore b/.gitignore index 5fe3efb..47d2cad 100644 --- a/.gitignore +++ b/.gitignore @@ -34,6 +34,7 @@ desktop.ini *.swp *~ __pycache__/ +.pytest_cache/ *.pyc # LaTeX build artefacts @@ -48,4 +49,4 @@ __pycache__/ *.toc # Exception — the wiki's own log.md is text and must be tracked -!lensing_wiki/log.md +!wiki/*/log.md diff --git a/AGENTS.md b/AGENTS.md index 2d2655e..420ec5d 100644 --- a/AGENTS.md +++ b/AGENTS.md @@ -15,13 +15,31 @@ packaging, tooling, and workflow tasks. When you do read: 1. **Index first.** Start at [`index.md`](index.md), then the relevant - sub-wiki's own `index.md` (`lensing_wiki/`, `smbh_wiki/`, `cti_wiki/`, - `methods_wiki/`, `galaxies_wiki/`). + sub-wiki's own `index.md` (`wiki/lensing/`, `wiki/smbh/`, `wiki/cti/`, + `wiki/methods/`, `wiki/galaxies/`). 2. **Then at most 2–3 pages.** Read only the concept/entity/source pages the index points you to. **Never bulk-load a sub-wiki.** 3. **Do not couple to the internal layout** — reach pages through the indexes, not hard-coded paths. +## The write contract (layout rules) + +The repo has exactly **two content homes**, enforced by +`make validate-structure` (CI runs it on every push/PR): + +- **`wiki//`** — every sub-wiki, following the shared schema in + [`wiki/CLAUDE.md`](wiki/CLAUDE.md). New sub-wikis are added beside the + existing ones, never at the repo root. +- **`bibliography/`** — the *only* place BibTeX lives. One canonical file + (`pyautomemory.bib`) plus `bibkey_aliases.yaml`; never add loose `.bib` + files anywhere else. + +**Source PDFs live off-repo.** Never commit a paper (PDF/HTML, with or +without a file extension) — read it, stub it in the right +`wiki//sources/*.md`, add its canonical entry to `bibliography/`, +and run `make validate`. Unrecognised top-level files/folders fail the lint; +the allowlist is in `scripts/validate_structure.py`. + ## What does NOT live here - **Operational history** — what the organism *did* (prior tasks, decisions, diff --git a/CTI/Hall1952Theory b/CTI/Hall1952Theory deleted file mode 100755 index d1f90b3..0000000 --- a/CTI/Hall1952Theory +++ /dev/null @@ -1,69 +0,0 @@ - - Physical Review Journals Archive

Physical Review Journals Archive

Published by the American Physical Society

Authorization Required

Individual Subscribers

Cancel

Other Options

Search

Article Lookup

Paste a citation or DOI
Enter a citation
×
\ No newline at end of file diff --git a/DarkMatterModels/Navarro1996StructureCDMHalos.563N b/DarkMatterModels/Navarro1996StructureCDMHalos.563N deleted file mode 100755 index 3fc8101..0000000 Binary files a/DarkMatterModels/Navarro1996StructureCDMHalos.563N and /dev/null differ diff --git a/Euclid/Paykari2020.bib b/Euclid/Paykari2020.bib deleted file mode 100755 index c64d131..0000000 --- a/Euclid/Paykari2020.bib +++ /dev/null @@ -1,18 +0,0 @@ -@ARTICLE{2020A&A...635A.139E, - author = {{Euclid Collaboration} and {Paykari}, P. and {Kitching}, T. and {Hoekstra}, H. and {Azzollini}, R. and {Cardone}, V.~F. and {Cropper}, M. and {Duncan}, C.~A.~J. and {Kannawadi}, A. and {Miller}, L. and {Aussel}, H. and {Conti}, I.~F. and {Auricchio}, N. and {Baldi}, M. and {Bardelli}, S. and {Biviano}, A. and {Bonino}, D. and {Borsato}, E. and {Bozzo}, E. and {Branchini}, E. and {Brau-Nogue}, S. and {Brescia}, M. and {Brinchmann}, J. and {Burigana}, C. and {Camera}, S. and {Capobianco}, V. and {Carbone}, C. and {Carretero}, J. and {Castander}, F.~J. and {Castellano}, M. and {Cavuoti}, S. and {Charles}, Y. and {Cledassou}, R. and {Colodro-Conde}, C. and {Congedo}, G. and {Conselice}, C. and {Conversi}, L. and {Copin}, Y. and {Coupon}, J. and {Courtois}, H.~M. and {Da Silva}, A. and {Dupac}, X. and {Fabbian}, G. and {Farrens}, S. and {Ferreira}, P.~G. and {Fosalba}, P. and {Fourmanoit}, N. and {Frailis}, M. and {Fumana}, M. and {Galeotta}, S. and {Garilli}, B. and {Gillard}, W. and {Gillis}, B.~R. and {Giocoli}, C. and {Graci{\'a}-Carpio}, J. and {Grupp}, F. and {Hormuth}, F. and {Ili{\'c}}, S. and {Israel}, H. and {Jahnke}, K. and {Keihanen}, E. and {Kermiche}, S. and {Kilbinger}, M. and {Kirkpatrick}, C.~C. and {Kubik}, B. and {Kunz}, M. and {Kurki-Suonio}, H. and {Laureijs}, R. and {Le Mignant}, D. and {Ligori}, S. and {Lilje}, P.~B. and {Lloro}, I. and {Maciaszek}, T. and {Maiorano}, E. and {Marggraf}, O. and {Markovic}, K. and {Martinet}, N. and {Marulli}, F. and {Massey}, R. and {Mauri}, N. and {Medinaceli}, E. and {Mei}, S. and {Mellier}, Y. and {Meneghetti}, M. and {Metcalf}, R.~B. and {Moresco}, M. and {Moscardini}, L. and {Munari}, E. and {Neissner}, C. and {Nichol}, R.~C. and {Niemi}, S. and {Nutma}, T. and {Padilla}, C. and {Paltani}, S. and {Pasian}, F. and {Pettorino}, V. and {Pires}, S. and {Polenta}, G. and {Raison}, F. and {Renzi}, A. and {Rhodes}, J. and {Romelli}, E. and {Roncarelli}, M. and {Rossetti}, E. and {Saglia}, R. and {Sakr}, Z. and {S{\'a}nchez}, A.~G. and {Sapone}, D. and {Scaramella}, R. and {Schneider}, P. and {Schrabback}, T. and {Scottez}, V. and {Secroun}, A. and {Serrano}, S. and {Sirignano}, C. and {Sirri}, G. and {Stanco}, L. and {Starck}, J. -L. and {Sureau}, F. and {Tallada-Cresp{\'\i}}, P. and {Taylor}, A. and {Tenti}, M. and {Tereno}, I. and {Toledo-Moreo}, R. and {Torradeflot}, F. and {Valenziano}, L. and {Vannier}, M. and {Vassallo}, T. and {Zoubian}, J. and {Zucca}, E.}, - title = "{Euclid preparation. VI. Verifying the performance of cosmic shear experiments}", - journal = {\aap}, - keywords = {gravitational lensing: weak, Astrophysics - Cosmology and Nongalactic Astrophysics}, - year = 2020, - month = mar, - volume = {635}, - eid = {A139}, - pages = {A139}, - doi = {10.1051/0004-6361/201936980}, -archivePrefix = {arXiv}, - eprint = {1910.10521}, - primaryClass = {astro-ph.CO}, - adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...635A.139E}, - adsnote = {Provided by the SAO/NASA Astrophysics Data System} -} - diff --git a/Hubble1926.321H b/Hubble1926.321H deleted file mode 100755 index 1f0eb92..0000000 Binary files a/Hubble1926.321H and /dev/null differ diff --git a/LightProFFits/devVaucoleuris1948pdf b/LightProFFits/devVaucoleuris1948pdf deleted file mode 100755 index e5d5d1b..0000000 Binary files a/LightProFFits/devVaucoleuris1948pdf and /dev/null differ diff --git a/Makefile b/Makefile index ee179a6..d1a3c34 100644 --- a/Makefile +++ b/Makefile @@ -1,4 +1,12 @@ -.PHONY: validate-literature-citations +.PHONY: validate validate-literature-citations validate-structure test + +validate: validate-literature-citations validate-structure validate-literature-citations: python scripts/validate_literature_citations.py + +validate-structure: + python scripts/validate_structure.py + +test: + python -m pytest tests/ -q diff --git a/Medical/Liu2024CUPRCT.htm b/Medical/Liu2024CUPRCT.htm deleted file mode 100755 index cc27673..0000000 --- a/Medical/Liu2024CUPRCT.htm +++ /dev/null @@ -1,929 +0,0 @@ - - - - Security verification - - - - - - - - - - - - - - - - - - - \ No newline at end of file diff --git a/README.md b/README.md index aa322d9..c60b2c1 100644 --- a/README.md +++ b/README.md @@ -17,20 +17,20 @@ The sub-wikis (self-contained, shared schema): | Wiki | Covers | |------|--------| -| [`lensing_wiki/`](lensing_wiki/index.md) | strong gravitational lensing (the primary wiki) | -| [`smbh_wiki/`](smbh_wiki/index.md) | supermassive black holes, binaries, recoil, GW background | -| [`cti_wiki/`](cti_wiki/index.md) | charge transfer inefficiency, Euclid VIS calibration | -| [`methods_wiki/`](methods_wiki/index.md) | Bayesian inference, samplers, deep learning, simulations | -| [`galaxies_wiki/`](galaxies_wiki/index.md) | galaxy formation and evolution | +| [`wiki/lensing/`](wiki/lensing/index.md) | strong gravitational lensing (the primary wiki) | +| [`wiki/smbh/`](wiki/smbh/index.md) | supermassive black holes, binaries, recoil, GW background | +| [`wiki/cti/`](wiki/cti/index.md) | charge transfer inefficiency, Euclid VIS calibration | +| [`wiki/methods/`](wiki/methods/index.md) | Bayesian inference, samplers, deep learning, simulations | +| [`wiki/galaxies/`](wiki/galaxies/index.md) | galaxy formation and evolution | [`bibliography/`](bibliography/README.md) holds the canonical BibTeX metadata every wiki cites against; [`reading-queue.md`](reading-queue.md) is what's waiting to be read and filed. New knowledge updates the metadata and the claim support together, then passes -`make validate-literature-citations`. +`make validate`. The wiki schema is defined in -[`lensing_wiki/CLAUDE.md`](lensing_wiki/CLAUDE.md) and inherited by every +[`wiki/CLAUDE.md`](wiki/CLAUDE.md) and inherited by every sub-wiki. How agents should read this repo: [AGENTS.md](AGENTS.md). The organism this repo is the Memory of: [PyAutoBrain/ORGANISM.md](https://github.com/PyAutoLabs/PyAutoBrain/blob/main/ORGANISM.md), diff --git a/bibliography/README.md b/bibliography/README.md index cbb18c7..20e21fd 100644 --- a/bibliography/README.md +++ b/bibliography/README.md @@ -1,26 +1,27 @@ # Canonical PyAutoMemory bibliography -`pyautomemory.bib` is the canonical metadata layer shared by every `*_wiki/` in this +`pyautomemory.bib` is the canonical metadata layer shared by every sub-wiki under `../wiki/` in this repository. Wiki source entries explain which claims papers support; the BibTeX file records citation metadata and canonical keys. Keep PDFs, local paths, abstracts, and long paper summaries out of both layers. -> Renamed from `pyautopaper.bib` (when this repo was PyAutoPaper). The old path -> `pyautopaper.bib` remains as a symlink to `pyautomemory.bib` for backwards -> compatibility; new references should use `pyautomemory.bib`. +> Renamed from `pyautopaper.bib` (when this repo was PyAutoPaper); the back-compat +> `pyautopaper.bib` symlink was retired in 2026-07 once nothing referenced it. -The initial canonical file prioritises `library.bib`. Entries with new keys from the other +The initial canonical file prioritised `library.bib`. Entries with new keys from the other tracked legacy `.bib` files were added, but conflicting records never replaced the -`library.bib` entry. The root-level files remain legacy inputs and project bibliographies; -new canonical metadata belongs here. +`library.bib` entry. The legacy root-level `.bib` files were deleted in 2026-07 after a +key-level audit confirmed every unique key already existed here (they remain in git +history). All canonical metadata lives in this folder; loose `.bib` files must not be +added elsewhere in the repo. ## Adding a paper 1. Verify the paper from an authoritative public record or the paper itself. 2. Search `pyautomemory.bib` by DOI, arXiv ID, and title. Reuse the existing canonical key; otherwise add verified metadata under a unique, stable author-year key. -3. Add a compact section to the relevant `_wiki/sources/*.md` using the inherited - schema in [`../lensing_wiki/CLAUDE.md`](../lensing_wiki/CLAUDE.md). +3. Add a compact section to the relevant `../wiki//sources/*.md` using the inherited + schema in [`../wiki/CLAUDE.md`](../wiki/CLAUDE.md). 4. Add concept/entity links only where the paper materially supports existing text. 5. Run `make validate-literature-citations`. diff --git a/bibliography/pyautomemory.bib b/bibliography/pyautomemory.bib index da6b05e..24ebfbf 100644 --- a/bibliography/pyautomemory.bib +++ b/bibliography/pyautomemory.bib @@ -16547,3 +16547,13 @@ @article{Acebron2024 url = {https://arxiv.org/abs/2410.01883}, year = {2024} } + +@article{Hall1952, + author = {Hall, R. N.}, + doi = {10.1103/PhysRev.87.387}, + journal = {Physical Review}, + pages = {387}, + title = {{Electron-Hole Recombination in Germanium}}, + volume = {87}, + year = {1952} +} diff --git a/bibliography/pyautopaper.bib b/bibliography/pyautopaper.bib deleted file mode 120000 index 19674bd..0000000 --- a/bibliography/pyautopaper.bib +++ /dev/null @@ -1 +0,0 @@ -pyautomemory.bib \ No newline at end of file diff --git a/cooper.bib b/cooper.bib deleted file mode 100755 index ef45cfe..0000000 --- a/cooper.bib +++ /dev/null @@ -1,173 +0,0 @@ -@STRING{apj = "ApJ"} -@STRING{mnras = "MNRAS"} - -@article{Amorisco:2017aa, - Author = {{Amorisco}, N.~C.}, - Journal = {\mnras}, - Month = jan, - Pages = {2882-2895}, - Title = {{Contributions to the accreted stellar halo: an atlas of stellar deposition}}, - Volume = 464, - Year = 2017} - -@article{Baugh:1996aa, - Author = {{Baugh}, C.~M. and {Cole}, S. and {Frenk}, C.~S.}, - Journal = {\mnras}, - Month = dec, - Pages = {1361-1378}, - Title = {{Evolution of the Hubble sequence in hierarchical models for galaxy formation}}, - Volume = 283, - Year = 1996} - -@article{Bower:2016aa, - Author = {{Bower}, R. and {Schaye}, J. and {Frenk}, C.~S. and {Theuns}, T. and {Schaller}, M. and {Crain}, R.~A. and {McAlpine}, S.}, - Journal = {ArXiv e-prints}, - Month = jul, - Title = {{The dark nemesis of galaxy formation: why hot haloes trigger black hole growth and bring star formation to an end}}, - Year = 2016} - - -@article{Boylan-Kolchin:2006aa, - Author = {{Boylan-Kolchin}, M. and {Ma}, C.-P. and {Quataert}, E.}, - Journal = {\mnras}, - Month = jul, - Pages = {1081-1089}, - Title = {{Red mergers and the assembly of massive elliptical galaxies: the fundamental plane and its projections}}, - Volume = 369, - Year = 2006} - - -@article{Bullock:2005aa, - Author = {{Bullock}, J.~S. and {Johnston}, K.~V.}, - Journal = {\apj}, - Month = dec, - Pages = {931-949}, - Title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, - Volume = 635, - Year = 2005} - -@article{Cole:2000aa, - Author = {{Cole}, S. and {Lacey}, C.~G. and {Baugh}, C.~M. and {Frenk}, C.~S.}, - Journal = {\mnras}, - Month = nov, - Pages = {168-204}, - Title = {{Hierarchical galaxy formation}}, - Volume = 319, - Year = 2000} - -@article{Cooper:2010aa, - Author = {{Cooper}, A.~P. and {Cole}, S. and {Frenk}, C.~S. and {White}, S.~D.~M. and {Helly}, J. and {Benson}, A.~J. and {De Lucia}, G. and {Helmi}, A. and {Jenkins}, A. and {Navarro}, J.~F. and {Springel}, V. and {Wang}, J.}, - Journal = {\mnras}, - Month = aug, - Pages = {744-766}, - Title = {{Galactic stellar haloes in the CDM model}}, - Volume = 406, - Year = 2010} - -@article{Cooper:2015aa, - Author = {{Cooper}, A.~P. and {Parry}, O.~H. and {Lowing}, B. and {Cole}, S. and {Frenk}, C.}, - Journal = {\mnras}, - Month = dec, - Pages = {3185-3199}, - Title = {{Formation of in situ stellar haloes in Milky Way-mass galaxies}}, - Volume = 454, - Year = 2015} - -@article{De-Lucia:2006aa, - Author = {{De Lucia}, G. and {Springel}, V. and {White}, S.~D.~M. and {Croton}, D. and {Kauffmann}, G.}, - Journal = {\mnras}, - Month = feb, - Pages = {499-509}, - Title = {{The formation history of elliptical galaxies}}, - Volume = 366, - Year = 2006} - -@article{De-Lucia:2007aa, - Author = {{De Lucia}, G. and {Blaizot}, J.}, - Journal = {\mnras}, - Month = feb, - Pages = {2-14}, - Title = {{The hierarchical formation of the brightest cluster galaxies}}, - Volume = 375, - Year = 2007} - -@article{Furlong:2017aa, - Author = {{Furlong}, M. and {Bower}, R.~G. and {Crain}, R.~A. and {Schaye}, J. and {Theuns}, T. and {Trayford}, J.~W. and {Qu}, Y. and {Schaller}, M. and {Berthet}, M. and {Helly}, J.~C.}, - Journal = {\mnras}, - Month = feb, - Pages = {722-738}, - Title = {{Size evolution of normal and compact galaxies in the EAGLE simulation}}, - Volume = 465, - Year = 2017} - -@article{Guo:2008aa, - Author = {{Guo}, Q. and {White}, S.~D.~M.}, - Journal = {\mnras}, - Month = feb, - Pages = {2-10}, - Title = {{Galaxy growth in the concordance {$\Lambda$}CDM cosmology}}, - Volume = 384, - Year = 2008} - -@article{Iodice:2016aa, - Author = {{Iodice}, E. and {Capaccioli}, M. and {Grado}, A. and {Limatola}, L. and {Spavone}, M. and {Napolitano}, N.~R. and {Paolillo}, M. and {Peletier}, R.~F. and {Cantiello}, M. and {Lisker}, T. and {Wittmann}, C. and {Venhola}, A. and {Hilker}, M. and {D'Abrusco}, R. and {Pota}, V. and {Schipani}, P.}, - Journal = {\apj}, - Month = mar, - Pages = {42}, - Title = {{The Fornax Deep Survey with VST. I. The Extended and Diffuse Stellar Halo of NGC 1399 out to 192 kpc}}, - Volume = 820, - Year = 2016} - -@article{Kormendy:2009aa, - Author = {{Kormendy}, J. and {Fisher}, D.~B. and {Cornell}, M.~E. and {Bender}, R.}, - Journal = {\apjs}, - Month = may, - Pages = {216-309}, - Title = {{Structure and Formation of Elliptical and Spheroidal Galaxies}}, - Volume = 182, - Year = 2009} - -@article{Laporte:2013aa, - Author = {{Laporte}, C.~F.~P. and {White}, S.~D.~M. and {Naab}, T. and {Gao}, L.}, - Journal = {\mnras}, - Month = oct, - Pages = {901-909}, - Title = {{The growth in size and mass of cluster galaxies since z = 2}}, - Volume = 435, - Year = 2013} - -@article{Oser:2010aa, - Author = {{Oser}, L. and {Ostriker}, J.~P. and {Naab}, T. and {Johansson}, P.~H. and {Burkert}, A.}, - Journal = {\apj}, - Month = dec, - Pages = {2312-2323}, - Title = {{The Two Phases of Galaxy Formation}}, - Volume = 725, - Year = 2010} - -@article{Roy:2018aa, - Author = {{Roy}, N. and {Napolitano}, N.~R. and {La Barbera}, F. and {Tortora}, C. and {Getman}, F. and {Radovich}, M. and {Capaccioli}, M. and {Brescia}, M. and {Cavuoti}, S. and {Longo}, G. and {Raj}, M.~A. and {Puddu}, E. and {Covone}, G. and {Amaro}, V. and {Vellucci}, C. and {Grado}, A. and {Kuijken}, K. and {Verdoes Kleijn}, G. and {Valentijn}, E.}, - Journal = {\mnras}, - Month = oct, - Pages = {1057-1080}, - Title = {{Evolution of galaxy size-stellar mass relation from the Kilo-Degree Survey}}, - Volume = 480, - Year = 2018} - -@article{Xie:2015aa, - Author = {{Xie}, L. and {Guo}, Q. and {Cooper}, A.~P. and {Frenk}, C.~S. and {Li}, R. and {Gao}, L.}, - Journal = {\mnras}, - Month = feb, - Pages = {636-645}, - Title = {{The size evolution of elliptical galaxies}}, - Volume = 447, - Year = 2015} - -@article{Trujillo:2006aa, - Author = {{Trujillo}, I. and {F{\"o}rster Schreiber}, N.~M. and {Rudnick}, G. and {Barden}, M. and {Franx}, M. and {Rix}, H.-W. and {Caldwell}, J.~A.~R. and {McIntosh}, D.~H. and {Toft}, S. and {H{\"a}ussler}, B. and {Zirm}, A. and {van Dokkum}, P.~G. and {Labb{\'e}}, I. and {Moorwood}, A. and {R{\"o}ttgering}, H. and {van der Wel}, A. and {van der Werf}, P. and {van Starkenburg}, L.}, - Journal = {\apj}, - Month = oct, - Pages = {18-41}, - Title = {{The Size Evolution of Galaxies since z\~{}3: Combining SDSS, GEMS, and FIRES}}, - Volume = 650, - Year = 2006} diff --git a/cticomments b/cticomments deleted file mode 100755 index f4fe263..0000000 --- a/cticomments +++ /dev/null @@ -1,45 +0,0 @@ --> Luca - - Hi James, - - Very nice paper. - I only have a question: I remember there was the possibility (if not the baseline) that charge injection would happen with the shutter open, hence with stars and galaxies in the background. - This seems confirmed in your text as you mention that the sequence would last 565 s, the same of a typical VIS exposure. - - If this is the case, do you think the presence of background objects would affect the analysis? - - If instead the plan is to observe with the shutter closed, then forget my question (sorry, I didn’t follow Euclid too much in the last months). - - Kind regards, - Luca - --> Ruyman - - https://drive.google.com/file/d/1ff56U5ShOAEZ5J79TyZHI_UNoLZvF7KW/view - --> Jesper - - Thank you for an interesting and well-written paper. I don’t have any major changes, but there were a few minor things that I wanted to point out: - - Sect 2.2 and table 1: - In the middle of the paragraph you refer to table 2, but I think you mean table 1? - Table 1 has no units - is that on purpose? I assume that the tau values are in pixel shift times? (I think you refer to that in sect 5.2) - In section 2.1 you write that tau depends on the physical nature of the trap species, but I am not sure that the numbers in table 1 has any relation to the actual physical values that we find, for instance with trap pumping, but is rather a best fit representation to the broad distributions we find with the trap pumping method. - - Figs 1,2,4, etc - It is a bit odd that your figures showing CIL examples has the readout in the upper left corner, when the axis starts in the lower left corner. That means that you clock towards 0 in x, and away from 0 in y. Can you flip the y-axis? - Consider using a uniform sequential colormap (will also be uniform in greyscale - for instance 'viridis') for your plots instead of the 'jet' colormap that goes from dark to light to dark. - Sect. 3.4.2: You list a number of things that can give a non-uniform CIL structure: "Voltage spikes, loose connections and faults in the charge injection electronics". However, these things would not give the repeatable pattern that you show in Fig 4, but something completely useless. This pattern comes from very small differences in the CI pixel structure for each column, which is inevitable in the production process. This pattern is highly repeatable as this is governed by kTC noise and not shot noise, as a normal photon flatfield image would. I cannot figure out if this matches with the way you simulate the non-uniform CIL? It sounds like all CILs are random? - Figure 3: - - You have 4 panels but refer to the right and left panel in the first line of the caption. Maybe number each panel and refer to those numbers in the caption instead? - Maybe change the title of the plots to 'Parallel (or Serial) CTI model EPER and species profiles (or EPER)'. That way the title is shorter and you can make the font bigger, so it is easier to read. - - Is Table 2 meant to show the exact same values in both lines? - You never reference figure 9. I think the reference to Fig 10 in sect 6.1 2nd para should be to Fig 9. - Sect 6.2: missing reference in 2nd paragraph - Sect 7.3.1: The paper you cite here, Skottfelt et al. 2017 (Journal of Astronomical Telescopes, Instruments, and Systems, 3, 028001), doesn't actually contain any Trap Pumping data. I suggest you reference this paper instead: http://oro.open.ac.uk/52705/ - --> Henk - - See Documents/Papers diff --git a/devaucoleurs1948.247D b/devaucoleurs1948.247D deleted file mode 100755 index 6f99e3f..0000000 Binary files a/devaucoleurs1948.247D and /dev/null differ diff --git a/euclid.sty b/euclid.sty deleted file mode 100755 index 317dc1c..0000000 --- a/euclid.sty +++ /dev/null @@ -1,189 +0,0 @@ -%------------------------------------------------------------------------------ -% Style file for Euclid mission publications -% -% based in part on the Planck style file that was -% generously provided to us by C.R. Lawrence -% -% Usage: after specifying the \documentclass command in the La\TeX\ input file, -% add this command: \usepackage{euclid} -% -% Please send questions/comments to: -% Thomas Erben (terben@astro.uni-bonn.de) -%------------------------------------------------------------------------------ - -\ProvidesPackage{euclid}[2019/11/14 Version 1.0 Euclid publication package] -\NeedsTeXFormat{LaTeX2e} - -% packages that we always need/want: - -% AMS mathematical packages: -\RequirePackage{amsmath,amssymb} -% Units -\RequirePackage{siunitx} -% correct spaces after 'newcommand' definitions -\RequirePackage{xspace} - -%----------------------------------------------------------------------- -% Deinitions for the correct spelling of space missions -%----------------------------------------------------------------------- -\newcommand*{\Euclid}{\textit{Euclid}\xspace} -\newcommand*{\Planck}{\textit{Planck}\xspace} -\newcommand*{\Herschel}{\textit{Herschel}\xspace} -\newcommand*{\Fermi}{\textit{Fermi}\xspace} -\newcommand*{\Chandra}{\textit{Chandra}\xspace} -\newcommand*\XMMN{XMM-\textit{Newton}\xspace} -\newcommand*{\WMAP}{\textit{Wilkinson} Microwave Anisotropy Probe\xspace} -\newcommand*{\Spitzer}{\textit{Spitzer} Space Telescope\xspace} -\newcommand*{\HST}{\textit{Hubble} Space Telescope\xspace} - -%----------------------------------------------------------------------- -% Deinitions/shortcuts for mathematical and physical symbols/operators -% I just transfered them from Peters original Euclid.tex file -%----------------------------------------------------------------------- -\DeclareMathOperator{\logten}{log_{10}} -\newcommand*{\Ltwo}{\ensuremath{L_2}} -\newcommand*{\inv}{\ensuremath{^{-1}}} -\newcommand*{\superscr}[1]{\ensuremath{^{\rm #1}}} -\newcommand*{\expo}[1]{\ensuremath{\times 10^{#1}}} -\newcommand*{\diff}{\ensuremath{{\rm d}}} - -% The following two newcommands finally define the command 'simprop' -% for a \propto with a \sim underneath. It is from stackoverflow -% (https://tex.stackexchange.com/questions/33538/how-to-get-an-approximately-proportional-to-symbol) -% The definition makes sure that the symbol can also be used correctly in -% sub- and superscripts: -\newcommand{\simpropinn}[2]{\mathrel{\vcenter{ - \offinterlineskip\halign{\hfil$##$\cr - #1\propto\cr\noalign{\kern2pt}#1\sim\cr\noalign{\kern-2pt}}}}} -\newcommand{\simprop}{\mathpalette\simpropinn\relax} - -%----------------------------------------------------------------------- -% Definitions for mathematical expressions in parenthese/brackets .. -% of correct size -%----------------------------------------------------------------------- -% parentheses -\newcommand*{\paren}[1]{\left( #1 \right)} -% brackets -\newcommand*{\brackets}[1]{\left[ #1 \right]} -% curly braces -\newcommand*{\curly}[1]{\left\{ #1 \right\}} -% averages -\newcommand*{\ave}[1]{\left\langle #1 \right\rangle} -% absolute values -\newcommand*{\abs}[1]{\left| #1 \right|} -% within Euclid we want vectors to be printed in mathbold: -\renewcommand*\vec[1]{\ensuremath{\boldsymbol{#1}}} -\newcommand*\tens[1]{\ensuremath{\mathsf{#1}}} - -%---------------------------------------------------------------------- -% Definitions for units with siunitx -%---------------------------------------------------------------------- -% -% some more base units which are not defined within siunitx but wich -% are very common in astronomy: -\DeclareSIUnit \century{century} -\DeclareSIUnit \parsec{pc} -\DeclareSIUnit \year{yr} -\DeclareSIUnit \steradian{sr} -% -% solar-mass as unit -\DeclareSIUnit \solarmass{\text{\ensuremath{\textup{M}_{\odot}}}} -% solar-luminosity as unit -\DeclareSIUnit \solarluminosity{\text{\ensuremath{\textup{L}_{\odot}}}} -% small 'h' Hubble constant - we define it for siunitx so that it -% can be used easily 'as a unit': -\DeclareSIUnit \h{\ensuremath{\mathnormal{h}}} -\DeclareSIUnit \hubble{\h} -% Definition for h_{70} Hubble constant -\DeclareSIUnit \hseventy{\ensuremath{\mathnormal{h_{70}}}} -% shortcut for h^{-1} Mega parsec -\DeclareSIUnit \hMpc{\per\h\mega\parsec} -% shortcut for micrometer -\DeclareSIUnit \micron{\micro\meter} -% shortcut for kilometers per second -\DeclareSIUnit \kms{\kilo\meter\per\second} -% shortcut for kilometers per second per Mega Parsec -\DeclareSIUnit \kmsMpc{\kilo\meter\per\second\per\mega\parsec} - -% newcommand to typeset Ra-values in hours, minutes and seconds -% (angles in degrees, minutes and seconds can be done with the -% ang-command) -\newcommand*{\ra}[2][]{{% extra pair of braces to keep the \defintion local! - \def\SIUnitSymbolDegree{\textsuperscript{h}}% - \def\SIUnitSymbolArcminute{\textsuperscript{m}}% - \def\SIUnitSymbolArcsecond{\textsuperscript{s}}% - \ang[#1]{#2}}% -} -% Euclid convention to print angle symbol over the decimal -% point: -\sisetup{angle-symbol-over-decimal} -\sisetup{arc-separator = \,} -% Euclid convention to print errors with a +/- sign: -\sisetup{separate-uncertainty = true} -% to print ranges of numbers with a dash -\sisetup{range-phrase= ~\textendash~} - -%---------------------------------------------------------------------- -% Intuitive abbreviations for often used LaTeX-commands -%---------------------------------------------------------------------- -% -\newcommand*{\bea}{\begin{align}} -\newcommand*{\eea}{\end{align}} -\newcommand*{\be}{\begin{equation}} -\newcommand*{\ee}{\end{equation}} -\newcommand*{\bc}{\begin{center}} -\newcommand*{\ec}{\end{center}} -\newcommand*{\bfig}{\begin{figure}} -\newcommand*{\bfigs}{\begin{figure}\sidecaption} -\newcommand*{\efig}{\end{figure}} -\newcommand*{\btable}{\begin{table}} -\newcommand*{\etable}{\end{table}} -\newcommand*{\bi}{\begin{itemize}} -\newcommand*{\ei}{\end{itemize}} -\newcommand*{\ben}{\begin{enumerate}} -\newcommand*{\een}{\end{enumerate}} -\newcommand*{\bd}{\begin{description}} -\newcommand*{\ed}{\end{description}} - -%---------------------------------------------------------------------- -% Convenience abbreviations for manual unit typesetting -% These abbreviations can be used by people who do not want -% to use siunitx to typeset units -%---------------------------------------------------------------------- -% -\newcommand*{\degree}{\si{\degree}} -\newcommand*{\arcminute}{\si{\arcminute}} -\newcommand*{\arcsecond}{\si{\arcsecond}} -\newcommand*{\GHz}{\si{\giga\hertz}} -\newcommand*{\hMpc}{\si{\hMpc}} -\newcommand*{\kms}{\si{\kilo\meter\per\second}} -\newcommand*{\kmsMpc}{\si{\kmsMpc}} -\newcommand*{\mHz}{\si{\mega\hertz}} -\newcommand*{\Lsolar}{\si{\solarluminosity}} -\newcommand*{\Msolar}{\si{\solarmass}} -\newcommand*{\micron}{\si{\micro\meter}} - -% ------------------------------------------------------------ -% Macros for acknowledgement texts -% -\newcommand*{\AckInstitutions}{a number of agencies and - institutes that have supported the development of \Euclid, in - particular -the Academy of Finland, the Agenzia Spaziale Italiana, -the Belgian Science Policy, the Canadian Euclid Consortium, the Centre -National d'Etudes Spatiales, the Deutsches Zentrum f\"ur Luft- und -Raumfahrt, the Danish Space Research Institute, the Funda\c{c}\~{a}o -para a Ci\^{e}ncia e a Tecnologia, the Ministerio de Economia y -Competitividad, the National Aeronautics and Space Administration, the -Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space -Agency, the Romanian Space Agency, the State Secretariat for -Education, Research and Innovation (SERI) at the Swiss Space Office -(SSO), and the United Kingdom Space Agency. A complete and detailed - list is available on the \Euclid\ web site -(\texttt{http://www.euclid-ec.org}).\xspace} -\newcommand{\AckEC}{The Euclid Consortium acknowledges the European - Space Agency and \AckInstitutions} -\newcommand{\AckECon}{The authors acknowledge the Euclid Consortium, - the European Space Agency, and \AckInstitutions} -\newcommand{\AckECol}{The authors acknowledge the Euclid - Collaboration, the European Space Agency, and \AckInstitutions} diff --git a/index.md b/index.md index b1c8dbd..73844c8 100644 --- a/index.md +++ b/index.md @@ -3,25 +3,25 @@ The PyAuto organism's long-term knowledge: a multi-domain knowledge base of accumulated scientific and project knowledge, organised as several Karpathy-style LLM wikis over a shared canonical bibliography. Each sub-wiki uses -the schema in [`lensing_wiki/CLAUDE.md`](lensing_wiki/CLAUDE.md). +the schema in [`wiki/CLAUDE.md`](wiki/CLAUDE.md). ## Sub-wikis -- [`lensing_wiki/`](lensing_wiki/index.md) — **strong gravitational +- [`wiki/lensing/`](wiki/lensing/index.md) — **strong gravitational lensing.** The primary sub-wiki. Lens equation, mass models, source reconstruction, degeneracies, time-delay cosmography, dark-matter substructure, surveys (SLACS, BELLS, H0liCOW, TDCOSMO, Euclid Q1, HFF), software (PyAutoLens, lenstronomy). -- [`smbh_wiki/`](smbh_wiki/index.md) — **supermassive black holes.** +- [`wiki/smbh/`](wiki/smbh/index.md) — **supermassive black holes.** Binaries, recoil, scouring, mass functions, GW background (NANOGrav), seeds and growth. -- [`cti_wiki/`](cti_wiki/index.md) — **Charge Transfer Inefficiency.** +- [`wiki/cti/`](wiki/cti/index.md) — **Charge Transfer Inefficiency.** CCD trap physics, forward-model correction (`arctic`), trap pumping, Euclid VIS calibration, HST ACS, Gaia. -- [`methods_wiki/`](methods_wiki/index.md) — **statistical and +- [`wiki/methods/`](wiki/methods/index.md) — **statistical and computational methods.** Bayesian inference, samplers, deep learning, probabilistic programming, NUFFT, simulations, scientific software. -- [`galaxies_wiki/`](galaxies_wiki/index.md) — **galaxy formation and +- [`wiki/galaxies/`](wiki/galaxies/index.md) — **galaxy formation and evolution.** Massive ellipticals (MASSIVE survey), bulge/disk decomposition, IFU spectroscopy, stellar halos, COSMOS, high-redshift, halo-galaxy connection, galaxy-scale DM geometry. @@ -31,14 +31,14 @@ the schema in [`lensing_wiki/CLAUDE.md`](lensing_wiki/CLAUDE.md). - [`reading-queue.md`](reading-queue.md) — paper queue (moved from `admin_jammy/papers.md` on 2026-05-22). Section headers (Strong Lensing, SMBHs, Galaxy Formation, Dark Matter, Stats, SETI, Cancer) - match topic folders. When a queued paper is acquired as a PDF, file - it under the matching folder and stub it in the appropriate - `_wiki/sources/*.md`. + match the sub-wiki domains. When a queued paper is read, stub it in + the appropriate sub-wiki `sources/*.md` and add its canonical entry + to `bibliography/` — the PDF itself stays off-repo, never committed. ## Schema The schema is defined once in -[`lensing_wiki/CLAUDE.md`](lensing_wiki/CLAUDE.md) and inherited by +[`wiki/CLAUDE.md`](wiki/CLAUDE.md) and inherited by all sub-wikis. Each sub-wiki has its own `CLAUDE.md` that diverges only on the `## Scope` section. Per-page frontmatter, naming conventions, `[[wiki-links]]`, status flags (`stub | drafted | diff --git a/library.bib b/library.bib deleted file mode 100755 index 928583b..0000000 --- a/library.bib +++ /dev/null @@ -1,47316 +0,0 @@ -Automatically generated by Mendeley Desktop 1.19.8 -Any changes to this file will be lost if it is regenerated by Mendeley. - -BibTeX export options can be customized via Options -> BibTeX in Mendeley Desktop - -@article{Minor2025, -abstract = {Recent studies have shown that the dark substructure reported in the gravitational lens SDSS J0946+1006 has a high central density, which is in apparent tension with the flat cold dark matter ($\Lambda$CDM) paradigm. However, its detection significance has been found in D. J. Ballard et al. to be sensitive to prior assumptions about the smoothness of the source galaxy. Here we show that the detection significance of the substructure is higher than previously reported (log-Bayes factor $\Delta$ ln E ≈ 143 , equivalent to a ∼17 $\sigma$ detection) by approximating the integration of light over each pixel via ray tracing and averaging over many subpixels—a technique known as supersampling—and this result is insensitive to the assumed prior on the source galaxy smoothness. Assuming a dark matter subhalo, the combination of supersampling and modeling both sets of lensed arcs also tightens the subhalo constraints: we find the subhalo's projected mass within 1 kpc lies in the range (2.2–3.4) × 10 9 M ⊙ at 95% confidence in our highest evidence model, while the log-slope of the subhalo's projected density at 1 kpc is steeper than −1.75 at the 95% confidence level, further establishing it as an outlier compared to expectations from CDM. We also identify a systematic that has biased the slope of the primary lensing galaxy's density profile in prior studies, which we speculate might be due to the presence of dust or an imperfect foreground subtraction. Our analysis places the existence of the substructure on firmer ground, and should motivate deeper follow-up observations to better constrain its properties and clarify its apparent tension with $\Lambda$CDM.}, -author = {Minor, Quinn E.}, -doi = {10.3847/1538-4357/adb1b6}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Minor2025SuperSamplin.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -number = {1}, -pages = {2}, -publisher = {IOP Publishing}, -title = {{High Significance Detection of the Dark Substructure in Gravitational Lens SDSS J0946+1006 by Image Pixel Supersampling}}, -url = {http://dx.doi.org/10.3847/1538-4357/adb1b6}, -volume = {981}, -year = {2025} -} -@article{Nightingale2020, -author = {Nightingale, James W and Hayes, Richard G and Kelly, Ashley and Etherington, Amy and Cao, Xiaoyue and Massey, Richard J and Amvrosiadis, Aristeidis and Cole, Shaun and Li, Ran and Frenk, S and Harvey, David R and He, Qiuahn and Robertson, Andrew}, -file = {::}, -keywords = {galaxies,gravitational lensing,structure}, -number = {2018}, -pages = {1--7}, -title = {{PyAutoLens : Catchy Subtitle With a Play on Words}}, -volume = {7}, -year = {2020} -} -@article{Herbert-Fort2007, -abstract = {We measure the distribution of velocities for prograde and retrograde satellite galaxies using a combination of published data and new observations for 78 satellites of 63 extremely isolated disc galaxies (169 satellites total). We find that the velocity distribution is non-Gaussian ({\textgreater}99.9{\%} confidence), but that it can be described as the sum of two Gaussians, one of which is broad (sigma = 176 pm 15 km/s), has a mean prograde velocity of 86 pm 30 km/s, and contains {\$\sim${}}55{\%} of the satellites, while the other is slightly retrograde with a mean velocity of -21 pm 22 km/s and sigma = 74 pm 18 km/s and contains {\$\sim${}}45{\%} of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher-level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Negrello2010, -abstract = {Gravitational lensing is a powerful astrophysical and cosmological probe and is particularly valuable at submillimeter wavelengths for the study of the statistical and individual properties of dusty star-forming galaxies. However, the identification of gravitational lenses is often time-intensive, involving the sifting of large volumes of imaging or spectroscopic data to find few candidates. We used early data from the Herschel Astrophysical Terahertz Large Area Survey to demonstrate that wide-area submillimeter surveys can simply and easily detect strong gravitational lensing events, with close to 100% efficiency.}, -archivePrefix = {arXiv}, -arxivId = {1011.1255}, -author = {Negrello, Mattia and Hopwood, R. and {De Zotti}, G. and Cooray, A. and Verma, A. and Bock, J. and Frayer, D. T. and Gurwell, M. A. and Omont, A. and Neri, R. and Dannerbauer, H. and Leeuw, L. L. and Barton, E. and Cooke, J. and Kim, S. and {Da Cunha}, E. and Rodighiero, G. and Cox, P. and Bonfield, D. G. and Jarvis, M. J. and Serjeant, S. and Ivison, R. J. and Dye, S. and Aretxaga, I. and Hughes, D. H. and Ibar, E. and Bertoldi, F. and Valtchanov, I. and Eales, S. and Dunne, L. and Driver, S. P. and Auld, R. and Buttiglione, S. and Cava, A. and Grady, C. A. and Clements, D. L. and Dariush, A. and Fritz, J. and Hill, D. and Hornbeck, J. B. and Kelvin, L. and Lagache, G. and Lopez-Caniego, M. and Gonzalez-Nuevo, J. and Maddox, S. and Pascale, E. and Pohlen, M. and Rigby, E. E. and Robotham, A. and Simpson, C. and Smith, D. J.B. and Temi, P. and Thompson, M. A. and Woodgate, B. E. and York, D. G. and Aguirre, J. E. and Beelen, A. and Blain, A. and Baker, A. J. and Birkinshaw, M. and Blundell, R. and Bradford, C. M. and Burgarella, D. and Danese, L. and Dunlop, J. S. and Fleuren, S. and Glenn, J. and Harris, A. I. and Kamenetzky, J. and Lupu, R. E. and Maddalena, R. J. and Madore, B. F. and Maloney, P. R. and Matsuhara, H. and Michaowski, M. J. and Murphy, E. J. and Naylor, B. J. and Nguyen, H. and Popescu, C. and Rawlings, S. and Rigopoulou, D. and Scott, D. and Scott, K. S. and Seibert, M. and Smail, I. and Tuffs, R. J. and Vieira, J. D. and {Van Der Werf}, P. P. and Zmuidzinas, J.}, -doi = {10.1126/science.1193420}, -eprint = {1011.1255}, -isbn = {1095-9203 (Electronic)\n0036-8075 (Linking)}, -issn = {10959203}, -journal = {Science}, -keywords = {CosmicDawn}, -number = {6005}, -pages = {800--804}, -pmid = {21051633}, -title = {{The detection of a population of submillimeter-bright, strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1011.1255}, -volume = {330}, -year = {2010} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless} $\sigma$∗ {\textless} 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Mendez-Abreu2010a, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A < 0.9). This fraction is 33%, 55%, and 43% if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C < (A + B)/2). Only 18% of the observed bulges have a probability >50% and none has a probability >90% of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n > 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T > 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n > 2 and B/T > 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n > 2 and with B/T > 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n > 2 and B/T > 0.3. {\textcopyright} 2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J. and Simonneau, E. and Aguerri, J. A.L. and Corsini, E. M.}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/M{\'{e}}ndez-Abreu et al. - 2010 - Structural properties of disk galaxies II. Intrinsic shape of bulges(3).pdf:pdf}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {galaxies: bulges,galaxies: elliptical and lenticular, cD,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Hilz2013, -abstract = {There is observational evidence for inside-out growth of giant elliptical galaxies since z≳ 2-3, which is - in contrast to disc galaxies - not driven by in situ star formation. Many of the $\sim$1011M⊙ systems at high redshift have small sizes $\sim$1 kpc and surface brightness profiles with low-{\'{S}}ersic indices n. The most likely descendants at z = 0 have, on average, grown by a factor of 2 in mass and a factor of 4 in size, indicating r$\alpha$ M$\alpha$ with $\alpha$ ≳2. They also have surface brightness profiles with n ≳ 5. This evolution can be qualitatively explained on the basis of two assumptions: compact ellipticals predominantly grow by collisionless minor (mass-ratio 1:10) or intermediate (mass-ratio 1:5) 'dry' mergers, and they are embedded in massive dark matter haloes which support the stripping of merging satellite stars at large radii. We draw these conclusions from idealized collisionless mergers spheroidal galaxies - with and without dark matter - with mass ratios of 1:1, 1:5 and 1:10. The sizes evolve as r$\alpha$ M$\alpha$ with$\alpha$ <2 for mass-ratios of 1:1 (and 1:5 without dark matter haloes) and, while doubling the stellar mass, the {\'{S}}ersic index increases from n $\sim$ 4 to n $\sim$ 5. For minor mergers of galaxies embedded in dark matter haloes, the sizes grow significantly faster and the profile shapes change more rapidly. Surprisingly, already mergers with moderate mass-ratios of 1:5, well motivated by recent cosmological simulations, give $\alpha$ $\sim$ 2.3 and after only two merger generations ($\sim$40 per cent added stellar mass) the {\'{S}}ersic index has increased to n > 8 (n $\sim$ 5.5 without dark matter), reaching a final value of n = 9.5 after doubling the stellar mass. This is accompanied by a significant increase of the dark matter fraction (from $\sim$40 to ≳70 per cent) within the stellar half-mass radius, driven by the strong size increase probing larger, dark matter-dominated regions. For equal-mass mergers the effect is much weaker. We conclude that only a few intermediate mass-ratio mergers ($\sim$3-5 with initial mass-ratios of 1:5) of galaxies embedded in massive dark matter haloes can result in the observed concurrent inside-out growth and the rapid evolution in profile shapes. This process might explain the existence of present-day giant ellipticals with sizes, r > 4 kpc, high {\'{S}}ersic indices, n > 5, and a significant amount of dark matter within the half-light radius. Apart from negative stellar metallicity gradients such a 'minor' merger scenario also predicts significantly lower dark matter fractions for z $\sim$ 2 compact quiescent galaxies and their rare present-day analogues. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1206.5004}, -author = {Hilz, Michael and Naab, Thorsten and Ostriker, J. P.}, -doi = {10.1093/mnras/sts501}, -eprint = {1206.5004}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cd-Galaxies,Galaxies,ellipticals and lenticular,evolution-Galaxies,fundamental parameters-Galaxies,haloes-galaxies,photometry-Galaxies,structure}, -month = {mar}, -number = {4}, -pages = {2924--2933}, -title = {{How do minor mergers promote inside-out growth of ellipticals, transforming the size, density profile and dark matter fraction?}}, -volume = {429}, -year = {2013} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Lauer2005, -abstract = {We present observations of 77 early-type galaxies imaged with the PC1 CCD of the Hubble Space Telescope (HST) WFPC2. "Nuker-law" parametric fits to the surface brightness profiles are used to classify the central structure into "core" or "power-law" forms. Core galaxies are typically rounder than power-law galaxies. Nearly all power-law galaxies with central ellipticities $\epsilon$ ≥ 0.3 have stellar disks, implying that disks are present in power-law galaxies with $\epsilon$ < 0.3 but are not visible because of unfavorable geometry. A few low-luminosity flattened core galaxies also have disks; these may be transition forms from power-law galaxies to more luminous core galaxies, which lack disks. Several core galaxies have strong isophote twists interior to their break radii, although power-law galaxies have interior twists of similar physical significance when the photometric perturbations implied by the twists are evaluated. Central color gradients are typically consistent with the envelope gradients; core galaxies have somewhat weaker color gradients than power-law galaxies. Nuclei are found in 29% of the core galaxies and 60% of the power-law galaxies. Nuclei are typically bluer than the surrounding galaxy. While some nuclei are associated with active galactic nuclei (AGNs), just as many are not; conversely, not all galaxies known to have a low-level AGN exhibit detectable nuclei in the broadband filters. NGC 4073 and 4382 are found to have central minima in their intrinsic starlight distributions; NGC 4382 resembles the double nucleus of M31. In general, the peak brightness location is coincident with the photocenter of the core to a typical physical scale of < 1 pc. Five galaxies, however, have centers significantly displaced from their surrounding cores; these may be unresolved asymmetric double nuclei. Finally, as noted by previous authors, central dust is visible in about half of the galaxies. The presence and strength of dust correlates with nuclear emission; thus, dust may outline gas that is falling into the central black hole. The prevalence of dust and its morphology suggest that dust clouds form, settle to the center, and disappear repeatedly on ∼ 10 8 yr timescales. We discuss the hypothesis that cores are created by the decay of a massive black hole binary formed in a merger. Apart from their brightness profiles, there are no strong differences between core galaxies and power-law galaxies that demand this scenario; however, the rounder shapes of core, their lack of disks, and their reduced color gradients may be consistent with it. {\textcopyright} 2005. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0412040}, -author = {Lauer, Tod R. and Faber, S. M. and Gebhardt, Karl and Richstone, Douglas and Tremaine, Scott and Ajhar, Edward A. and Aller, M. C. and Bender, Ralf and Dressler, Alan and Filippenko, Alexei V. and Green, Richard and Grillmair, Carl J. and Ho, Luis C. and Kormendy, John and Magorrian, John and Pinkney, Jason and Siopis, Christos}, -doi = {10.1086/429565}, -eprint = {0412040}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lauer et al. - 2005 - The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry.pdf:pdf}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2138--2185}, -primaryClass = {arXiv:astro-ph}, -title = {{ The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry }}, -url = {http://stacks.iop.org/1538-3881/129/i=5/a=2138}, -volume = {129}, -year = {2005} -} -@article{Bortolussi2018, -abstract = {We consider probabilistic model checking for continuous-time Markov chains (CTMCs) induced from Stochastic Reaction Networks (SRNs) against a fragment of Continuous Stochastic Logic (CSL) extended with reward operators. Classical numerical algorithms for CSL model checking based on uniformisation are limited to finite CTMCs|e approximation of the CTMC in terms of a Gaussian process based on the Central Limit Approximation (CLA), also known as the Linear Noise Approximation (LNA), whose solution requires solving a number of differential equations that is quadratic in the number of species and independent of the population size. We then develop efficient and scalable approximate model checking algorithms on the resulting Gaussian process, where we restrict the target regions for probabilistic reachability to convex polytopes. This allows us to derive an abstraction in terms of a time-inhomogeneous discrete-time Markov chain (DTMC), whose dimension is independent of the number of species, on which model checking is performed. Using results from probability theory, we prove the convergence in distribution of our algorithms to the corresponding measures on the original CTMC. We implement the techniques and, on a set of examples, demonstrate that they allow us to overcome the state space explosion problem, while still correctly characterizing the stochastic behaviour of the system. Our methods can be used for formal analysis of a wide range of distributed stochastic systems, including biochemical systems, sensor networks and population protocols.}, -archivePrefix = {arXiv}, -arxivId = {1804.08744}, -author = {Bortolussi, Luca and Cardelli, Luca and Kwiatkowska, Marta and Laurenti, Luca}, -eprint = {1804.08744}, -month = {apr}, -title = {{Central Limit Model Checking}}, -url = {http://arxiv.org/abs/1804.08744}, -year = {2018} -} -@article{Report2011, -abstract = {Modelling students' behaviour in relation to tuition fees is a complex task since students' 'talent' is not common knowledge. Students observe a private noisy signal of their abilities, while university receives noisy information based on the quantitative and qualitative data provided by university applicants. In this article, we add the heterogeneity of the population to this model: we assume that this heterogeneity means that the perception of skills among a part of the population is biased and underestimates the capabilities of its members to succeed in the higher education system. Our conclusions differ from those derived in the literature and show in particular that the optimal tuition fees for a given number of students are lower than those obtained for a homogeneous population. {\textcopyright}2013 Copyright Taylor and Francis Group, LLC.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Alexander2019a, -abstract = {Strong gravitational lensing is a promising probe of the substructure of dark matter halos. Deep learning methods have the potential to accurately identify images containing substructure, and differentiate WIMP dark matter from other well motivated models, including vortex substructure of dark matter condensates and superfluids. This is crucial in future efforts to identify the true nature of dark matter. We implement, for the first time, a classification approach to identifying dark matter substructure based on simulated strong lensing images with different substructure. Utilizing convolutional neural networks trained on sets of simulated images, we demonstrate the feasibility of deep neural networks to reliably distinguish among different types of dark matter substructure. With thousands of strong lensing images anticipated with the coming launch of LSST, we expect that supervised and unsupervised deep learning models will play a crucial role in determining the nature of dark matter.}, -archivePrefix = {arXiv}, -arxivId = {1909.07346}, -author = {Alexander, Stephon and Gleyzer, Sergei and McDonough, Evan and Toomey, Michael W and Usai, Emanuele}, -doi = {10.3847/1538-4357/ab7925}, -eprint = {1909.07346}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {15}, -title = {{Deep Learning the Morphology of Dark Matter Substructure}}, -url = {http://arxiv.org/abs/1909.07346}, -volume = {893}, -year = {2020} -} -@article{Cyr-Racine2019, -abstract = {Gravitational lensing has emerged as a powerful probe of the matter distribution on subgalactic scales, which itself may contain important clues about the fundamental origins and properties of dark matter. Broadly speaking, two different approaches have been taken in the literature to map the small-scale structure of the Universe using strong lensing, with one focused on measuring the position and mass of a small number of discrete massive subhalos appearing close in projection to lensed images, and the other focused on detecting the collective effect of all the small-scale structure between the lensed source and the observer. In this paper, we follow the latter approach and perform a detailed study of the sensitivity of galaxy-scale gravitational lenses to the ensemble properties of small-scale structure. As in some previous studies, we adopt the language of the substructure power spectrum to characterize the statistical properties of the small-scale density field. We present a comprehensive theory that treats lenses with extended sources as well as those with time-dependent compact sources (such as quasars) in a unified framework for the first time. Our approach uses mode functions to provide both computational advantages and insights about couplings between the lens and source. The goal of this paper is to develop the theory and gain the intuition necessary to understand how the sensitivity to the substructure power spectrum depends on the source and lens properties, with the eventual aim of identifying the most promising targets for such studies.}, -archivePrefix = {arXiv}, -arxivId = {1806.07897}, -author = {Cyr-Racine, Francis-Yan and Keeton, Charles R and Moustakas, Leonidas A}, -doi = {10.1103/physrevd.100.023013}, -eprint = {1806.07897}, -issn = {2470-0010}, -journal = {Physical Review D}, -number = {2}, -pages = {1--30}, -title = {{Beyond subhalos: Probing the collective effect of the Universe's small-scale structure with gravitational lensing}}, -volume = {100}, -year = {2019} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{McLure2004, -abstract = {Virial black hole mass estimates are presented for 12698 quasars in the redshift interval 0.1 ≤ z ≤ 2.1, based on modelling of spectra from the Sloan Digital Sky Survey (SDSS) first data release. The black hole masses of the SDSS quasars are found to lie between ≃10 7 M⊙ and an upper limit of ≃3 × 10 9 M⊙, entirely consistent with the largest black hole masses found to date in the local Universe. The estimated Eddington ratios of the broad-line quasars (full width at half-maximum ≥ 2000 km s -1) show a clear upper boundary at L bol/L Edd≃1, suggesting that the Eddington luminosity is still a relevant physical limit to the accretion rate of luminous broad-line quasars at z ≤ 2. By combining the black hole mass distribution of the SDSS quasars with the two degree field (2dF) quasar luminosity function, the number density of active black holes at z ≃2 is estimated as a function of mass. In addition, we independently estimate the local black hole mass function for early-type galaxies using the M bh-$\sigma$ and M bhL bulge correlations. Based on the SDSS velocity dispersion function and the Two Micron All Sky Survey (2MASS) K-band luminosity function, both estimates are found to be consistent at the high-mass end (M bh ≥ 10 8 M⊙). By comparing the estimated number density of active black holes at z ≃2 with the local mass density of dormant black holes, we set lower limits on the quasar lifetimes and find that the majority of black holes with mass ≥ 10 8.5 M⊙ are in place by ≃2.}, -author = {McLure, Ross J. and Dunlop, James S.}, -doi = {10.1111/j.1365-2966.2004.08034.x}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Mcclure2014QuasarBHMasses.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Black hole physics,Galaxies: active,Galaxies: nuclei,Quasars: general}, -number = {4}, -pages = {1390--1404}, -title = {{The cosmological evolution of quasar black hole masses}}, -volume = {352}, -year = {2004} -} -@article{James2018, -abstract = {We present the first spatially-resolved rest-frame UV study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z=2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each {\$\sim${}}4-8 kpc{\^{}}2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with CIII] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. The mapped CIII] emission shows distinct kinematical structure, with velocity offsets of {\$\sim${}}+/-50 km/s between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionisation parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing between -200{\textless}v(km/s){\textless}-50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star-formation rates remain relatively constant ({\$\sim${}}8-16 M{\_}sol/yr), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced. We measure electron densities with a range of log(Ne)=3.92-4.36 cm{\^{}}-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially-resolved rest-frame UV studies expected with future observatories, such as JWST.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L and Auger, Matt and Pettini, Max and Stark, Daniel P and Belokurov, V and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Rhodes2004, -abstract = {A wide-field space-based imaging telescope is necessary to fully exploit the technique of observing dark matter via weak gravitational lensing. This first paper in a three part series outlines the survey strategies and relevant instrumental parameters for such a mission. As a concrete example of hardware design, we consider the proposed Supernova/Acceleration Probe (SNAP). Using SNAP engineering models, we quantify the major contributions to this telescope's point spread function (PSF). These PSF contributions are relevant to any similar wide-field space telescope. We further show that the PSF of SNAP or a similar telescope will be smaller than current ground-based PSFs, and more isotropic and stable over time than the PSF of the Hubble Space Telescope. We outline survey strategies for two different regimes--a "wide" 300 square degree survey and a "deep" 15 square degree survey that will accomplish various weak lensing goals including statistical studies and dark matter mapping. {\textcopyright} 2003 Elsevier B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0304417}, -author = {Rhodes, Jason and Refregier, Alexandre and Massey, Richard and Albert, Justin and Bacon, David and Bernstein, Gary and Ellis, Richard and Jain, Bhuvnesh and Kim, Alex and Lampton, Mike and McKay, Tim and Akerlof, C. and Aldering, G. and Amanullah, R. and Astier, P. and Baltay, C. and Barrelet, E. and Bebek, C. and Bergstr{\"{o}}m, L. and Bercovitz, J. and Bester, M. and Bigelow, B. and Bohlin, R. and Bonissent, A. and Bower, C. and Brown, M. and Campbell, M. and Carithers, W. and Commins, E. and Day, C. and Deustua, S. and DiGennaro, R. and Ealet, A. and Emmet, W. and Eriksson, M. and Fouchez, D. and Fruchter, A. and Genat, J. F. and Gerdes, D. and Gladney, L. and Goldhaber, G. and Goobar, A. and Groom, D. and Harris, S. and Harvey, P. and Heetderks, H. and Holland, S. and Huterer, D. and Johnston, W. and Karcher, A. and Kolbe, W. and Krieger, B. and Kushner, G. and Kuznetsova, N. and Lafever, R. and Lamoureux, J. and Levi, M. and Linder, E. and Loken, S. and Lorenzon, W. and Malina, R. and Mazure, A. and McKee, S. and Miquel, R. and Morgan, N. and M{\"{o}}rtsell, E. and Mostek, N. and Mufson, S. and Musser, J. and Nugent, P. and Oluseyi, H. and Pain, R. and Palaio, N. and Pankow, D. and Perlmutter, S. and Pratt, R. and Prieto, E. and Rabinowitz, D. and Robinson, K. and Roe, N. and Rusin, D. and Schubnell, M. and Sholl, M. and Smadja, G. and Smith, R. and Smoot, G. and Snyder, J. and Spadafora, A. and Szymkowiak, A. and Tarl{\'{e}}, G. and Taylor, K. and Tilquin, A. and Tomasch, A. and von der Lippe, H. and Vincent, D. and Walder, J. P. and Wang, G.}, -doi = {10.1016/j.astropartphys.2003.10.002}, -eprint = {0304417}, -issn = {09276505}, -journal = {Astroparticle Physics}, -keywords = {Dark energy,Dark matter,Instrumentation}, -month = {jan}, -number = {4}, -pages = {377--389}, -primaryClass = {astro-ph}, -title = {{Weak lensing from space I: Instrumentation and survey strategy}}, -volume = {20}, -year = {2004} -} -@article{Xie2014, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stu2487}, -volume = {447}, -year = {2015} -} -@article{Pontzen2015a, -abstract = {Galaxies and the dark matter halos that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealised calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter core-creation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are "maximally stable", i.e. that do not evolve at first order when external potentials (which arise from baryons, large scale tidal fields or infalling substructure) are applied. We show that a spherically-symmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for near-isotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealised spherically-symmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter halos (formed in collisionless cosmological simulations) nearly attain our maximally-stable limit, but their evolution freezes out before reaching it.}, -archivePrefix = {arXiv}, -arxivId = {1502.07356}, -author = {Pontzen, Andrew and Read, Justin I and Teyssier, Romain and Governato, Fabio and Gualandris, Alessia and Roth, Nina and Devriendt, Julien}, -doi = {10.1093/mnras/stv1032}, -eprint = {1502.07356}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {1366--1379}, -title = {{Milking the spherical cow - on aspherical dynamics in spherical coordinates}}, -volume = {451}, -year = {2015} -} -@article{Shen2013, -abstract = {I review the current status of quasar black hole (BH) mass estimations. Spectroscopic methods have been developed to estimate BH mass in broad line quasars to an accuracy of $\sim$ 0:5 dex. Despite their popularity, significant issues and confusion remain regarding these mass estimators. I provide an in-depth discussion on the merits and caveats of the single-epoch (SE) virial BH mass estimators, and a detailed derivation of the statistical biases of these SE mass estimates resulting from their errors. I show that error-induced sample biases on the order of a factor of several are likely present in the SE mass estimates for flux-limited, statistical quasar samples, and the distribution of SE masses in finite luminosity bins can be narrower than the nominal uncertainty of these mass estimates. I then discuss the latest applications of SE virial masses in quasar studies, including the early growth of supermassive black holes, quasar demography in the mass-luminosity plane, and the evolution of the BH-host scaling relations, with specific emphases on selection effects and sample biases in the SE masses. I conclude that there is a pressing need to understand and deal with the errors in these BH mass estimates, and to improve these BH weighing methods with substantially more and better reverberation mapping data.}, -archivePrefix = {arXiv}, -arxivId = {1302.2643}, -author = {Shen, Yue}, -eprint = {1302.2643}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Shen2013MassofQuasars.pdf:pdf}, -issn = {03049523}, -journal = {Bulletin of the Astronomical Society of India}, -keywords = {Black hole physics,Galaxies: Active,Quasars: General,Surveys}, -number = {1}, -pages = {61--115}, -title = {{The mass of quasars}}, -volume = {41}, -year = {2013} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}}, host galaxy Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {00160032}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -pages = {1--7}, -title = {{Spatially Resolved Patchy Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} Emission Within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8}}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -year = {2017} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. with the particletagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of $\sim$1900 massive dark matter haloes (1012-1014M⊙) from the Millennium II $\lambda$ cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of MilkyWay-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a S{\`{e}}rsic profile, the radial scale and amplitude of which vary systematically with halo mass (M200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M* and M200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z ≈ 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P. and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S. and White, Simon D.M.}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cooper et al. - 2013 - Galactic accretion and the outer structure of galaxies in the CDM model(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Greco2017, -abstract = {We present a catalog of extended low-surface-brightness galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first {\$}{\{}\backslashsim{\}}{\$}200 deg{\$}{\^{}}2{\$} of the survey, we have uncovered 781 LSBGs, spanning red ({\$}g-i\backslashgeq0.64{\$}) and blue ({\$}g-i{\textless}0.64{\$}) colors and a wide range of morphologies. Since we focus on extended galaxies ({\$}r{\_}\backslashmathrm{\{}eff{\}}=2.5{\$}-{\$}14{\^{}}{\{}\backslashprime\backslashprime{\}}{\$}), our sample is likely dominated by low-redshift objects. We define LSBGs to have mean surface brightnesses {\$}\backslashbar{\{}\backslashmu{\}}{\_}\backslashmathrm{\{}eff{\}}(g){\textgreater}24.3{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, which allows nucleated galaxies into our sample. As a result, the central surface brightness distribution spans a wide range of {\$}\backslashmu{\_}0(g)=18{\$}-{\$}27.4{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, with 50{\%} and 95{\%} of galaxies fainter than 24.3 and 22 mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, respectively. Furthermore, the surface brightness distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well-characterized by single-component S$\backslash$'{\{}e{\}}rsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We crossmatch our sample with existing optical, HI, and ultraviolet catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, ranging from dwarf spheroidals and ultra-diffuse galaxies in nearby groups to gas-rich irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the LSBG population.}, -archivePrefix = {arXiv}, -arxivId = {1709.04474}, -author = {Greco, Johnny P and Greene, Jenny E and Strauss, Michael A and Macarthur, Lauren A and Flowers, Xzavier and Goulding, Andy D and Huang, Song and Kim, Ji Hoon and Komiyama, Yutaka and Leauthaud, Alexie and Leisman, Lukas and Lupton, Robert H and Sif{\'{o}}n, Crist{\'{o}}bal and Wang, Shiang-Yu}, -doi = {10.3847/1538-4357/aab842}, -eprint = {1709.04474}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {dwarf,galaxies,general,keywords}, -number = {2}, -pages = {104}, -title = {{Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey}}, -url = {http://arxiv.org/abs/1709.04474%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aab842}, -volume = {857}, -year = {2018} -} -@article{Greene2017, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and S{\'{e}}rsic index distributions obtained from two-dimensional structural fits to 40, 000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of S{\'{e}}rsic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. {\textcopyright}2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Christensen2014, -abstract = {We present a detailed comparison between the photometric properties of the bulges of two simulated galaxies and those of a uniform sample of observed galaxies. This analysis shows that the simulated galaxies have bulges with realistic surface brightnesses for their sizes and magnitude. These two field disc galaxies have rotational velocities ̃100 km s-1 and were integrated to a redshift of zero in a fully cosmological $\delta$ cold dark matter context as part of high-resolution smoothed particle hydrodynamic simulations. We performed bulge- disc decompositions of the galaxies using artificial observations, in order to conduct a fair comparison to observations. We also dynamically decomposed the galaxies and compared the star formation histories of the bulges to those of the entire galaxies. These star formation histories showed that the bulges were primarily formed before z = 1 and during periods of rapid star formation. Both galaxies have large amounts of early star formation, which is likely related to the relatively high bulge-to-disc ratios also measured for them. Unlike almost all previous cosmological simulations, the realistically concentrated bulges of these galaxies do not lead to unphysically high rotational velocities, causing them to naturally lie along the observed Tully-Fisher relation. {\textcopyright}2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1402.2702}, -author = {Christensen, C R and Brooks, A M and Fisher, D B and Governato, F and McCleary, J and Quinn, T R and Shen, S and Wadsley, J}, -doi = {10.1093/mnrasl/slu020}, -eprint = {1402.2702}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Bulges,Formation,Galaxies,Methods,Numerical,Spiral,Structure}, -number = {1}, -pages = {1--6}, -title = {{Simulating disc galaxy bulges that are consistent with observed scaling relations}}, -volume = {440}, -year = {2014} -} -@article{Mandelbaum2017, -abstract = {Weak gravitational lensing, the deflection of light by mass, is one of the best tools to constrain the growth of cosmic structure with time and reveal the nature of dark energy. I discuss the sources of systematic uncertainty in weak lensing measurements and their theoretical interpretation, including our current understanding and other options for future improvement. These include long-standing concerns such as the estimation of coherent shears from galaxy images or redshift distributions of galaxies selected on the basis of photometric redshifts, along with systematic uncertainties that have received less attention to date because they are subdominant contributors to the error budget in current surveys. I also discuss methods for automated systematics detection using survey data of the 2020s. The goal of this review is to describe the current state of the field and what must be done so that if weak lensing measurements lead toward surprising conclusions about key questions such as the nature of dark energy, those conclusions will be credible.}, -archivePrefix = {arXiv}, -arxivId = {1710.03235}, -author = {Mandelbaum, Rachel}, -doi = {10.1146/annurev-astro-081817-051928}, -eprint = {1710.03235}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {cosmological parameters,cosmology: observations,gravitational lensing,methods: data analysis,methods: statistical,techniques: image processing}, -number = {1}, -pages = {393--433}, -title = {{Weak Lensing for Precision Cosmology}}, -url = {http://arxiv.org/abs/1710.03235%7B%5C%25%7D0Ahttp://dx.doi.org/10.1146/annurev-astro-081817-051928}, -volume = {56}, -year = {2018} -} -@article{Rudnick2006, -author = {{Trujillo}, I. and {F{\"o}rster Schreiber}, N.$\sim$M. and {Rudnick}, G. and {Barden}, M. and {Franx}, M. and {Rix}, H.-W. and {Caldwell}, J.$\sim$A.$\sim$R. and {McIntosh}, D.$\sim$H. and {Toft}, S. and {H{\"a}ussler}, B. and {Zirm}, A. and {van Dokkum}, P.$\sim$G. and {Labb{\'e}}, L.}, -file = {{:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Trujillo}, I. and {F{o}rster Schreiber}, N.$\sim$M. and {Rudnick}, G. and {Barden}, M. and {Franx}, M. and {Rix}, H.-W. and {Caldwell}, J.$\sim$A..pdf:pdf}, -title = {{}}, -year = {2006} -} -@article{Newman2012a, -abstract = {The presence of extremely compact galaxies at z ∼ 2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 galaxies selected with 0.4 < z < 2.5 and stellar masses M* > 1010.7 M {\textperiodcentered} in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and the mean size of these systems at fixed stellar mass grows by a factor of 3.5 0.3 over this redshift interval. The data are sufficiently deep to identify companions to these hosts whose stellar masses are ten times smaller. By searching for these around 404 quiescent hosts within a physical annulus 10 h -1 kpc < R < 30 h -1 kpc, we estimate the minor merger rate over 0.4 < z < 2. We find that 13%-18% of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6% ± 2% per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers may explain most of the size evolution observed at z ≲ 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes. {\textcopyright} 2012 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1110.1637}, -author = {Newman, Andrew B. and Ellis, Richard S. and Bundy, Kevin and Treu, Tommaso}, -doi = {10.1088/0004-637X/746/2/162}, -eprint = {1110.1637}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Newman et al. - 2012 - Can minor merging account for the size growth of quiescent galaxies New results from the CANDELS survey.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: structure}, -number = {2}, -title = {{Can minor merging account for the size growth of quiescent galaxies? New results from the CANDELS survey}}, -volume = {746}, -year = {2012} -} -@article{Belfiore2017, -abstract = {We study radial profiles in Ha equivalent width and specific star formation rate (sSFR) derived from spatially resolved SDSS-IV MaNGA spectroscopy to gain insight on the physical mechanisms that suppress star formation and determine a galaxy's location in the SFR-M* diagram. Even within the star-forming 'main sequence', the measured sSFR decreases with stellar mass, in both an integrated and spatially resolved sense. Flat sSFR radial profiles are observed for log(M*/M⊙) {\textless} 10.5, while star-forming galaxies of higher mass show a significant decrease in sSFR in the central regions, a likely consequence of both larger bulges and an inside-out growth history. Our primary focus is the green valley, constituted by galaxies lying below the star formation main sequence, but not fully passive. In the green valley we find sSFR profiles that are suppressed with respect to star-forming galaxies of the same mass at all galactocentric distances out to 2 effective radii. The responsible quenching mechanism therefore appears to affect the entire galaxy, not simply an expanding central region. The majority of green valley galaxies of log(M*/M⊙) {\textgreater} 10.0 are classified spectroscopically as central low-ionization emission-line regions (cLIERs). Despite displaying a higher central stellar mass concentration, the sSFR suppression observed in cLIER galaxies is not simply due to the larger mass of the bulge. Drawing a comparison sample of star-forming galaxies with the sameM* and $\Sigma$1 kpc (the mass surface density within 1 kpc), we show that a high $\Sigma$1 kpc is not a sufficient condition for determining central quiescence.}, -archivePrefix = {arXiv}, -arxivId = {1710.05034}, -author = {Belfiore, Francesco and Maiolino, Roberto and Bundy, Kevin and Masters, Karen and Bershady, Matthew and Oyarz{\'{u}}n, Grecco A and Lin, Lihwai and Cano-Diaz, Mariana and Wake, David and Spindler, Ashley and Thomas, Daniel and Brownstein, Joel R and Drory, Niv and Yan, Renbin}, -doi = {10.1093/mnras/sty768}, -eprint = {1710.05034}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Evolution,Galaxies: Fundamental parameters,Galaxies: ISM}, -number = {3}, -pages = {3014--3029}, -title = {{SDSS IV MaNGA - sSFR profiles and the slow quenching of discs in green valley galaxies}}, -url = {http://arxiv.org/abs/1710.05034}, -volume = {477}, -year = {2018} -} -@article{2001ey, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Galan2021, -abstract = {Strong gravitational lensing provides a wealth of astrophysical information on the baryonic and dark matter content of galaxies. It also serves as a valuable cosmological probe by allowing us to measure the Hubble constant independently of other methods. These applications all require the difficult task of inverting the lens equation and simultaneously reconstructing the mass profile of the lens along with the original light profile of the unlensed source. As there is no reason for either the lens or the source to be simple, we need methods that both invert the lens equation with a large number of degrees of freedom and also enforce a well-controlled regularisation that avoids the appearance of spurious structures. This can be beautifully accomplished by representing signals in wavelet space. Building on the Sparse Lens Inversion Technique (SLIT), we present an improved sparsity-based method that describes lensed sources using wavelets and optimises over the parameters given an analytical lens mass profile. We applied our technique on simulated HST and E-ELT data, as well as on real HST images of lenses from the Sloan Lens ACS sample, assuming a lens model. We show that wavelets allowed us to reconstruct lensed sources containing detailed substructures when using both present-day data and very high-resolution images expected from future thirty-metre-class telescopes. In the latter case, wavelets moreover provide a much more tractable solution in terms of quality and computation time compared to using a source model that combines smooth analytical profiles and shapelets. Requiring very little human interaction, our flexible pixel-based technique fits into the ongoing effort to devise automated modelling schemes. It can be incorporated in the standard workflow of sampling analytical lens model parameters while modelling the source on a pixelated grid. The method, which we call SLITRONOMY, is freely available as a new plug-in to the modelling software LENSTRONOMY.}, -archivePrefix = {arXiv}, -arxivId = {2012.02802}, -author = {Galan, A. and Peel, A. and Joseph, R. and Courbin, F. and Starck, J. L.}, -doi = {10.1051/0004-6361/202039363}, -eprint = {2012.02802}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Galan2021SLIT.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Galaxies: high-redshift,Galaxies: structure,Gravitation,Gravitational lensing: strong,Methods: data analysis,Techniques: image processing}, -number = {A176}, -pages = {21}, -title = {{SLIT RONOMY: Towards a fully wavelet-based strong lensing inversion technique}}, -volume = {647}, -year = {2021} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ($z = 1.489$), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5$+$2223 ($z = 0.542$), published by Grillo et al. (2016), and explore different $\Lambda$CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of $H_{0}$ and $\Omega_{\rm m}$ with relative (1$\sigma$) statistical errors of, respectively, 6% (7%) and 31% (26%) in flat (general) cosmological models, assuming a conservative 3% uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of $H_{0}$, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C. and Rosati, P. and Suyu, S. H. and Balestra, I. and Caminha, G. B. and Halkola, A. and Kelly, P. L. and Lombardi, M. and Mercurio, A. and Rodney, S. A. and Treu, T.}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Grillo et al. - 2018 - Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -number = {2}, -pages = {94}, -title = {{Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”}}, -url = {http://arxiv.org/abs/1802.01584}, -volume = {860}, -year = {2018} -} -@article{Blain2002, -abstract = {A cosmologically significant population of very luminous high-redshift galaxies has recently been discovered at submillimeter (submm) wavelengths. Advances in submm detector technologies have opened this new window on the distant Universe. Here we discuss the properties of the high-redshift submm galaxies, their significance for our understanding of the process of galaxy formation, and the selection effects that apply to deep submm surveys. The submm galaxies generate a significant fraction of the energy output of all the galaxies in the early Universe. We emphasize the importance of studying a complete sample of submm galaxies, and stress that because they are typically very faint in other wavebands, these follow-up observations are very challenging. Finally, we discuss the surveys that will be made using the next generation of submm-wave instruments under development. {\textcopyright} 2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202228}, -author = {Blain, Andrew W. and Smail, Ian and Ivison, R. J. and Kneib, J. P. and Frayer, David T.}, -doi = {10.1016/S0370-1573(02)00134-5}, -eprint = {0202228}, -file = {:C\:/Users/Jammy/Documents/Papers/High_Redshift_galaxies/Blain2000SubMMSummary.pdf:pdf}, -isbn = {03701573}, -issn = {03701573}, -journal = {Physics Report}, -keywords = {Dust extinction,Galaxy evolution,Galaxy formation,Gravitational lensing,Observational cosmology,Radio continuum}, -number = {2}, -pages = {111--176}, -primaryClass = {astro-ph}, -title = {{Submillimeter galaxies}}, -volume = {369}, -year = {2002} -} -@article{Yang2019a, -abstract = {We use the Illustris simulation to study the distributions of ellipticities and kinematic misalignments of galactic projections, as well as the intrinsic shapes and rotation of the simulated galaxies. Our results for the projections of galaxies display clear trends of an overall increase of kinematic misalignment and a slight decrease of ellipticity for fast rotators with increasing masses, while revealing no clear distinction between slow rotators of different mass. It is also found that the number of very slow rotators with large ellipticities is much larger than found in observations. The intrinsic properties of the galaxies are then analysed. The results for the intrinsic shapes of the galaxies are mostly consistent with previous results inferred from observational data. The distributions of intrinsic misalignment of the galaxies suggest that some of the galaxies produced by Illustris have significant rotation around their medium axes. Further analysis reveals that most of these galaxies display signs of non-equilibrium. We then study the evolution of the intrinsic misalignments and shapes of three specific Illustris galaxies, which we consider as typical ones, along the main progenitor line of their merger trees, revealing how mergers influence the intrinsic shapes and kinematics: the spin axis in general stays close to the shortest axis, and tends to quickly relax to such an equilibrium state within a few dynamical times of the galaxy after major perturbations; triaxiality and intrinsic flatness in general decrease with time, however, sometimes increases occur that are clearly seen to correlate with major merger events.}, -archivePrefix = {arXiv}, -arxivId = {1908.01102}, -author = {Yang, Lisiyuan and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hongyu}, -doi = {10.1093/mnras/stz2156}, -eprint = {1908.01102}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: kinematics and dynamics,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -number = {1}, -pages = {534--547}, -title = {{Photometric and kinematic misalignments and their evolution among fast and slow rotators in the illustris simulation}}, -volume = {489}, -year = {2019} -} -@article{Dunne2011, -abstract = {We present the first direct and unbiased measurement of the evolution of the dust mass function of galaxies over the past 5 billion years of cosmic history using data from the Science Demonstration Phase of the Herschel-Astrophysical Terahertz Large Area Survey (Herschel-ATLAS). The sample consists of galaxies selected at 250 m which have reliable counterparts from the Sloan Digital Sky Survey (SDSS) at z < 0.5, and contains 1867 sources. Dust masses are calculated using both a single-temperature grey-body model for the spectral energy distribution and also a model with multiple temperature components. The dust temperature for either model shows no trend with redshift. Splitting the sample into bins of redshift reveals a strong evolution in the dust properties of the most massive galaxies. At z= 0.4-0.5, massive galaxies had dust masses about five times larger than in the local Universe. At the same time, the dust-to-stellar mass ratio was about three to four times larger, and the optical depth derived from fitting the UV-sub-mm data with an energy balance model was also higher. This increase in the dust content of massive galaxies at high redshift is difficult to explain using standard dust evolution models and requires a rapid gas consumption time-scale together with either a more top-heavy initial mass function (IMF), efficient mantle growth, less dust destruction or combinations of all three. This evolution in dust mass is likely to be associated with a change in overall interstellar medium mass, and points to an enhanced supply of fuel for star formation at earlier cosmic epochs. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1012.5186}, -author = {Dunne, L. and Gomez, H. L. and da Cunha, E. and Charlot, S. and Dye, S. and Eales, S. and Maddox, S. J. and Rowlands, K. and Smith, D. J.B. and Auld, R. and Baes, M. and Bonfield, D. G. and Bourne, N. and Buttiglione, S. and Cava, A. and Clements, D. L. and Coppin, K. E.K. and Cooray, A. and Dariush, A. and de Zotti, G. and Driver, S. and Fritz, J. and Geach, J. and Hopwood, R. and Ibar, E. and Ivison, R. J. and Jarvis, M. J. and Kelvin, L. and Pascale, E. and Pohlen, M. and Popescu, C. and Rigby, E. E. and Robotham, A. and Rodighiero, G. and Sansom, A. E. and Serjeant, S. and Temi, P. and Thompson, M. and Tuffs, R. and van der Werf, P. and Vlahakis, C.}, -doi = {10.1111/j.1365-2966.2011.19363.x}, -eprint = {1012.5186}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,ISM: evolution,Submillimetre: galaxies}, -number = {2}, -pages = {1510--1533}, -pmid = {276971300024}, -title = {{Herschel -ATLAS: Rapid evolution of dust in galaxies over the last 5 billion years}}, -volume = {417}, -year = {2011} -} -@article{Schaye2014, -abstract = {We introduce the Virgo Consortium's Evolution and Assembly of GaLaxies and their Environments (EAGLE) project, a suite of hydrodynamical simulations that follow the formation of galaxies and supermassive black holes in cosmologically representative volumes of a standard $\Lambda$ cold dark matter universe. We discuss the limitations of such simulations in light of their finite resolution and poorly constrained subgrid physics, and how these affect their predictive power. One major improvement is our treatment of feedback from massive stars and active galactic nuclei (AGN) in which thermal energy is injected into the gas without the need to turn off cooling or decouple hydrodynamical forces, allowing winds to develop without predetermined speed or mass loading factors. Because the feedback efficiencies cannot be predicted from first principles, we calibrate them to the present-day galaxy stellar mass function and the amplitude of the galaxy-central black hole mass relation, also taking galaxy sizes into account. The observed galaxy stellar mass function is reproduced to ≲0.2 dex over the full resolved mass range, 108 < M*/M⊙ ≲ 1011, a level of agreement close to that attained by semi-analytic models, and unprecedented for hydrodynamical simulations. We compare our results to a representative set of low-redshift observables not considered in the calibration, and find good agreement with the observed galaxy specific star formation rates, passive fractions, Tully-Fisher relation, total stellar luminosities of galaxy clusters, and column density distributions of intergalactic C IV and O VI. While the mass-metallicity relations for gas and stars are consistent with observations for M* ≳ 109 M⊙ (M* ≳ 1010 M⊙ at intermediate resolution), they are insufficiently steep at lower masses. For the reference model, the gas fractions and temperatures are too high for clusters of galaxies, but for galaxy groups these discrepancies can be resolved by adopting a higher heating temperature in the subgrid prescription for AGN feedback. The EAGLE simulation suite, which also includes physics variations and higher resolution zoomed-in volumes described elsewhere, constitutes a valuable new resource for studies of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1407.7040}, -author = {Schaye, Joop and Crain, Robert A. and Bower, Richard G. and Furlong, Michelle and Schaller, Matthieu and Theuns, Tom and {Dalla Vecchia}, Claudio and Frenk, Carlos S. and Mccarthy, I. G. and Helly, John C. and Jenkins, Adrian and Rosas-Guevara, Y. M. and White, Simon D.M. and Baes, Maarten and Booth, C. M. and Camps, Peter and Navarro, Julio F. and Qu, Yan and Rahmati, Alireza and Sawala, Till and Thomas, Peter A. and Trayford, James}, -doi = {10.1093/mnras/stu2058}, -eprint = {1407.7040}, -isbn = {047149870X}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {1}, -pages = {521--554}, -title = {{The EAGLE project: Simulating the evolution and assembly of galaxies and their environments}}, -volume = {446}, -year = {2015} -} -@article{Newman2012a, -abstract = {The presence of extremely compact galaxies at z ∼ 2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 galaxies selected with 0.4 < z < 2.5 and stellar masses M* > 1010.7 M {\textperiodcentered} in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and the mean size of these systems at fixed stellar mass grows by a factor of 3.5 0.3 over this redshift interval. The data are sufficiently deep to identify companions to these hosts whose stellar masses are ten times smaller. By searching for these around 404 quiescent hosts within a physical annulus 10 h -1 kpc < R < 30 h -1 kpc, we estimate the minor merger rate over 0.4 < z < 2. We find that 13%-18% of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6% ± 2% per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers may explain most of the size evolution observed at z ≲ 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes. {\textcopyright} 2012 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1110.1637}, -author = {Newman, Andrew B. and Ellis, Richard S. and Bundy, Kevin and Treu, Tommaso}, -doi = {10.1088/0004-637X/746/2/162}, -eprint = {1110.1637}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Newman et al. - 2012 - Can minor merging account for the size growth of quiescent galaxies New results from the CANDELS survey.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: structure}, -number = {2}, -title = {{Can minor merging account for the size growth of quiescent galaxies? New results from the CANDELS survey}}, -volume = {746}, -year = {2012} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M{\textgreater}10{\^{}}11 M{\_}sun) galaxies at 1.7{\textless}z{\textless}3 utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our sample is almost an order of magnitude larger than previous studies at these redshifts, providing the first statistical study of massive galaxy sizes at z{\textgreater}2, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n{\textless}2) and spheroid-like (n{\textgreater}2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z{\$\sim${}}2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z{\textgreater}2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ({\$\sim${}}2x10{\^{}}10 M{\_}sun kpc{\^{}}-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J and Bouwens, Rychard J and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -isbn = {1005-0302}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61----L64}, -title = {{ Size Evolution of the Most Massive Galaxies at 1.7 {\textless} z {\textless} 3 from GOODS NICMOS Survey Imaging }}, -url = {http://arxiv.org/abs/0807.4141%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently-discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially-interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorised according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}10{\^{}}11 Msun to {\textgreater}10{\^{}}13 Msun. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}10{\^{}}11 Msun. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW05). The two low-mass outliers are J0206-095 (SW19) and J2217+015 (SW42); if these two are indeed lenses, they probe an interesting regime of very low star-formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Reines2015, -abstract = {Scaling relations between central black hole (BH) mass and host galaxy properties are of fundamental importance to studies of BH and galaxy evolution throughout cosmic time. Here we investigate the relationship between BH mass and host galaxy total stellar mass using a sample of 262 broad-line active galactic nuclei (AGNs) in the nearby universe (z {\textless} 0.055), as well as 79 galaxies with dynamical BH masses. The vast majority of our AGN sample is constructed using Sloan Digital Sky Survey spectroscopy and searching for Seyfert-like narrow-line ratios and broad H$\alpha$ emission. BH masses are estimated using standard virial techniques. We also include a small number of dwarf galaxies with total stellar masses Mstellar ≲ 109.5 Mo and a subsample of the reverberation-mapped AGNs. Total stellar masses of all 341 galaxies are calculated in the most consistent manner feasible using color-dependent mass-to-light ratios. We find a clear correlation between BH mass and total stellar mass for the AGN host galaxies, with MBH ∝ Mstellar, similar to that of early-type galaxies with dynamically detected BHs. However, the relation defined by the AGNs has a normalization that is lower by more than an order of magnitude, with a BH-to-total stellar mass fraction of MBH/Mstellar ∼ 0.025{\%} across the stellar mass range 108 ≤ Mstellar/Mo ≤ 1012. This result has significant implications for studies at high redshift and cosmological simulations in which stellar bulges cannot be resolved.}, -archivePrefix = {arXiv}, -arxivId = {1508.06274}, -author = {Reines, Amy E and Volonteri, Marta}, -doi = {10.1088/0004-637X/813/2/82}, -eprint = {1508.06274}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: Seyfert,galaxies: active,galaxies: evolution,galaxies: nuclei}, -number = {2}, -title = {{RELATIONS between CENTRAL BLACK HOLE MASS and TOTAL GALAXY STELLAR MASS in the LOCAL UNIVERSE}}, -volume = {813}, -year = {2015} -} -@article{Pontzen2015a, -abstract = {Galaxies and the dark matter haloes that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealized calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter core-creation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are 'maximally stable', i.e. that do not evolve at first order when external potentials (which arise from baryons, large-scale tidal fields or infalling substructure) are applied. We show that a spherically symmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for near-isotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealized spherically symmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter haloes (formed in collisionless cosmological simulations) nearly attain our maximally stable limit, but their evolution freezes out before reaching it.}, -archivePrefix = {arXiv}, -arxivId = {1502.07356}, -author = {Pontzen, Andrew and Read, Justin I and Teyssier, Romain and Governato, Fabio and Gualandris, Alessia and Roth, Nina and Devriendt, Julien}, -doi = {10.1093/mnras/stv1032}, -eprint = {1502.07356}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {1366--1379}, -title = {{Milking the spherical cow - on aspherical dynamics in spherical coordinates}}, -volume = {451}, -year = {2015} -} -@article{Lanusse2017a, -abstract = {Galaxy-scale strong gravitational lensing can not only provide a valuable probe of the dark matter distribution of massive galaxies, but also provide valuable cosmological constraints, either by studying the population of strong lenses or by measuring time delays in lensed quasars. Due to the rarity of galaxy-scale strongly lensed systems, fast and reliable automated lens finding methods will be essential in the era of large surveys such as Large Synoptic Survey Telescope, Euclid and Wide-Field Infrared Survey Telescope. To tackle this challenge, we introduce CMU DeepLens, a new fully automated galaxy-galaxy lens finding method based on deep learning. This supervised machine learning approach does not require any tuning after the training step which only requires realistic image simulations of strongly lensed systems. We train and validate our model on a set of 20 000 LSST-like mock observations including a range of lensed systems of various sizes and signal-to-noise ratios (S/N).We find on our simulated data set that for a rejection rate of non-lenses of 99 per cent, a completeness of 90 per cent can be achieved for lenses with Einstein radii larger than 1.4 arcsec and S/N larger than 20 on individual g-band LSST exposures. Finally, we emphasize the importance of realistically complex simulations for training such machine learning methods by demonstrating that the performance of models of significantly different complexities cannot be distinguished on simpler simulations.}, -archivePrefix = {arXiv}, -arxivId = {1703.02642}, -author = {Lanusse, Fran{\c{c}}ois and Ma, Quanbin and Li, Nan and Collett, Thomas E and Li, Chun Liang and Ravanbakhsh, Siamak and Mandelbaum, Rachel and P{\'{o}}czos, Barnab{\'{a}}s}, -doi = {10.1093/mnras/stx1665}, -eprint = {1703.02642}, -isbn = {0021-9258 (Print){\$}\backslash{\$}r0021-9258 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: statistical,gravitational lensing: strong}, -number = {3}, -pages = {3895--3906}, -pmid = {10913147}, -title = {{CMU DeepLens: Deep learning for automatic image-based galaxy-galaxy strong lens finding}}, -url = {http://arxiv.org/abs/1703.02642}, -volume = {473}, -year = {2018} -} -@article{Li2017, -abstract = {We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier {\$}\backslashrm ATLAS{\^{}}{\{}3D{\}}{\$} results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients.}, -archivePrefix = {arXiv}, -arxivId = {1703.04894}, -author = {Li, Hongyu and Ge, Junqiang and Mao, Shude and Cappellari, Michele and Long, R J and Li, Ran and Emsellem, Eric and Dutton, Aaron A and Li, Cheng and Bundy, Kevin and Thomas, Daniel and Drory, Niv and Lopes, Alexandre Roman}, -doi = {10.3847/1538-4357/aa662a}, -eprint = {1703.04894}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {77}, -title = {{SDSS-IV MaNGA: Variation of the Stellar Initial Mass Function in Spiral and Early-type Galaxies}}, -url = {http://arxiv.org/abs/1703.04894%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa662a}, -volume = {838}, -year = {2017} -} -@article{Rybak2015, -abstract = {We present a sub-100 pc-scale analysis of the CO molecular gas emission and kinematics of the gravitational lens system SDP.81 at redshift 3.042 using Atacama Large Millimetre/submillimetre Array (ALMA) science verification data and a visibility-plane lens reconstruction technique. We find clear evidence for an excitation dependent structure in the unlensed molecular gas distribution, with emission in CO (5-4) being significantly more diffuse and structured than in CO (8-7). The intrinsic line luminosity ratio is r_8-7/5-4 = 0.30 +/- 0.04, which is consistent with other low-excitation starbursts at z $\sim$ 3. An analysis of the velocity fields shows evidence for a star-forming disk with multiple velocity components that is consistent with a merger/post-coalescence merger scenario, and a dynamical mass of M(< 1.56 kpc) = 1.6 +/- 0.6 x 10^10 M_sol . Source reconstructions from ALMA and the Hubble Space Telescope show that the stellar component is offset from the molecular gas and dust components. Together with Karl G. Jansky Very Large Array CO (1-0) data, they provide corroborative evidence for a complex $\sim$2 kpc-scale starburst that is embedded within a larger $\sim$15 kpc structure.}, -archivePrefix = {arXiv}, -arxivId = {1506.01425}, -author = {Rybak, M. and Vegetti, S. and McKean, J. P. and Andreani, P. and White, S. D M}, -doi = {10.1093/mnrasl/slv092}, -eprint = {1506.01425}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Galaxies: high redshift,Gravitational lensing: strong,Submillimetre: galaxies}, -number = {1}, -pages = {L26--L30}, -title = {{ALMA imaging of SDP.81-II. A pixelated reconstruction of the CO emission lines}}, -volume = {453}, -year = {2015} -} -@article{Nightingale2021a, -abstract = {A major trend in academia and data science is the rapid adoption of Bayesian statistics for data analysis and modeling, leading to the development of probabilistic programming languages (PPL). A PPL provides a framework that allows users to easily specify a probabilistic model and perform inference automatically. PyAutoFit is a Python-based PPL which interfaces with all aspects of the modeling (e.g., the model, data, fitting procedure, visualization, results) and therefore provides complete management of every aspect of modeling. This includes composing high-dimensionality models from individual model components, customizing the fitting procedure and performing data augmentation before a model-fit. Advanced features include database tools for analysing large suites of modeling results and exploiting domain-specific knowledge of a problem via non-linear search chaining. Accompanying PyAutoFit is the autofit workspace (see https://github.com/Jammy2211/autofit_workspace), which includes example scripts and the HowToFit lecture series which introduces non-experts to model-fitting and provides a guide on how to begin a project using PyAutoFit. Readers can try PyAutoFit right now by going to the introduction Jupyter notebook on Binder (see https://mybinder.org/v2/gh/Jammy2211/autofit_workspace/HEAD) or checkout our readthedocs(see https://pyautofit.readthedocs.io/en/latest/) for a complete overview of PyAutoFit's features.}, -archivePrefix = {arXiv}, -arxivId = {2102.04472}, -author = {Nightingale, James. and Hayes, Richard and Griffiths, Matthew}, -doi = {10.21105/joss.02550}, -eprint = {2102.04472}, -file = {:C\:/Users/Jammy/Documents/Papers/Software/PyAutoFit.pdf:pdf}, -issn = {2475-9066}, -journal = {J. Open Source Softw.}, -number = {58}, -pages = {2550}, -title = {{PyAutoFit: A Classy Probabilistic Programming Language for Model Composition and Fitting}}, -volume = {6}, -year = {2021} -} -@article{Rizzo2018, -abstract = {We present a 3D Bayesian method to model the kinematics of strongly lensed galaxies from spatially resolved emission-line observations. This technique enables us to simultaneously recover the lens-mass distribution and the source kinematics directly from the 3D data cube. We have tested this new method with simulated OSIRIS observations for nine star-forming lensed galaxies with different kinematic properties. The simulated rotation curves span a range of shapes that are prototypes of different morphological galaxy types, from dwarf to massive spiral galaxies. We have found that the median relative accuracy on the inferred lens and kinematic parameters are at the level of 1 and 2 per cent, respectively. We have also tested the robustness of the technique against different inclination angles, signal-to-noise ratios, the presence of warps, or non-circular motions and we have found that the accuracy stays within a few per cent in most cases. This technique represents a significant step forward with respect to the methods used until now, as the lens parameters and the kinematics of the source are derived from the same 3D data. This enables us to study the possible degeneracies between the two and estimate the uncertainties on all model parameters consistently.}, -archivePrefix = {arXiv}, -arxivId = {1809.07340}, -author = {Rizzo, Francesca and Vegetti, Simona and Fraternali, Filippo and {Di Teodoro}, Enrico}, -doi = {10.1093/MNRAS/STY2594}, -eprint = {1809.07340}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rizzo et al. - 2018 - A novel 3D technique to study the kinematics of lensed galaxies.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: high-redshift,Galaxies: kinematics and dynamics,Gravitational lensing: strong -methods: data analy}, -number = {4}, -pages = {5606--5629}, -title = {{A novel 3D technique to study the kinematics of lensed galaxies}}, -url = {http://arxiv.org/abs/1809.07340%0Ahttp://dx.doi.org/10.1093/mnras/sty2594}, -volume = {481}, -year = {2018} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brooks, Christensen - 2015 - Bulge formation via mergers in cosmological simulations.pdf:pdf}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Pontzen2017, -abstract = {We show how the interplay between active galactic nuclei (AGNs) and merger history determines whether a galaxy quenches star formation (SF) at high redshift. We first simulate, in a full cosmological context, a galaxy of total dynamical mass Mvir = 1012M⊙ at z = 2. Then we systematically alter the accretion history of the galaxy by minimally changing the linear overdensity in the initial conditions. This 'genetic modification' approach allows the generation of three sets of $\Lambda$ CDM initial conditions leading to maximum merger ratios of 1:10, 1:5 and 2:3, respectively. The changes leave the final halo mass, large-scale structure and local environment unchanged, providing a controlled numerical experiment. Interaction between the AGN physics and mergers in the three cases leads, respectively, to a star-forming, temporarily quenched and permanently quenched galaxy. However, the differences do not primarily lie in the black hole accretion rates, but in the kinetic effects of the merger: the galaxy is resilient against AGN feedback unless its gaseous disc is first disrupted. Typical accretion rates are comparable in the three cases, falling below 0.1M⊙ yr-1, equivalent to around 2 per cent of the Eddington rate or 10-3 times the pre-quenching star formation rate, in agreement with observations. This low level of black hole accretion can be sustained even when there is insufficient dense cold gas for SF. Conversely, supernova feedback is too distributed to generate outflows in high-mass systems, and cannot maintain quenching over periods longer than the halo gas cooling time.}, -archivePrefix = {arXiv}, -arxivId = {1607.02507}, -author = {Pontzen, Andrew and Tremmel, Michael and Roth, Nina and Peiris, Hiranya V and Saintonge, Am{\'{e}}lie and Volonteri, Marta and Quinn, Tom and Governato, Fabio}, -doi = {10.1093/mnras/stw2627}, -eprint = {1607.02507}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: star formation,Galaxies: stellar content}, -number = {1}, -pages = {547--558}, -title = {{How to quench a galaxy}}, -volume = {465}, -year = {2017} -} -@article{Keres2009b, -abstract = {We compare the properties of galaxies that form in a cosmological simulation without strong feedback to observations of the z = 0 galaxy population. We confirm previous findings that models without strong feedback overproduce the observed galaxy baryonic mass function, especially at the low- and high-mass extremes. Through post-processing we investigate what kinds of feedback would be required to reproduce the statistics of observed galaxy masses and star formation rates. To mimic an extreme form of 'preventive' feedback, such as a highly efficient active galactic nucleus 'radio mode', we remove all baryonic mass that was originally accreted from shock-heated gas ('hot-mode' accretion). This removal does not bring the high-mass end of the galaxy mass function into agreement with observations because much of the stellar mass in these systems formed at high redshift from baryons that originally accreted via 'cold mode' on to lower mass progenitors. An efficient 'ejective' feedback mechanism, such as supernova-driven galactic winds, must reduce the masses of these progenitors before they merge to form today's massive galaxies. Feedback must also reduce the masses of lower mass z = 0 galaxies, which assemble at lower redshifts and have much lower star formation rates. If we monotonically remap galaxy masses to reproduce the observed mass function, but retain the simulation-predicted star formation rates, we obtain fairly good agreement with the observed sequence of star-forming galaxies. However, we fail to recover the observed population of passive, low star formation rate galaxies, especially at the high-mass end. Suppressing all hot-mode accretion improves the agreement for high-mass galaxies, but it worsens the agreement at intermediate masses. Reproducing these z = 0 observations requires a feedback mechanism that dramatically suppresses star formation in a fraction of galaxies, increasing with mass, while leaving star formation rates of other galaxies essentially unchanged. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.1880}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Dav{\'{e}}, Romeel and Fardal, Mark and Weinberg, David H.}, -doi = {10.1111/j.1365-2966.2009.14924.x}, -eprint = {0901.1880}, -isbn = {doi:10.1111/j.1365-2966.2009.14541.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function, mass function,Methods: numerical - cooling flows}, -month = {jul}, -number = {4}, -pages = {2332--2344}, -title = {{Galaxies in a simulated $\Lambda$cDM universe - II. Observable properties and constraints on feedback}}, -volume = {396}, -year = {2009} -} -@article{Johnston2016, -abstract = {With the availability of large integral field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, howgalaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present bulge-disc decomposition of IFU data cubes (BUDDI), a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GALFITM, a modified form of GALFIT which can fit multiwaveband images simultaneously. The benefit of this technique over traditional multiwaveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the Sloan Digital Sky Survey-IV Mapping Nearby Galaxies atAPO(MaNGA)survey with redshifts z < 0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec full width at half-maximum and field of view of > 22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from theMaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data.}, -archivePrefix = {arXiv}, -arxivId = {1611.00609}, -author = {Johnston, Evelyn J. and H{\"{a}}u{\ss}ler, Boris and Arag{\'{o}}n-Salamanca, Alfonso and Merrifield, Michael R. and Bamford, Steven and Bershady, Matthew A. and Bundy, Kevin and Drory, Niv and Fu, Hai and Law, David and Nitschelm, Christian and Thomas, Daniel and Lopes, Alexandre Roman and Wake, David and Yan, Renbin}, -doi = {10.1093/mnras/stw2823}, -eprint = {1611.00609}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Johnston et al. - 2017 - SDSS-IV MaNGA Bulge-disc decomposition of IFU data cubes (BUDDI)(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content,Galaxies: structure}, -number = {2}, -pages = {2317--2341}, -title = {{SDSS-IV MaNGA: Bulge-disc decomposition of IFU data cubes (BUDDI)}}, -url = {http://arxiv.org/abs/1611.00609%0Ahttp://dx.doi.org/10.1093/mnras/stw2823}, -volume = {465}, -year = {2017} -} -@article{Version2018, -archivePrefix = {arXiv}, -arxivId = {arXiv:1306.4330v2}, -author = {Version, Raft}, -eprint = {arXiv:1306.4330v2}, -title = {{Constraining sub-parsec binary supermassive black holes in quasars with multi-epoch spectroscopy. i. the general quasar population}}, -year = {2018} -} -@article{Schombert2013, -abstract = { Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the S{\'{e}}rsic r 1/ n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the S{\'{e}}rsic r 1/ n model produces good fits to the core regions of ellipticals ( r {\textless} r half ), but is an inadequate function for the entire profile of an elliptical from core to halo due to competing effects on the S{\'{e}}rsic n index and the fact that the interior shape of an elliptical is only weakly correlated with its halo shape. In addition, there are a wide range of S{\'{e}}rsic parameters that will equally describe the shape of the outer profile, degrading the S{\'{e}}rsic model's usefulness as a describer of the entire profile. Empirically determined parameters, such as half-light radius and total luminosity, have less scatter than fitting function variables. The scaling relations for ellipticals are often non-linear, but for ellipticals brighter than M J {\textless} −23 the following structural relations are found: L ∝ r 0.8±0.1 , L ∝ $\Sigma$ −0.5±0.1 , and $\Sigma$ ∝ r −1.5±0.1 . }, -archivePrefix = {arXiv}, -arxivId = {1303.4710}, -author = {Schombert, J M}, -doi = {10.1017/pas.2013.010}, -eprint = {1303.4710}, -issn = {13233580}, -journal = {Publications of the Astronomical Society of Australia}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: star formation,galaxies: structure}, -number = {1}, -title = {{The structure of galaxies: II. Fitting functions and scaling relations for ellipticals}}, -url = {http://arxiv.org/abs/1303.4710%7B%5C%25%7D0Ahttp://dx.doi.org/10.1017/pas.2013.010}, -volume = {30}, -year = {2013} -} -@article{Schneider2014b, -abstract = {Strong gravitational lensing of sources with different redshifts has been used to determine cosmological distance ratios, which in turn depend on the expansion history. Hence, such systems are viewed as potential tools for constraining cosmological parameters. Here we show that in lens systems with two distinct source redshifts, of which the nearest one contributes to the light deflection toward the more distant one, there exists an invariance transformation that leaves all strong-lensing observables unchanged (except for the product of time delay and Hubble constant), generalizing the well-known mass-sheet transformation in single-plane lens systems. The transformation preserves the relative location of mass and light. All time delays (from sources on both planes) scale with the same factor-time-delay ratios are therefore invariant under the mass-sheet transformation. Changing cosmological parameters, and thus distance ratios, is essentially equivalent to such a mass-sheet transformation. As an example, we discuss the double-source plane system SDSSJ0946+1006, which has recently been studied by Collett and Auger, and show that variations of cosmological parameters within reasonable ranges lead to only a weak mass-sheet transformation in both lens planes. Hence, the ability to extract cosmological information from such systems depends heavily on the ability to break the mass-sheet degeneracy. {\textcopyright} 2014 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1406.6152}, -author = {Schneider, Peter}, -doi = {10.1051/0004-6361/201424450}, -eprint = {1406.6152}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Cosmological parameters,Gravitational lensing: strong}, -month = {aug}, -pages = {L2}, -title = {{Can one determine cosmological parameters from multi-plane strong lens systems}}, -url = {http://arxiv.org/abs/1406.6152%0Ahttp://dx.doi.org/10.1051/0004-6361/201424450}, -volume = {568}, -year = {2014} -} -@article{Yang2006, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd (2005), but inconsistent with several previous studies who detected a preferential minor axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M{\textless}inf{\textgreater}*{\textless}/inf{\textgreater} {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M{\textless}inf{\textgreater}⊙{\textless}/inf{\textgreater} galaxies at 1 {\textless} z {\textless} 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 {\textless} z {\textless} 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.5221}, -volume = {444}, -year = {2014} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter (CDM) galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes possess a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a $\Lambda$CDM universe. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R and Eke, Vincent R and Frenk, Carlos S and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{Barro2013, -abstract = {We combine high-resolution HST/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (log(M*) {\textgreater} 10) galaxies at redshifts z = 1.4 - 3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5 - 3. At z {\textgreater} 2 most cSFGs have specific star-formation rates (sSFR = 10{\^{}}-9 yr{\^{}}-1) half that of typical, massive SFGs at the same epoch, and host X-ray luminous AGN 30 times ({\$\sim${}}30{\%}) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 10{\^{}}8 yr). The cSFGs are continuously being formed at z = 2 - 3 and fade to cQGs by z = 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary scenarios of QG formation: an early (z {\textgreater} 2), fast-formation path of rapidly-quenched cSFGs that evolve into cQGs that later enlarge within the quiescent phase, and a slow, late-arrival (z {\textless} 2) path for SFGs to form QGs without passing through a compact state.}, -archivePrefix = {arXiv}, -arxivId = {1206.5000}, -author = {Barro, Guillermo and Faber, S M and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Koo, David C and Williams, Christina C and Kocevski, Dale D and Trump, Jonathan R and Mozena, Mark and McGrath, Elizabeth and {Van Der Wel}, Arjen and Wuyts, Stijn and Bell, Eric F and Croton, Darren J and Daniel, Ceverino and Dekel, Avishai and Ashby, M L N and Cheung, Edmond and Ferguson, Henry C and Fontana, Adriano and Fang, Jerome and Giavalisco, Mauro and Grogin, Norman A and Guo, Yicheng and Hathi, Nimish P and Hopkins, Philip F and Huang, Kuang Han and Koekemoer, Anton M and Kartaltepe, Jeyhan S and Lee, Kyoung Soo and Newman, Jeffrey A and Porter, Lauren A and Primack, Joel R and Ryan, Russell E and Rosario, David and Somerville, Rachel S and Salvato, Mara and Hsu, Li Ting}, -doi = {10.1088/0004-637X/765/2/104}, -eprint = {1206.5000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: high-redshift,galaxies: photometry,galaxies: starburst}, -number = {2}, -pmid = {7117407}, -title = {{Candels: The progenitors of compact quiescent galaxies at Z ∼ 2}}, -volume = {765}, -year = {2013} -} -@article{Liao2016, -abstract = {The standard galaxy formation theory assumes that baryons and dark matter are initially well-mixed before becoming segregated due to radiative cooling. We use non-radiative hydrodynamical simulations to explicitly examine this assumption and find that baryons and dark matter can also be segregated because of different physics obeyed by gas and dark matter during the build-up of the halo. As a result, baryons in many haloes do not originate from the same Lagrangian region as the dark matter. When using the fraction of corresponding dark matter and gas particles in the initial conditions (the "paired fraction") as a proxy of the dark matter and gas segregation strength of a halo, on average about {\$}25{\$} percent of the baryonic and dark matter of the final halo are segregated in the initial conditions. This is at odds with the assumption of the standard galaxy formation model. A consequence of this effect is that the baryons and dark matter of the same halo initially experience different tidal torques and thus their angular momentum vectors are often misaligned. The degree of the misalignment is largely preserved during later halo assembly and can be understood with the tidal torque theory. The result challenges the precision of some semi-analytical approaches which utilize dark matter halo merger trees to infer properties of gas associated to dark matter haloes.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.07592}, -author = {Liao, Shihong and Gao, Liang and Frenk, Carlos S and Guo, Qi and Wang, Jie}, -doi = {10.1093/mnras/stx1391}, -eprint = {1610.07592}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {2}, -pages = {2262--2269}, -title = {{The segregation of baryons and dark matter during halo assembly}}, -url = {http://arxiv.org/abs/1610.07592}, -volume = {470}, -year = {2017} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M * = 1010.2 to 1012.0 M . We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority (≳75{\%}) of elliptical galaxies is not well described by a single S{\'{e}}rsic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (Re ∼ 1 kpc) inner component with luminosity fraction f 0.1-0.15; an intermediate-scale (Re 2.5 kpc) middle component with f 0.2-0.25; and a dominant (f = 0.6), extended (Re 10 kpc) outer envelope. All subcomponents have average S{\'{e}}rsic indices n 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies. {\textcopyright}2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C and Peng, Chien Y and Li, Zhao Yu and Barth, Aaron J}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{Cappellari2011, -abstract = {The ATLAS3D project is a multiwavelength survey combined with a theoretical modelling effort. The observations span from the radio to the millimetre and optical, and provide multicolour imaging, two-dimensional kinematics of the atomic (Hi), molecular (CO) and ionized gas (H$\beta$, [Oiii] and [Ni]), together with the kinematics and population of the stars (H$\beta$, Fe5015 and Mg b), for a carefully selected, volume-limited (1.16 × 105Mpc3) sample of 260 early-type (elliptical E and lenticular S0) galaxies (ETGs). The models include semi-analytic, N-body binary mergers and cosmological simulations of galaxy formation. Here we present the science goals for the project and introduce the galaxy sample and the selection criteria. The sample consists of nearby (D < 42Mpc, |$\delta$- 29°| < 35°, |b| > 15°) morphologically selected ETGs extracted from a parent sample of 871 galaxies (8 per cent E, 22 per cent S0 and 70 per cent spirals) brighter than MK < -21.5mag (stellar mass M{black star}≳ 6 ×109M⊙). We analyse possible selection biases and we conclude that the parent sample is essentially complete and statistically representative of the nearby galaxy population. We present the size-luminosity relation for the spirals and ETGs and show that the ETGs in the ATLAS3D sample define a tight red sequence in a colour-magnitude diagram, with few objects in the transition from the blue cloud. We describe the strategy of the SAURON integral field observations and the extraction of the stellar kinematics with the ppxf method. We find typical 1$\sigma$ errors of $\Delta$V≈ 6kms-1, $\Delta$$\sigma$≈ 7kms-1, $\Delta$h3≈$\Delta$h4≈ 0.03 in the mean velocity, the velocity dispersion and Gauss-Hermite (GH) moments for galaxies with effective dispersion $\sigma$e≳ 120kms-1. For galaxies with lower $\sigma$e (≈40 per cent of the sample) the GH moments are gradually penalized by ppxf towards zero to suppress the noise produced by the spectral undersampling and only V and $\sigma$ can be measured. We give an overview of the characteristics of the other main data sets already available for our sample and of the ongoing modelling projects. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1012.1551}, -author = {Cappellari, Michele and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Mcdermid, Richard M. and Scott, Nicholas and {Verdoes Kleijn}, G. A. and Young, Lisa M. and Alatalo, Katherine and Bacon, R. and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and Lablanche, Pierre Yves and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Serra, Paolo and Weijmans, Anne Marie}, -doi = {10.1111/j.1365-2966.2010.18174.x}, -eprint = {1012.1551}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: distances and redshifts,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {813--836}, -title = {{The ATLAS3D project - I. A volume-limited sample of 260 nearby early-type galaxies: Science goals and selection criteria}}, -volume = {413}, -year = {2011} -} -@article{Veale2017a, -abstract = {We analyse the environmental properties of 370 local early-type galaxies (ETGs) in theMASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute K-band magnitude -21.5 ≳ MK ≳ -26.6, or stellar mass 8 × 109 ≲ M* ≲ 2 × 1012M⊙. We find these galaxies to reside in a diverse range of environments measured by four methods: group membership (whether a galaxy is a brightest group/cluster galaxy, satellite or isolated), halo mass, large-scale mass density (measured over a fewMpc) and local mass density (measured within the Nth neighbour). The spatially resolved IFS stellar kinematics provide robust measurements of the spin parameter $\lambda$e and enable us to examine the relationship among $\lambda$e, M* and galaxy environment. We find a strong correlation between $\lambda$e and M*, where the average $\lambda$e decreases from {\$\sim${}}0.4 to below 0.1 with increasing mass, and the fraction of slow rotators fslow increase from {\$\sim${}}10 to 90 per cent. We show for the first time that at fixed M*, there are almost no trends between galaxy spin and environment; the apparent kinematic morphology-density relation for ETGs is therefore primarily driven by M* and is accounted for by the joint correlations between M* and spin, and between M* and environment. A possible exception is that the increased fslow at high local density is slightly more than expected based only on these joint correlations. Our results suggest that the physical processes responsible for building up the present-day stellar masses of massive galaxies are also very efficient at reducing their spin, in any environment.}, -archivePrefix = {arXiv}, -arxivId = {1703.08573}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and McConnell, Nicholas and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/mnras/stx1639}, -eprint = {1703.08573}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {1428--1445}, -title = {{The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxies}}, -url = {http://arxiv.org/abs/1703.08573%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1639}, -volume = {471}, -year = {2017} -} -@article{2001es, -author = {عامر, د. وفاء محروس}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/عامر - 2001 - No Title المعالجة الحيوية للمولوثات البيئية(9).pdf:pdf}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Kochanek2021a, -abstract = {The two properties of the radial mass distribution of a gravitational lens that are well constrained by Einstein rings are the Einstein radius RE and $\zeta$2 = RE$\alpha$″(RE)/(1 - $\kappa$E), where $\alpha$″(RE) and $\kappa$E are the second derivative of the deflection profile and the convergence at RE, respectively. However, if there is a tight mathematical relationship between the radial mass profile and the angular structure, as is true of ellipsoids, an Einstein ring can appear to strongly distinguish radial mass distributions with the same $\zeta$2. This problem is beautifully illustrated by the ellipsoidal models in Millon et al. When using Einstein rings to constrain the radial mass distribution, the angular structure of the models must contain all the degrees of freedom expected in nature (e.g. external shear, different ellipticities for the stars and the dark matter, modest deviations from elliptical structure, modest twists of the axes, modest ellipticity gradients, etc.) that work to decouple the radial and angular structures of the gravity. Models of Einstein rings with too few angular degrees of freedom will lead to strongly biased likelihood distinctions between radial mass distributions and very precise but inaccurate estimates of H0 based on gravitational lens time delays.}, -archivePrefix = {arXiv}, -arxivId = {2003.08395}, -author = {Kochanek, C. S.}, -doi = {10.1093/mnras/staa4033}, -eprint = {2003.08395}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Kochanek2021radialdog.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cosmological parameters,distance scale,gravitational lensing: strong}, -number = {4}, -pages = {5021--5028}, -publisher = {Oxford University Press}, -title = {{Overconstrained models of time delay lenses redux: How the angular tail wags the radial dog}}, -volume = {501}, -year = {2021} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the TIGER principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper will report on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R. and Copin, Y. and Monnet, G. and Miller, Bryan W. and Allington-Smith, J. R. and Bureau, M. and Carollo, C. Marcella and Davies, Roger L. and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F. and Verolme, E. K. and {De Zeeuw}, P. Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bacon et al. - 2001 - The SAURON project - I. The panoramic integral-field spectrograph.pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Ludlow2016, -abstract = {We use a suite of cosmological simulations to study the mass-concentration-redshift relation, c(M, z), of dark matter haloes. Our simulations include standard $\Lambda$-cold dark matter (CDM) models, and additional runs with truncated power spectra, consistent with a thermal warm dark matter (WDM) scenario. We find that the mass profiles of CDM and WDM haloes are self-similar and well approximated by the Einasto profile. The c(M, z) relation of CDM haloes is monotonic: concentrations decrease with increasing virial mass at fixed redshift, and decrease with increasing redshift at fixed mass. The mass accretion histories (MAHs) of CDM haloes are also scale-free, and can be used to infer concentrations directly. These results do not apply to WDM haloes: their MAHs are not scale-free because of the characteristic scale imposed by the power spectrum suppression. Further, the WDM c(M, z) relation is non-monotonic: concentrations peak at a mass scale dictated by the truncation scale, and decrease at higher and lower masses. We show that the assembly history of a halo can still be used to infer its concentration, provided that the total mass of its progenitors is considered (the 'collapsed mass history'; CMH), rather than just that of its main ancestor. This exploits the scale-free nature of CMHs to derive a simple scaling that reproduces the mass-concentration-redshift relation of both CDM and WDM haloes over a vast range of halo masses and redshifts. Our model therefore provides a robust account of the mass, redshift, cosmology and power spectrum dependence of dark matter halo concentrations.}, -archivePrefix = {arXiv}, -arxivId = {1601.02624}, -author = {Ludlow, Aaron D. and Bose, Sownak and Angulo, Ra{\'{u}}l E. and Wang, Lan and Hellwing, Wojciech A. and Navarro, Julio F. and Cole, Shaun and Frenk, Carlos S.}, -doi = {10.1093/mnras/stw1046}, -eprint = {1601.02624}, -file = {:C\:/Users/Jammy/Documents/Papers/Simulation/Ludlow2016MCRDMHalos.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: haloes,Methods: numerical}, -number = {2}, -pages = {1214--1232}, -title = {{The mass-concentration-redshift relation of cold and warm dark matter haloes}}, -volume = {460}, -year = {2016} -} -@article{Libeskind2014, -abstract = {We examine the angular infall pattern of subhaloes on to host haloes in the context of the large-scale structure. We find that this infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are found to be preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that it is always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range (∼10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large-scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group. {\textcopyright}2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1407.0394}, -author = {Libeskind, Noam I and Knebe, Alexander and Hoffman, Yehuda and Gottl{\"{o}}ber, Stefan}, -doi = {10.1093/mnras/stu1216}, -eprint = {1407.0394}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Large-scale structure of universe}, -number = {2}, -pages = {1274--1280}, -title = {{The universal nature of subhalo accretion}}, -volume = {443}, -year = {2014} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR {\$}\backslasheta(z){\$} using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of {\$}102{\$} SGL with the measurement of corresponding velocity dispersion {\$}\backslashsigma{\_}0{\$} and Einstein radius {\$}\backslashtheta{\_}E{\$}. In addition, we also use a dataset of {\$}12{\$} two image lensing systems containing the measure of time delay {\$}\backslashDelta t{\$} between source images. Jointly these two datasets give us the angular diameter distance {\$}D{\_}{\{}A{\_}{\{}ol{\}}{\}}{\$} of the lens. Further, for luminosity distance, we use the {\$}740{\$} observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ({\$}\backslasheta=1{\$}) within {\$}2\backslashsigma{\$} confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R F L}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Rowlands2014, -abstract = {We present a comparison of the physical properties of a rest-frame 250-$\mu$m-selected sample of massive, dusty galaxies from 0 1 SMGs have an average star formation rate (SFR) of 390+80-70 M⊙ yr-1, which is 120 times that of the low-redshift sample matched in stellar mass to the SMGs (SFR=3.3±0.2M⊙ yr-1). The SMGsharbour a substantialmass of dust (1.2+0.3-0.2 ×109 M⊙), compared to (1.6 ± 0.1) ×108 M⊙ for low-redshift dusty galaxies. At low redshifts, the dust luminosity is dominated by the diffuse interstellar medium, whereas a large fraction of the dust luminosity in SMGs originates from star-forming regions. At the same dust mass, SMGs are offset towards a higher SFR compared to the low-redshift H-ATLAS galaxies. This is not only due to the higher gas fraction in SMGs but also because they are undergoing a more efficient mode of star formation, which is consistent with their bursty star formation histories. The offset in SFR between SMGs and low-redshift galaxies is similar to that found in CO studies, suggesting that dust mass is as good a tracer of molecular gas as CO. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.2994}, -author = {Rowlands, K. and Dunne, L. and Dye, S. and Arag{\'{o}}n-Salamanca, A. and Maddox, S. and Cunha, E. and Smith, D. J.B. and Bourne, N. and Eales, S. and Gomez, H. L. and Smail, I. and Alpaslan, M. and Clark, C. J.R. and Driver, S. and Ibar, E. and Ivison, R. J. and Robotham, A. and Smith, M. W.L. and Valiante, E.}, -doi = {10.1093/mnras/stu510}, -eprint = {1403.2994}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dust, extinction-galaxies,Evolution-galaxies,Fundamental parameters-galaxies,Galaxies,High-redshift-galaxies,ISM-submillimetre}, -number = {2}, -pages = {1017--1039}, -title = {{Herschel-ATLAS: Properties of dusty massive galaxies at low and high redshifts}}, -volume = {441}, -year = {2014} -} -@article{Dutton2007, -abstract = {We use observed rotation velocity-luminosity (VL) and size-luminosity (RL) relations to single out a specific scenario for disk galaxy formation in the $\Lambda$CDM cosmology. Our model involves four independent lognormal random variables: dark halo concentration c, disk spin $\lambda$gal, disk mass fraction mgal, and stellar mass-to-light ratio $\Upsilon$I. A simultaneous match of the VL and RL zero points with adiabatic contraction requires low-c halos, but this model has V2.2$\sim$1.8Vvir (where V2.2 and Vvir are the circular velocity at 2.2 disk scale lengths and the virial radius, respectively), which will be unable to match the luminosity function (LF). Similarly models without adiabatic contraction but standard c also predict high values of V2.2/Vvir. Models in which disk formation induces an expansion rather than the commonly assumed contraction of the dark matter halos have V2.2$\sim$1.2Vvir, which allows a simultaneous fit of the LF. This may result from nonspherical, clumpy gas accretion, where dynamical friction transfers energy from the gas to the dark matter. This model requires low $\lambda$gal and mgal values, contrary to naive expectations. However, the low $\lambda$gal is consistent with the notion that disk galaxies predominantly survive in halos with a quiet merger history, while a low mgal is also indicated by galaxy-galaxy lensing. The smaller than expected scatter in the RL relation and the lack of correlation between the residuals of the VL and RL relations, respectively, imply that the scatter in $\lambda$gal and in c needs to be smaller than predicted for $\Lambda$CDM halos, again consistent with the idea that disk galaxies preferentially reside in halos with a quiet merger history.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0604553}, -author = {Dutton, Aaron A. and van den Bosch, Frank C. and Dekel, Avishai and Courteau, Stephane}, -doi = {10.1086/509314}, -eprint = {0604553}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Formation,Galaxies: Fundamental Parameters,Galaxies: Spiral,Galaxies: Structure}, -month = {jan}, -number = {1}, -pages = {27--52}, -primaryClass = {astro-ph}, -title = {{A Revised Model for the Formation of Disk Galaxies: Low Spin and Dark Halo Expansion}}, -url = {http://adsabs.harvard.edu/abs/2007ApJ...654...27D}, -volume = {654}, -year = {2007} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos and predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of {\$}50{\$} keV {\$}\backslashlesssim m c{\^{}}2 \backslashlesssim 345{\$} keV, can be an alternative interpretation of the central compact object in Sgr A*. We present in this work the gravitational lensing properties of this novel DM model in Milky Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the Non-Singular Isothermal Sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, {\$}m c{\^{}}2\backslashapprox 10{\^{}}{\{}2{\}}{\$} keV, we draw the following conclusions. At distances {\$}r\backslashgtrsim 20{\$} pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. We show that at distances {\$}\backslashsim 10{\^{}}{\{}-4{\}}{\$} pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances {\$}r\backslashlesssim 10{\^{}}{\{}-6{\}}{\$} pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used. We find that quantum DM cores do not show a photon sphere what implies that they do not cast a shadow. Similar conclusions apply to the other DM distributions for other fermion masses in the above specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Tacconi2008, -abstract = {We report subarcsecond resolution IRAM PdBI millimeter CO interferometry of four z$\sim$2 submillimeter galaxies (SMGs), and sensitive CO(3-2) flux limits toward three z$\sim$2 UV/optically selected star-forming galaxies. The new data reveal for the first time spatially resolved CO gas kinematics in the observed SMGs. Two of the SMGs show double or multiple morphologies, with complex, disturbed gas motions. The other two SMGs exhibit CO velocity gradients of $\sim$500 km s-1 across <=0.2" (1.6 kpc) diameter regions, suggesting that the star-forming gas is in compact, rotating disks. Our data provide compelling evidence that these SMGs represent extreme, short-lived ``maximum'' star-forming events in highly dissipative mergers of gas-rich galaxies. The resulting high-mass surface and volume densities of SMGs are similar to those of compact quiescent galaxies in the same redshift range and much higher than those in local spheroids. From the ratio of the comoving volume densities of SMGs and quiescent galaxies in the same mass and redshift ranges, and from the comparison of gas exhaustion timescales and stellar ages, we estimate that the SMG phase duration is about 100 Myr. Our analysis of SMGs and optically/UV selected high-redshift star-forming galaxies supports a ``universal'' Chabrier IMF as being valid over the star-forming history of these galaxies. We find that the 12CO luminosity to total gas mass conversion factors at z$\sim$2-3 are probably similar to those assumed at z$\sim$0. The implied gas fractions in our sample galaxies range from 20% to 50%. Based on observations obtained at the IRAM Plateau de Bure Interferometer (PdBI). IRAM is funded by the Centre National de la Recherch{\'{e}} Scientifique (France), the Max-Planck Gesellschaft (Germany), and the Instituto Geografico Nacional (Spain).}, -archivePrefix = {arXiv}, -arxivId = {0801.3650}, -author = {Tacconi, L. J. and Genzel, R. and Smail, I. and Neri, R. and Chapman, S. C. and Ivison, R. J. and Blain, A. and Cox, P. and Omont, A. and Bertoldi, F. and Greve, T. and {F{\"{o}}rster Schreiber}, N. M. and Genel, S. and Lutz, D. and Swinbank, A. M. and Shapley, A. E. and Erb, D. K. and Cimatti, A. and Daddi, E. and Baker, A. J.}, -doi = {10.1086/587168}, -eprint = {0801.3650}, -isbn = {9781405169004}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {246--262}, -pmid = {17011326}, -title = {{ Submillimeter Galaxies at z ∼ 2: Evidence for Major Mergers and Constraints on Lifetimes, IMF, and CO‐H 2 Conversion Factor }}, -url = {http://stacks.iop.org/0004-637X/680/i=1/a=246}, -volume = {680}, -year = {2008} -} -@article{Aguero2016, -abstract = {We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75{\%} of the hosts), with a bar (44{\%} weak, 37{\%} strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem not to be important for the appearance of CNRs, which appear to be more related to intrinsic properties of the host galaxies or to minor merger processes; 2) the proportion of weak bars in galaxies with a CNR is higher than expected; 3) the incidence of Seyfert (Sy) activity coeval with CNRs is significantly larger than the rate expected from the morphological distribution of the host galaxies; 4) the rate of Sy 2 to Sy 1 type galaxies with CNRs is about three times larger than the expected ratio for galaxies without CNRs and is opposite to that predicted by the geometric paradigm of the classical unified model for AGNs, although it does support the hypothesis that Sy 2 activity is linked to circumnuclear star formation. The possible selection effects of the sample are discussed, and we conclude that the detected trends are strong enough to justify high quality observations of as large as possible set of galaxies with circumnuclear rings and their matched control samples.}, -author = {Ag{\"{u}}ero, Mar{\'{i}}a P and D{\'{i}}az, Rub{\'{e}}n J and Dottori, Horacio}, -doi = {10.4236/ijaa.2016.63018}, -issn = {2161-4717}, -journal = {International Journal of Astronomy and Astrophysics}, -keywords = {active,dynamics,galaxies,nuclei,spiral,structure}, -number = {03}, -pages = {219--235}, -title = {{Nuclear Activity in Circumnuclear Ring Galaxies}}, -url = {http://www.scirp.org/journal/doi.aspx?DOI=10.4236/ijaa.2016.63018}, -volume = {06}, -year = {2016} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of LCDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2004} -} -@article{Bruce2012, -abstract = { We have used high-resolution, HST WFC3/IR, near-infrared imaging to conduct a detailed bulge-disk decomposition of the morphologies of ≃ 200 of the most massive ( M * {\textgreater} 10 11 M ⊙ ) galaxies at 1 {\textless} z {\textless} 3 in the CANDELS-UDS field. We find that, while such massive galaxies at low redshift are generally bulge-dominated, at redshifts 1{\textless} z {\textless}2 they are predominantly mixed bulge+disk systems, and by z {\textgreater} 2 they are mostly disk-dominated. Interestingly, we find that while most of the quiescent galaxies are bulge-dominated, a significant fraction (25–40{\%}) of the most quiescent galaxies, have disk-dominated morphologies. Thus, our results suggest that the physical mechanisms which quench star-formation activity are not simply connected to those responsible for the morphological transformation of massive galaxies. }, -archivePrefix = {arXiv}, -arxivId = {1206.4322}, -author = {Bruce, V A and Dunlop, J S and Cirasuolo, M and McLure, R J and Targett, T A and Bell, E F and Croton, D J and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Kocevski, D D and Koekemoer, A M and Koo, D C and Lai, K and Lotz, J M and McGrath, E J and Newman, J A and {Van Der Wel}, A}, -doi = {10.1017/S1743921313004237}, -eprint = {1206.4322}, -isbn = {9781107033849}, -issn = {17439213}, -journal = {Proceedings of the International Astronomical Union}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: high-redshift,galaxies: structure}, -month = {dec}, -number = {S295}, -pages = {49--52}, -title = {{The morphologies of massive galaxies at 1{\textless}z{\textless}3 in the CANDELS-UDS field: Compact bulges, and the rise and fall of massive disks}}, -volume = {8}, -year = {2012} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Hopkins2006, -abstract = {We present an evolutionary model for starbursts, quasars, and spheroidal galaxies in which mergers between gas-rich galaxies drive nuclear inflows of gas, producing intense starbursts and feeding the buried growth of supermassive black holes (BHs) until feedback expels gas and renders a briefly visible optical quasar. The quasar lifetime and obscuring column density depend on both the instantaneous and peak luminosity of the quasar, and we determine this dependence using a large set of simulations of galaxy mergers varying host galaxy properties, orbital geometry, and gas physics. We use these fits to deconvolve observed quasar luminosity functions (LFs) and obtain the evolution of the formation rate of quasars with a certain peak luminosity, n(L{\_}peak,z). Quasars spend extended periods of time at luminosities well below peak, and so n(L{\_}peak) has a maximum corresponding to the 'break' in the observed LF, falling off at both brighter and fainter luminosities. From n(L{\_}peak) and our simulation results, we obtain self-consistent fits to hard and soft X-ray and optical quasar LFs and predict many observables, including: column density distributions of optical and X-ray samples, the LF of broad-line quasars in X-ray samples and the broad-line fraction as a function of luminosity, active BH mass functions, the distribution of Eddington ratios at z{\$\sim${}}0-2, the z=0 mass function of relic BHs and total mass density of BHs, and the cosmic X-ray background. In every case, our predictions agree well with observed estimates, and unlike previous modeling attempts, we are able to reproduce them without invoking any ad hoc assumptions about source properties or distributions. We provide a library of Monte Carlo realizations of our models for comparison with observations. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506398}, -author = {Hopkins, Philip F and Hernquist, Lars and Cox, Thomas J and {Di Matteo}, Tiziana and Robertson, Brant and Springel, Volker}, -doi = {10.1086/499298}, -eprint = {0506398}, -isbn = {doi:10.1086/499298}, -issn = {0067-0049}, -journal = {The Astrophysical Journal Supplement Series}, -number = {1}, -pages = {1--49}, -primaryClass = {astro-ph}, -title = {{A Unified, Merger‐driven Model of the Origin of Starbursts, Quasars, the Cosmic X‐Ray Background, Supermassive Black Holes, and Galaxy Spheroids}}, -url = {http://arxiv.org/abs/astro-ph/0506398%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/499298}, -volume = {163}, -year = {2006} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless} $\sigma$∗ {\textless} 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Greco2017, -abstract = {We present a catalog of extended low-surface-brightness galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first ${\sim}$200 deg$^2$ of the survey, we have uncovered 781 LSBGs, spanning red ($g-i\geq0.64$) and blue ($g-i<0.64$) colors and a wide range of morphologies. Since we focus on extended galaxies ($r_\mathrm{eff}=2.5$-$14^{\prime\prime}$), our sample is likely dominated by low-redshift objects. We define LSBGs to have mean surface brightnesses $\bar{\mu}_\mathrm{eff}(g)>24.3$ mag arcsec$^{-2}$, which allows nucleated galaxies into our sample. As a result, the central surface brightness distribution spans a wide range of $\mu_0(g)=18$-$27.4$ mag arcsec$^{-2}$, with 50% and 95% of galaxies fainter than 24.3 and 22 mag arcsec$^{-2}$, respectively. Furthermore, the surface brightness distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well-characterized by single-component S\'{e}rsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We crossmatch our sample with existing optical, HI, and ultraviolet catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, ranging from dwarf spheroidals and ultra-diffuse galaxies in nearby groups to gas-rich irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the LSBG population.}, -archivePrefix = {arXiv}, -arxivId = {1709.04474}, -author = {Greco, Johnny P. and Greene, Jenny E. and Strauss, Michael A. and Macarthur, Lauren A. and Flowers, Xzavier and Goulding, Andy D. and Huang, Song and Kim, Ji Hoon and Komiyama, Yutaka and Leauthaud, Alexie and Leisman, Lukas and Lupton, Robert H. and Sif{\'{o}}n, Crist{\'{o}}bal and Wang, Shiang-Yu}, -doi = {10.3847/1538-4357/aab842}, -eprint = {1709.04474}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greco et al. - 2018 - Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {dwarf,galaxies,general,keywords}, -number = {2}, -pages = {104}, -title = {{Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey}}, -url = {http://arxiv.org/abs/1709.04474%0Ahttp://dx.doi.org/10.3847/1538-4357/aab842}, -volume = {857}, -year = {2018} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently-discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially-interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorised according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}10{\^{}}11 Msun to {\textgreater}10{\^{}}13 Msun. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}10{\^{}}11 Msun. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW05). The two low-mass outliers are J0206-095 (SW19) and J2217+015 (SW42); if these two are indeed lenses, they probe an interesting regime of very low star-formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Keeton2003, -abstract = {Gravitational lensing provides a unique probe of the inner 10-1000 pc of distant galaxies (z=0.2-1). Lens theory predicts that every strong lens system should have a faint image near the center of the lens galaxy, which should be visible in radio lenses but have not been observed. We study these ``core'' images using models derived from the stellar distributions in nearby early-type galaxies. We find that realistic galaxies predict a remarkably wide range of core images, with lensing magnifications spanning some six orders of magnitude. More concentrated galaxies produce fainter core images, although not with any simple, quantitative, model independent relation. Some real galaxies have diffuse cores and predict bright core images (magnification mu>$\sim$0.1), but more common are galaxies that predict faint core images (mu<$\sim$0.001). Thus, stellar mass distributions alone are probably concentrated enough to explain the lack of observed core images, and may require observational sensitivity to improve by an order of magnitude before detections of core images become common. Two-image lenses will tend to have brighter core images than four-image lenses, so they will be the better targets for finding core images and exploiting these tools for studying the central mass distributions of distant galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0206243}, -author = {Keeton, Charles R.}, -doi = {10.1086/344539}, -eprint = {0206243}, -issn = {0004-637X}, -journal = {ApJ}, -number = {1}, -pages = {17--29}, -primaryClass = {astro-ph}, -title = {{Lensing and the Centers of Distant Early‐Type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/582/i=1/a=17}, -volume = {582}, -year = {2003} -} -@article{Suyu2012, -abstract = {The time delays between the multiple images of a strong lens system, together with a model of the lens mass distribution, allow a one-step measurement of a cosmological distance, namely, the 'time-delay distance' of the lens (D $\Delta$t) that encodes cosmological information. The time-delay distance depends sensitively on the radial profile slope of the lens mass distribution; consequently, the lens slope must be accurately constrained for cosmological studies. We show that the slope cannot be constrained in two-image systems with single-component compact sources, whereas it can be constrained in systems with two-component sources provided that the separation between the image components can be measured with milliarcsecond precisions, which is not feasible in most systems. In contrast, we demonstrate that spatially extended images of the source galaxy in two-image systems break the radial slope degeneracy and allow D $\Delta$t to be measured with uncertainties of a few per cent. Deep and high-resolution imaging of the lens systems are needed to reveal the extended arcs, and stable point spread functions are required for our lens modelling technique. Two-image systems, no longer plagued by the radial profile slope degeneracy, would augment the sample of useful time-delay lenses by a factor of ∼6, providing substantial advances for cosmological studies. {\textcopyright} 2012 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1202.0287}, -author = {Suyu, S. H.}, -doi = {10.1111/j.1365-2966.2012.21661.x}, -eprint = {1202.0287}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Distance scale,Gravitational lensing: strong,Methods: data analysis}, -month = {oct}, -number = {2}, -pages = {868--879}, -title = {{Cosmography from two-image lens systems: Overcoming the lens profile slope degeneracy}}, -volume = {426}, -year = {2012} -} -@article{Pontzen2017, -abstract = {We show how the interplay between active galactic nuclei (AGNs) and merger history determines whether a galaxy quenches star formation (SF) at high redshift. We first simulate, in a full cosmological context, a galaxy of total dynamical mass Mvir = 1012M⊙ at z = 2. Then we systematically alter the accretion history of the galaxy by minimally changing the linear overdensity in the initial conditions. This 'genetic modification' approach allows the generation of three sets of $\Lambda$ CDM initial conditions leading to maximum merger ratios of 1:10, 1:5 and 2:3, respectively. The changes leave the final halo mass, large-scale structure and local environment unchanged, providing a controlled numerical experiment. Interaction between the AGN physics and mergers in the three cases leads, respectively, to a star-forming, temporarily quenched and permanently quenched galaxy. However, the differences do not primarily lie in the black hole accretion rates, but in the kinetic effects of the merger: the galaxy is resilient against AGN feedback unless its gaseous disc is first disrupted. Typical accretion rates are comparable in the three cases, falling below 0.1M⊙ yr-1, equivalent to around 2 per cent of the Eddington rate or 10-3 times the pre-quenching star formation rate, in agreement with observations. This low level of black hole accretion can be sustained even when there is insufficient dense cold gas for SF. Conversely, supernova feedback is too distributed to generate outflows in high-mass systems, and cannot maintain quenching over periods longer than the halo gas cooling time.}, -archivePrefix = {arXiv}, -arxivId = {1607.02507}, -author = {Pontzen, Andrew and Tremmel, Michael and Roth, Nina and Peiris, Hiranya V. and Saintonge, Am{\'{e}}lie and Volonteri, Marta and Quinn, Tom and Governato, Fabio}, -doi = {10.1093/mnras/stw2627}, -eprint = {1607.02507}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pontzen et al. - 2017 - How to quench a galaxy.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: star formation,Galaxies: stellar content}, -number = {1}, -pages = {547--558}, -title = {{How to quench a galaxy}}, -volume = {465}, -year = {2017} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. with the particletagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of {\$\sim${}}1900 massive dark matter haloes (1012-1014M⊙) from the Millennium II $\lambda$ cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of MilkyWay-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a S{\`{e}}rsic profile, the radial scale and amplitude of which vary systematically with halo mass (M200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M* and M200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z ≈ 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S and White, Simon D M}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Enia2018, -abstract = {We perform lens modelling and source reconstruction of Sub-millimetre Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500$\mu$m in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). A previous analysis of the same data set used a single S{\'{e}}rsic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from theH-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission.We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5s. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value reff {\$\sim${}} 1.77 kpc and a median Gaussian full width at half-maximum {\$\sim${}}1.47 kpc. After correction for magnification, our sources have intrinsic star formation rates (SFR) {\$\sim${}} 900-3500M⊙ yr-1, resulting in a median SFR surface density $\Sigma$SFR {\$\sim${}} 132M⊙ yr-1 kpc-2 (or {\$\sim${}}218M⊙ yr-1 kpc-2 for the Gaussian fit). This is consistent with that observed for other star-forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst.}, -archivePrefix = {arXiv}, -arxivId = {1801.01831}, -author = {Enia, A and Negrello, M and Gurwell, M and Dye, S and Rodighiero, G and Massardi, M and {De Zotti}, G and Franceschini, A and Cooray, A and van der Werf, P and Birkinshaw, M and Michalowski, M J and Oteo, I}, -doi = {10.1093/mnras/sty021}, -eprint = {1801.01831}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong,Instrumentation: interferometers}, -number = {3}, -pages = {3467--3484}, -title = {{The Herschel-ATLAS: Magnifications and physical sizes of 500-$\mu$m-selected strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1801.01831}, -volume = {475}, -year = {2018} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M{\textgreater}10{\^{}}11 M{\_}sun) galaxies at 1.7{\textless}z{\textless}3 utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our sample is almost an order of magnitude larger than previous studies at these redshifts, providing the first statistical study of massive galaxy sizes at z{\textgreater}2, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n{\textless}2) and spheroid-like (n{\textgreater}2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z{\$\sim${}}2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z{\textgreater}2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ({\$\sim${}}2x10{\^{}}10 M{\_}sun kpc{\^{}}-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J and Bouwens, Rychard J and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -isbn = {1005-0302}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61----------------L64}, -title = {{Size evolution of the most massive galaxies at 1.7{\textless}z{\textless}3 from GOODS NICMOS survey imaging}}, -url = {http://arxiv.org/abs/0807.4141%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ($\sim$100 deg2) and deep (>28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of $\sim$7000 massive galaxies at z $\sim$ 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E. and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2018 - Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 z 0.5 using Hyper Suprime-Cam(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 < z < 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Zehavi2017, -abstract = {We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -- halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto- and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.}, -archivePrefix = {arXiv}, -arxivId = {1706.07871}, -author = {Zehavi, Idit and Contreras, Sergio and Padilla, Nelson and Smith, Nicholas J and Baugh, Carlton M and Norberg, Peder}, -doi = {10.3847/1538-4357/aaa54a}, -eprint = {1706.07871}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {clustering,cosmology,evolution,galaxies,halos,large-scale structure of universe,statistics,theory}, -number = {1}, -pages = {84}, -title = {{The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos}}, -url = {http://arxiv.org/abs/1706.07871%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaa54a}, -volume = {853}, -year = {2018} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the TIGER principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper will report on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R and Copin, Y and Monnet, G and Miller, Bryan W and Allington-Smith, J R and Bureau, M and Carollo, C Marcella and Davies, Roger L and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F and Verolme, E K and {De Zeeuw}, P Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs,cD}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{Oser2010, -abstract = {Cosmological simulations of galaxy formation appear to show a "two-phase" character with a rapid early phase at z≳2 duringwhich "in situ" stars are formedwithin the galaxy from infalling cold gas followed by an extended phase since z≲3 duringwhich "ex situ" stars are primarily accreted. In the latter phase, massive systems growconsiderably in mass and radius by accretion of smaller satellite stellar systems formed at quite early times (z > 3) outside of the virial radius of the forming central galaxy. These tentative conclusions are obtained from high-resolution resimulations of 39 individual galaxies in a full cosmological context with present-day virial halomasses ranging from 7×10 11M⊙ h -1 ≲ Mvir ≲ 2.7×1013M⊙ h -1 (h = 0.72) and central galaxy masses between 4.5×1010M⊙ h -1 ≲ M* ≲ 3.6 × 1011M⊙ h -1. The simulations include the effects of a uniform UV background, radiative cooling, star formation, and energetic feedback from Type II supernova. The importance of stellar accretion increases with galaxy mass and toward lower redshift. In our simulations, lower mass galaxies (M* ≲ 9 × 10 10M⊙ h -1) accrete about 60% of their present-day stellar mass. High-mass galaxy (M* ≳ 1.7 × 10 11M⊙ h -1) assembly is dominated by accretion and merging with about 80% of the stars added by the present day. In general the simulated galaxies approximately double their mass since z = 1. For massive systems this mass growth is not accompanied by significant star formation. The majority of the in situ created stars are formed at z > 2, primarily out of cold gas flows. We recover the observational result of "archaeological downsizing," where the most massive galaxies harbor the oldest stars. We find that this is not in contradiction with hierarchical structure formation. Most stars in the massive galaxies are formed early on in smaller structures; the galaxies themselves are assembled late. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1010.1381}, -author = {Oser, Ludwig and Ostriker, Jeremiah P. and Naab, Thorsten and Johansson, Peter H. and Burkert, Andreas}, -doi = {10.1088/0004-637X/725/2/2312}, -eprint = {1010.1381}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oser et al. - 2010 - The two phases of galaxy formation.pdf:pdf}, -isbn = {0315-162X (Print)\r0315-162X (Linking)}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Cosmology:theory,Dark matter,Galaxies:evolution,Galaxies:formation,Methods:numerical}, -number = {2}, -pages = {2312--2323}, -pmid = {24231395}, -title = {{The two phases of galaxy formation}}, -volume = {725}, -year = {2010} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1138?key=crossref.6ebb2a01dc7b45f1fa5c66089a37542b}, -volume = {709}, -year = {2010} -} -@article{Etherington2023, -author = {Etherington, Amy and Nightingale, James W and Massey, Richard and Robertson, Andrew and Cao, Xiaoyue and Amvrosiadis, Aristeidis and Cole, Shaun and Frenk, Carlos S and He, Qiuhan and Lagattuta, David J and Lange, Samuel and Li, Ran}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Etherington2023aBeyondBulge.pdf:pdf}, -journal = {MNRAS}, -keywords = {baryonic matter in the,cd,central few effective radii,distribution of dark plus,elliptical and lenticular,evolution,formation,galaxies,gravitational lensing,is roughly isothermal,observ ations have sho,of etgs is such,r,strong,that,their combined density profile,with,wn that the mean,$\gamma$,$\rho$}, -number = {4}, -pages = {6005--6018}, -title = {{Beyond the bulge – halo conspiracy ? Density profiles of early-type galaxies fr om extended-source strong lensing}}, -volume = {521}, -year = {2023} -} -@article{Yamamoto2019a, -author = {Yamamoto, Kimiyo N and Liu, Lin L and Nakamura, Akira and Haeno, Hiroshi and Michor, Franziska}, -doi = {10.1200/CCI.18.00079}, -issn = {2473-4276}, -journal = {JCO Clinical Cancer Informatics}, -month = {mar}, -number = {3}, -pages = {1--11}, -title = {{Supplementary Information Stochastic Evolution of Pancreatic Cancer Metastases During Logistic Clonal Expansion}}, -url = {http://ascopubs.org/doi/10.1200/CCI.18.00079}, -year = {2019} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of {\$\sim${}}3692 galaxies, with -18.5 {\textless}= M{\_}g {\textless} -22.0 mag and redshift 0.01 {\textless}= z {\textless} 0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of {\$\sim${}}2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined ({\textgreater}60 degrees) systems, we find the following results. (1) The optical r-band fraction (f{\_}opt-r) of barred galaxies is {\$\sim${}}48{\%}-52{\%}. (2) When galaxies are separated according to normalized half light radius (r{\_}e/R{\_}24), a remarkable result is seen: f{\_}opt-r rises sharply, from {\$\sim${}}40{\%} in galaxies that have small r{\_}e/R{\_}24 and visually appear to host prominent bulges, to {\$\sim${}}70{\%} for galaxies that have large r{\_}e/R{\_}24 and appear disk-dominated. (3) f{\_}opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that {\$\sim${}}20{\%} of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity {\textgreater}=0.4) and large enough (semi-major axis {\textgreater}=1.5 kpc) to be reliably characterized via ellipse-fitting out to z{\$\sim${}}0.8, we get an optical r-band fraction for strong bars f{\_}opt-s of {\$\sim${}}34{\%}. This value is higher only by a modest factor of 1.4, compared to the value of {\$\sim${}}24{\%}+-4{\%} reported at z{\$\sim${}}0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z{\$\sim${}}0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Johnson, Crockett}, -doi = {10.2307/3616804}, -eprint = {0802.3961}, -issn = {00255572}, -journal = {The Mathematical Gazette}, -keywords = {Astrophysics}, -number = {407}, -pages = {17}, -title = {{A Construction for a Regular Heptagon}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {59}, -year = {1975} -} -@article{Hoyos2011, -abstract = {We present a catalogue of structural parameters for 8814 galaxies in the 25 fields of the Hubble Space Telescope/ACS Coma Treasury Survey. Parameters from S{\'{e}}rsic fits to the two-dimensional surface brightness distributions are given for all galaxies from our published Coma photometric catalogue with mean effective surface brightness brighter than 26.0magarcsec-2 and brighter than 24.5mag (equivalent to absolute magnitude -10.5), as given by the fits, all in F814W(AB). The sample comprises a mixture of Coma members and background objects; 424 galaxies have redshifts and of these 163 are confirmed members. The fits were carried out using both the gim2dand galfit codes. We provide the following parameters: galaxy ID, RA, Dec., the total corrected automatic magnitude from the photometric catalogue, the total magnitude of the model (F814WAB), the geometric mean effective radius Re, the mean surface brightness within the effective radius 〈$\mu$〉e, the S{\'{e}}rsic index n, the ellipticity and the source position angle. The selection limits of the catalogue and the errors listed for the S{\'{e}}rsic parameters come from extensive simulations of the fitting process using synthetic galaxy models. The agreement between gim2d and galfit parameters is sensitive to details of the fitting procedure; for the settings employed here the agreement is excellent over the range of parameters covered in the catalogue. We define and present two goodness-of-fit indices which quantify the degree to which the image can be approximated by a S{\'{e}}rsic model with concentric, coaxial elliptical isophotes; such indices may be used to objectively select galaxies with more complex structures such as bulge-disc, bars or nuclear components. We make the catalogue available in electronic format at astro-wise and MAST. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1010.2352}, -author = {Hoyos, Carlos and {Den Brok}, Mark and Kleijn, Gijs Verdoes and Carter, David and Balcells, Marc and Guzm{\'{a}}n, Rafael and Peletier, Reynier and Ferguson, Henry C. and Goudfrooij, Paul and Graham, Alister W. and Hammer, Derek and Karick, Arna M. and Lucey, John R. and Matkovi{\'{c}}, Ana and Merritt, David and Mouhcine, Mustapha and Valentijn, Edwin}, -doi = {10.1111/j.1365-2966.2010.17855.x}, -eprint = {1010.2352}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: individual: Coma,Galaxies: dwarf,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: fundamental parameters}, -number = {4}, -pages = {2439--2460}, -title = {{The HST/ACS Coma Cluster Survey - III. Structural parameters of galaxies using single S{\'{e}}rsic fits}}, -url = {http://arxiv.org/abs/1010.2352v1%5Cnfile:///Users/boris/Documents/Papers/2010/Hoyos/arXiv 2010 Hoyos.pdf%5Cnpapers://82296e88-7781-4499-9ed0-1c7b65688f42/Paper/p766}, -volume = {411}, -year = {2011} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ($M_{*}>10^{10} M_{\odot}$), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at $z\sim2$. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that $39.2^{+3.9}_{-3.6}$\% (65/166) of cSFGs at $1.4=0.33^{+0.07}_{-0.09}$, in fair agreement with results from numerical simulations of CDM. This result provides strong support for the existence of dark matter, as an isotropic lensing signal is excluded with 99.5% confidence. We also study the average mass profile around the lenses, using a maximum likelihood analysis. We consider two models for the halo mass profile: a truncated isothermal sphere (TIS) and an NFW profile. We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo. The best fit NFW model yields a mass $M_{200}=(8.4\pm0.7\pm0.4)\times 10^{11} h^{-1} M_\odot$ and a scale radius $r_s=16.2^{+3.6}_{-2.9} h^{-1}$ kpc. This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, H. K. C. and Gladders, Michael D.}, -doi = {10.1086/382726}, -eprint = {0306515}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hoekstra, Yee, Gladders - 2004 - Properties of Galaxy Dark Matter Halos from Weak Lensing.pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of Galaxy Dark Matter Halos from Weak Lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2004} -} -@article{Napolitano2005, -abstract = {Owing to the fact that the near future should see a rapidly expanding set of probes of the halo masses of individual early-type galaxies, we introduce a convenient parameter for characterizing the halo masses from both observational and theoretical results: ∇ ℓ$\Upsilon$, the logarithmic radial gradient of the mass-to-light ratio. Using halo density profiles from $\Lambda$-cold dark matter (CDM) simulations, we derive predictions for this gradient for various galaxy luminosities and star formation efficiencies ∈ SF. As a pilot study, we assemble the available ∇ ℓ$\Upsilon$ data from kinematics in early-type galaxies - representing the first unbiased study of halo masses in a wide range of early-type galaxy luminosities - and find a correlation between luminosity and ∇ ℓ$\Upsilon$, such that the brightest galaxies appear the most dark-matter dominated. We find that the gradients in most of the brightest galaxies may fit in well with the $\Lambda$CDM predictions, but that there is also a population of fainter galaxies whose gradients are so low as to imply an unreasonably high star formation efficiency ∈ SF > 1. This difficulty is eased if dark haloes are not assumed to have the standard $\Lambda$CDM profiles, but lower central concentrations.}, -author = {Napolitano, N. R. and Capaccioli, M. and Romanowsky, A. J. and Douglas, N. G. and Merrifield, M. R. and Kuijken, K. and Arnaboldi, M. and Gerhard, O. and Freeman, K. C.}, -doi = {10.1111/j.1365-2966.2005.08683.x}, -file = {:C\:/Users/Jammy/Documents/Papers/Ellipticals/Napolitano2005ETGMLRRatioGradients.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {2}, -pages = {691--706}, -title = {{Mass-to-light ratio gradients in early-type galaxy haloes}}, -volume = {357}, -year = {2005} -} -@article{Greve2005, -abstract = {In this paper, we present results from an Institut de Radio Astronomie Millim{\'{e}}trique (IRAM) Plateau de Bure millimetre-wave Interferometer (PdBI) survey for carbon monoxide (CO) emission towards radio-detected submillimetre galaxies (SMGs) with known optical and near-infrared spectroscopic redshifts. Five sources in the redshift range z ∼ 1-3.5 were detected, nearly doubling the number of SMGs detected in CO. We summarize the properties of all 12 CO-detected SMGs, as well as six sources not detected in CO by our survey, and use this sample to explore the bulk physical properties of the submillimetre galaxy (SMG) population as a whole. The median CO line luminosity of the SMGs is 〈L′ CO) = (3.8 ±2.0) × 10 10K km s -1pc 2. Using a CO-to-H 2 conversion factor appropriate for starburst galaxies, this corresponds to a molecular gas mass 〈M(H 2)〉 = (3.0 ± 1.6) × 10 10 M ⊙ within an ∼ 2 kpc radius, approximately 4 times greater than the most luminous local ultraluminous infrared galaxies (ULIRGs) but comparable to that of the most extreme high-redshift radio galaxies (HzRGs) and quasi-sellar objects (QSOs). The median CO FWHM linewidth is broad, (FWHM) = 780 ± 320 km s -1, and the SMGs often have double-peaked line profiles, indicative of either a merger or a disc. From their median gas reservoirs (∼ 3 × 10 10 M ⊙) and star formation rates (≳ 700 M ⊙ yr -1), we estimate a lower limit on the typical gas-depletion time-scale of ≳ 40 Myr in SMGs. This is marginally below the typical age expected for the starbursts in SMGs and suggests that negative feedback processes may play an important role in prolonging the gas consumption time-scale, We find a statistically significant correlation between the far-infrared and CO luminosities of the SMGs, which extends the observed correlation for local ULIRGs to higher luminosities and higher redshifts. The non-linear nature of the correlation implies that SMGs have higher far-infrared to CO luminosity ratios and possibly higher star formation efficiencies (SFEs), than local ULIRGs. Assuming a typical CO source diameter of $\theta$ ∼ 0.5 arcsec (D ∼ 4 kpc), we estimate a median dynamical mass of 〈M dyn〉 ≃ (1.2 ± 1.5) × 10 11 M ⊙ for the SMG sample. Both the total gas and stellar masses imply that SMGs are very massive systems, dominated by baryons in their central regions. The baryonic and dynamical properties of these systems mirror those of local giant ellipticals and are consistent with numerical simulations of the formation of the most massive galaxies. We have been able to impose a lower limit of ≳ 5 × 10 -6 Mpc -3 to the comoving number density of massive galaxies in the redshift range z ∼ 2-3.5, which is in agreement with results from recent spectroscopic surveys and the most recent model predictions. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503055}, -author = {Greve, T. R. and Bertoldi, F. and Smail, Ian and Neri, R. and Chapman, S. C. and Blain, A. W. and Ivison, R. J. and Genzel, R. and Omont, A. and Cox, P. and Tacconi, L. and Kneib, J. P.}, -doi = {10.1111/j.1365-2966.2005.08979.x}, -eprint = {0503055}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Early Universe,Galaxies: formation,Galaxies: starburst}, -number = {3}, -pages = {1165--1183}, -primaryClass = {astro-ph}, -title = {{An interferometric CO survey of luminous submillimetre galaxies}}, -volume = {359}, -year = {2005} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of stellar parameters and abundances ("stellar labels") for hundreds of thousands of stars; this poses a formidable spectral modeling challenge. In many cases, there is a subset of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the "known" labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with and as the labels, and then applying it to the spectra of 55,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one-ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ness, M. and Hogg, David W. and Rix, H. W. and Ho, Anna Y.Q. and Zasowski, G.}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ness et al. - 2015 - THE CANNON A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{THE CANNON: A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION}}, -volume = {808}, -year = {2015} -} -@article{Mendez-Abreu2010, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims: We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods: We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results: We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A+B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater} 50{\%} and none has a probability {\textgreater} 90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions: According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {0004-6361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -pages = {A71}, -title = {{Structural properties of disk galaxies}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Hall2014, -abstract = {? 2013 IEEE.The science goals of missions from the Hubble Space Telescope through to Gaia and Euclid require ultra-precise positional information. However, in the radiation environment of the space telescopes, damage to the CCD focal plane detectors through high energy protons leads to the creation of traps, a loss of charge transfer efficiency and a consequent deterioration in the positional accuracy. An understanding of the traps produced and their properties in the CCD during operation is essential to allow optimisation of the devices and suitable modelling to correct the effect of the damage through the post-processing of images. The technique of 'pumping' single traps has allowed the study of individual traps to a new level of detail and accuracy that cannot be achieved with other techniques, such as Deep Level Transient Spectroscopy, whilst also locating each trap to the sub-pixel level in the device. Outlining the principles used, we have demonstrated the technique for the A-centre, the most influential trap in serial read-out, giving results consistent with the more general theoretical values, but here showing new results indicating the spread in the emission times achieved and the variation in capture probability of individual traps with increasing signal levels. This technique can now be applied to other time and temperature regimes in the CCD to characterise individual traps, localised to sub-pixel accuracy, such that dramatic improvements can be made to optimisation processes and modelling techniques.}, -author = {Hall, David J and Murray, Neil J and Holland, Andrew D and Gow, Jason and Clarke, Andrew and Burt, David}, -doi = {10.1109/TNS.2013.2295941}, -isbn = {9781467350570}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {A-centre,CCD image sensors,Euclid,Si-A,defect,pocket pumping,radiation damage,trap pumping}, -number = {4}, -pages = {1826--1833}, -title = {{Determination of in situ trap properties in CCDs using a "single-trap pumping" technique}}, -volume = {61}, -year = {2014} -} -@article{Zehavi2017, -abstract = {We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -- halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto- and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.}, -archivePrefix = {arXiv}, -arxivId = {1706.07871}, -author = {Zehavi, Idit and Contreras, Sergio and Padilla, Nelson and Smith, Nicholas J and Baugh, Carlton M and Norberg, Peder}, -doi = {10.3847/1538-4357/aaa54a}, -eprint = {1706.07871}, -issn = {1538-4357}, -keywords = {clustering,cosmology,evolution,galaxies,halos,large-scale structure of universe,statistics,theory}, -title = {{The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos}}, -url = {http://arxiv.org/abs/1706.07871%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaa54a}, -year = {2017} -} -@article{Enia2018, -abstract = {We perform lens modelling and source reconstruction of Submillimeter Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500{\$}\backslashbackslashmu{\{}\backslash{\$}{\}}m in the Herschel Astrophysical Terahertz Large Area Survey H-ATLAS. A previous analysis of the same dataset used a single S{\$}\backslash{\$}`ersic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from the H-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission. We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5{\$}\backslashbackslashsigma{\{}\backslash{\$}{\}}. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value {\$}r{\_}{\{}eff{\}}\backslash,\backslashbackslashsim 1.77\backslash,{\$}kpc and a median Gaussian full width at half maximum {\$}\backslashbackslashsim1.47\backslash,{\$}kpc. After correction for magnification, our sources have intrinsic star formation rates SFR{\$}\backslash,\backslashbackslashsim900-3500\backslash,M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}yr{\^{}}{\{}-1{\}}{\$}, resulting in a median star formation rate surface density {\$}\backslashbackslashSigma{\{}\backslash{\_}{\}}{\{}SFR{\}}\backslashbackslashsim132\backslash,M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} yr{\$}{\^{}}{\{}-1{\}}{\$} kpc{\$}{\^{}}{\{}-2{\}}{\$} (or {\$}\backslashbackslashsim 218\backslash,M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} yr{\$}{\^{}}{\{}-1{\}}{\$} kpc{\$}{\^{}}{\{}-2{\}}{\$} for the Gaussian fit). This is consistent with what observed for other star forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst.}, -archivePrefix = {arXiv}, -arxivId = {1801.01831}, -author = {Enia, A and Negrello, M and Gurwell, M and Dye, S and Rodighiero, G and Massardi, M and {De Zotti}, G and Franceschini, A and Cooray, A and van der Werf, P and Birkinshaw, M and Michalowski, M J and Oteo, I}, -doi = {10.1093/mnras/sty021}, -eprint = {1801.01831}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong,Instrumentation: interferometers}, -number = {3}, -pages = {3467--3484}, -title = {{The Herschel-ATLAS: Magnifications and physical sizes of 500-{\$}\mu{\$}m-selected strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1801.01831}, -volume = {475}, -year = {2018} -} -@article{Savorgnan2015, -abstract = {The S$\backslash$'ersic {\$}R{\^{}}{\{}1/n{\}}{\$} model is the best approximation known to date for describing the light distribution of stellar spheroidal and disk components, with the S$\backslash$'ersic index {\$}n{\$} providing a direct measure of the central radial concentration of stars. The S$\backslash$'ersic index of a galaxy's spheroidal component, {\$}n{\_}{\{}sph{\}}{\$}, has been shown to tightly correlate with the mass of the central supermassive black hole, {\$}M{\_}{\{}BH{\}}{\$}. The {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} correlation is also expected from other two well known scaling relations involving the spheroid luminosity, {\$}L{\_}{\{}sph{\}}{\$}: the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and the {\$}M{\_}{\{}BH{\}}-L{\_}{\{}sph{\}}{\$}. Obtaining an accurate estimate of the spheroid S$\backslash$'ersic index requires a careful modelling of a galaxy's light distribution and some studies have failed to recover a statistically significant {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} correlation. With the aim of re-investigating the {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} and other black hole mass scaling relations, we performed a detailed (i.e.{\$\sim${}}bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, that had been imaged at {\$}3.6\backslashrm{\\sim{}}\backslashmu m{\$} with Spitzer. In this paper, the third of this series, we present an analysis of the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} diagrams. While early-type (elliptical+lenticular) and late-type (spiral) galaxies split into two separate relations in the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}-L{\_}{\{}sph{\}}{\$} diagrams, they reunite into a single {\$}M{\_}{\{}BH{\}} \backslashpropto n{\_}{\{}sph{\}}{\^{}}{\{}3.39 \backslashpm 0.15{\}}{\$} sequence with relatively small intrinsic scatter ({\$}\backslashepsilon \backslashsimeq 0.25 \backslashrm{\\sim{}}dex{\$}). The black hole mass appears to be closely related to the spheroid central concentration of stars, which mirrors the inner gradient of the spheroid gravitational potential.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1603.01910}, -author = {Savorgnan, Giulia A D}, -doi = {10.3847/0004-637x/821/2/88}, -eprint = {1603.01910}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {88}, -title = {{ SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE M BH – n sph CORRELATION }}, -url = {http://arxiv.org/abs/1603.01910%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/821/2/88}, -volume = {821}, -year = {2016} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) 'CMASS' sample at z {\$\sim${}} 0.5. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogues which include selection effects, reproduce the overall SMF, the projected two-point correlation function wp, the CMASS dn/dz, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of 'age matching' and show that these effects are markedly different compared to the ones explored by Hearin et al. at lower stellar masses. We construct two models, one in which galaxy colour is stochastic ('AbM' model) as well as a model which contains assembly bias effects ('AgM' model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colours are not a stochastic process in high-mass haloes. Our results suggest that the colours of galaxies in high-mass haloes are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P and Bundy, Kevin and Zentner, Andrew R and Behroozi, Peter S and Reid, Beth A and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L and White, Martin and Schneider, Donald P}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P{\_}KS $\backslash$simeq 1.5 $\backslash$times 10{\^{}}{\{}-4{\}}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability $\backslash$simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R and Kravtsov, Andrey V and Gnedin, Oleg Y and Klypin, Anatoly A}, -doi = {10.1086/431355}, -eprint = {0502496}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Naab2007, -abstract = {We describe high-resolution smoothed particle hydrodynamics (SPH) simulations of three approximately M* field galaxies starting from $\Lambda$CDM initial conditions. The simulations are made intentionally simple, and include photoionization, cooling of the intergalactic medium, and star formation, but not feedback from AGNs or supernovae. All of the galaxies undergo an initial burst of star formation at z{\$\sim${}}5, accompanied by the formation of a bubble of heated gas. Two out of three galaxies show early-type properties at present, whereas only one of them experienced a major merger. Heating from shocks and PdV work dominates over cooling so that for most of the gas the temperature is an increasing function of time. By z{\$\sim${}}1 a significant fraction of the final stellar system is in place and the spectral energy distribution resembles those of observed massive red galaxies. The galaxies have grown from z=1--{\textgreater}0 on average by 25{\%} in mass and in size by gas-poor (dry) stellar mergers. By the present day the simulated galaxies are old ({\$\sim${}}10 Gyr), kinematically hot stellar systems surrounded by hot gaseous haloes. Stars dominate the mass of the galaxies up to {\$\sim${}}4 effective radii ({\$\sim${}}10 kpc). Kinematic and most photometric properties are in good agreement with those of observed elliptical galaxies. The galaxy with a major merger develops a counter-rotating core. Our simulations show that realistic intermediate-mass giant elliptical galaxies with plausible formation histories can be formed from $\Lambda$CDM initial conditions even without requiring recent major mergers or feedback from supernovae or AGNs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0512235}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P and Efstathiou, George}, -doi = {10.1086/510841}, -eprint = {0512235}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {710--720}, -primaryClass = {astro-ph}, -title = {{Formation of Early‐Type Galaxies from Cosmological Initial Conditions}}, -url = {http://stacks.iop.org/0004-637X/658/i=2/a=710}, -volume = {658}, -year = {2007} -} -@article{Mendez-Abreu2010, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A < 0.9). This fraction is 33%, 55%, and 43% if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C < (A + B)/2). Only 18% of the observed bulges have a probability >50% and none has a probability >90% of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n > 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T > 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n > 2 and B/T > 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n > 2 and with B/T > 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n > 2 and B/T > 0.3. {\textcopyright} 2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J. and Simonneau, E. and Aguerri, J. A.L. and Corsini, E. M.}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/M{\'{e}}ndez-Abreu et al. - 2010 - Structural properties of disk galaxies II. Intrinsic shape of bulges(3).pdf:pdf}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {galaxies: bulges,galaxies: elliptical and lenticular, cD,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S{\`{e}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as Mh(M*) ∝ reff$\eta$ (M*). We find that, on average, our lens galaxies have an $\eta$ = 0.42 ± 0.12, i.e. larger galaxies live in more massive dark matter haloes. The $\eta$ is strongest for high-mass luminous red galaxies. Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed M*, satellite galaxies have a larger $\eta$ and greater scatter in the Mh and reff relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J.L. and Hudson, Michael J. and Balogh, Michael L. and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Charlton et al. - 2017 - The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Jimenez-Vicente2019, -abstract = {We present a new approach in the study of the Initial Mass function (IMF) in external galaxies based on quasar microlensing observations. We use measurements of quasar microlensing magnifications in 24 lensed quasars to estimate the average mass of the stellar population in the lens galaxies without any a priori assumption on the shape of the IMF. The estimated mean mass of the stars is $\langle M \rangle =0.16^{+0.05}_{-0.08} M_\odot$ (at 68\% confidence level). We use this average mass to put constraints into two important parameters characterizing the IMF of lens galaxies: the low-mass slope, $\alpha_2$, and the low-mass cutoff, $M_{low}$. Combining these constraints with prior information based on lensing, stellar dynamics, and absorption spectral feature analysis, we calculate the posterior probability distribution for the parameters $M_{low}$ and $\alpha_2$. We estimate values for the low-mass end slope of the IMF $\langle \alpha_2\rangle=-2.6\pm 0.9$ (heavier than that of the Milky Way) and for the low-mass cutoff $\langle M_{low}\rangle=0.13\pm0.07$. These results are in good agreement with previous studies on these parameters and remain stable against the choice of different suitable priors.}, -archivePrefix = {arXiv}, -arxivId = {1910.10509}, -author = {Jim{\'{e}}nez-Vicente, J. and Mediavilla, E.}, -doi = {10.3847/1538-4357/ab46b8}, -eprint = {1910.10509}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Jim{\'{e}}nez-Vicente, Mediavilla - 2019 - The Initial Mass Function of Lens Galaxies from Quasar Microlensing.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {75}, -title = {{The Initial Mass Function of Lens Galaxies from Quasar Microlensing}}, -url = {http://arxiv.org/abs/1910.10509%0Ahttp://dx.doi.org/10.3847/1538-4357/ab46b8}, -volume = {885}, -year = {2019} -} -@article{Shao2016, -abstract = {The spatial distribution of the satellite populations of the Milky Way and Andromeda are puzzling in that they are nearly perpendicular to the discs of their central galaxies. To understand the origin of such configurations we study the alignment of the central galaxy, satellite system and dark matter halo in the largest of the 'Evolution and Assembly of GaLaxies and their Environments' (eagle) simulation. We find that centrals and their satellite systems tend to be well aligned with their haloes, with a median misalignment angle of 33° in both cases. While the centrals are better aligned with the inner 10 kpc halo, the satellite systems are better aligned with the entire halo indicating that satellites preferentially trace the outer halo. The central-satellite alignment is weak (median misalignment angle of 52°) and we find that around 20 per cent of systems have a misalignment angle larger than 78°, which is the value for the Milky Way. The central-satellite alignment is a consequence of the tendency of both components to align with the dark matter halo. As a consequence, when the central is parallel to the satellite system, it also tends to be parallel to the halo. In contrast, if the central is perpendicular to the satellite system, as in the case of the Milky Way and Andromeda, then the central-halo alignment is much weaker. Dispersion-dominated (spheroidal) centrals have a stronger alignment with both their halo and their satellites than rotation-dominated (disc) centrals. We also found that the halo, the central galaxy and the satellite system tend to be aligned with the surrounding large-scale distribution of matter, with the halo being the better aligned of the three.}, -archivePrefix = {arXiv}, -arxivId = {1605.01728}, -author = {Shao, Shi and Cautun, Marius and Frenk, Carlos S and Gao, Liang and Crain, Robert A and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw1247}, -eprint = {1605.01728}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3772--3783}, -title = {{Alignments between galaxies, satellite systems and haloes}}, -volume = {460}, -year = {2016} -} -@article{Herbert-Fort2007, -abstract = {We measure the distribution of velocities for prograde and retrograde satellite galaxies using a combination of published data and new observations for 78 satellites of 63 extremely isolated disc galaxies (169 satellites total). We find that the velocity distribution is non-Gaussian ({\textgreater}99.9 per cent confidence), but that it can be described as the sum of two Gaussians, one of which is broad ($\sigma$ = 176 ± 15 km s-1), has a mean prograde velocity of 86 ± 30 km s-1, and contains ∼55 per cent of the satellites, while the other is slightly retrograde with a mean velocity of -21 ± 22 km s-1 and $\sigma$ = 74 ± 18 km s-1 and contains ∼45 per cent of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy, and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Riechers2011, -abstract = {We report the detection of spatially resolved CO(J = 1→0) emission in the z 3.4 submillimeter galaxies (SMGs) SMMJ09431+4700 and SMMJ13120+4242, using the Expanded Very Large Array (EVLA). SMMJ09431+4700 is resolved into the two previously reported millimeter sources H6 and H7, separated by 30kpc in projection. We derive CO(J = 1→0) line luminosities of L′ CO(1-0) = (2.49 0.86) and (5.82 1.22) × 10 10Kkms-1pc2 for H6 and H7, and L′CO(1-0) = (23.4 4.1) × 1010Kkms -1pc2 for SMMJ13120+4242. These are 1.5-4.5 times higher than what is expected from simple excitation modeling of higher-J CO lines, suggesting the presence of copious amounts of low-excitation gas. This is supported by the finding that the CO(J = 1→0) line in SMMJ13120+4242, the system with the lowest CO excitation, appears to have a broader profile and more extended spatial structure than seen in higher-J CO lines (which is less prominently seen in SMMJ09431+4700). Based on L′CO(1-0) and excitation modeling, we find M gas = 2.0-4.3 and 4.7-12. 7×1010 M⊙ for H6 and H7, and M gas = 18.7-69.4×1010 M⊙ for SMMJ13120+4242. The observed CO(J = 1→0) properties are consistent with the picture that SMMJ09431+4700 represents an early-stage, gas-rich major merger and that SMMJ13120+4242 represents such a system in an advanced stage. This study thus highlights the importance of spatially and dynamically resolved CO(J = 1→0) observations of SMGs to further understand the gas physics that drive star formation in these distant galaxies, which is possible only now that the EVLA is rising to its full capabilities. {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1105.4177}, -author = {Riechers, Dominik A. and Hodge, Jacqueline and Walter, Fabian and Carilli, Christopher L. and Bertoldi, Frank}, -doi = {10.1088/2041-8205/739/1/L31}, -eprint = {1105.4177}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: active,galaxies: formation,galaxies: high-redshift,galaxies: starburst,radio lines: galaxies}, -number = {1}, -pages = {L31}, -title = {{Extended cold molecular gas reservoirs in z ≃ 3.4 submillimeter galaxies}}, -url = {http://adsabs.harvard.edu/abs/2011ApJ...739L..31R}, -volume = {739}, -year = {2011} -} -@article{Massey2018, -abstract = {We present integral field spectroscopy of galaxy cluster Abell 3827, using Atacama Large Millimetre Array (ALMA) and Very Large Telescope/Multi-Unit Spectroscopic Explorer. It reveals an unusual configuration of strong gravitational lensing in the cluster core, with at least seven lensed images of a single background spiral galaxy. Lens modelling based on Hubble Space Telescope imaging had suggested that the dark matter associated with one of the cluster's central galaxies may be offset. The new spectroscopic data enable better subtraction of foreground light, and better identification of multiple background images. The inferred distribution of dark matter is consistent with being centred on the galaxies, as expected by $\Lambda$ cold dark matter. Each galaxy's dark matter also appears to be symmetric. Whilst, we do not find an offset between mass and light (suggestive of self-interacting dark matter) as previously reported, the numerical simulations that have been performed to calibrate Abell 3827 indicate that offsets and asymmetry are still worth looking for in collisions with particular geometries. Meanwhile, ALMA proves exceptionally useful for strong lens image identifications.}, -archivePrefix = {arXiv}, -arxivId = {1708.04245}, -author = {Massey, Richard and Harvey, David and Liesenborgs, Jori and Richard, Johan and Stach, Stuart and Swinbank, Mark and Taylor, Peter and Williams, Liliya and Clowe, Douglas and Courbin, Fr{\'{e}}d{\'{e}}ric and Edge, Alastair and Israel, Holger and Jauzac, Mathilde and Joseph, R{\'{e}}my and Jullo, Eric and Kitching, Thomas D. and Leonard, Adrienne and Merten, Julian and Nagai, Daisuke and Nightingale, James and Robertson, Andrew and Romualdez, Luis Javier and Saha, Prasenjit and Smit, Renske and Tam, Sut Ieng and Tittley, Eric}, -doi = {10.1093/mnras/sty630}, -eprint = {1708.04245}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astroparticle physics,Dark matter,Galaxies: Clusters: Individual: Abell 3827,Gravitational lensing: Strong}, -number = {1}, -pages = {669--677}, -title = {{Dark matter dynamics in Abell 3827: New data consistent with standard cold dark matter}}, -volume = {477}, -year = {2018} -} -@article{Hogg2022, -abstract = {Line-of-sight effects in strong gravitational lensing have long been treated as a nuisance. However, it was recently proposed that the line-of-sight shear could be a cosmological observable in its own right, if it is not degenerate with lens model parameters. We first demonstrate that the line-of-sight shear can be accurately measured from a simple simulated strong lensing image with per cent precision. We then extend our analysis to more complex simulated images and stress test the recovery of the line-of-sight shear when using deficient fitting models, finding that it escapes from degeneracies with lens model parameters, albeit at the expense of the precision. Lastly, we check the validity of the tidal approximation by simulating and fitting an image generated in the presence of many line-of-sight dark matter haloes, finding that an explicit violation of the tidal approximation does not necessarily prevent one from measuring the line-of-sight shear.}, -archivePrefix = {arXiv}, -arxivId = {2210.07210}, -author = {Hogg, Natalie B. and Fleury, Pierre and Larena, Julien and Martinelli, Matteo}, -doi = {10.1093/mnras/stad512}, -eprint = {2210.07210}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Hogg2022SLShear.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cosmology: theory,gravitational lensing: strong,software: development}, -number = {4}, -pages = {5982--6000}, -title = {{Measuring line-of-sight shear with Einstein rings: a proof of concept}}, -url = {http://arxiv.org/abs/2210.07210}, -volume = {520}, -year = {2023} -} -@article{Milosavljevic2001, -abstract = {We investigate a model in which galactic nuclei form via the coalescence of pre-existing stellar systems containing supermassive black holes. Merger simulations are carried out using N-body algorithms that can follow the formation and decay of a black-hole binary and its effect on the surrounding stars down to sub-parsec scales. Our initial stellar systems have steep central density cusps similar to those in low-luminosity elliptical galaxies. Formation of a black-hole binary transfers energy to the stars and lowers the central density; continued decay of the binary creates a {\$\sim${}}1/r density cusp similar to those observed in bright elliptical galaxies, with a break radius that extends well beyond the sphere of gravitational influence of the black holes. The decay of the black hole binary is followed over a factor of {\$\sim${}}20 in separation after formation of a hard binary, considerably farther than in previous simulations. We see almost no dependence of the binary's decay rate on number of particles in the simulation, contrary to earlier studies in which a lower initial density of stars led to a more rapid depletion of the binary's loss cone. We nevertheless argue that the decay of a black hole binary in a real galaxy would be expected to stall at separations of 0.01-1 pc unless some additional mechanism is able to extract energy from the binary. Our results support a picture in which the observed dependence of nuclear cusp slope on galaxy luminosity is a consequence of galaxy interactions. We also discuss the implications of our results for the survivability of dark-matter cusps.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103350}, -author = {Milosavljevic, Milos and Merritt, David}, -doi = {10.1086/323830}, -eprint = {0103350}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {34--62}, -primaryClass = {astro-ph}, -title = {{Formation of Galactic Nuclei}}, -url = {http://arxiv.org/abs/astro-ph/0103350%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/323830}, -volume = {563}, -year = {2001} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high resolution N-body simulations of galactic dark matter halos to test if this remarkable property can be understood within the context of the cold dark matter cosmology. We construct halo merger trees from the simulations and use a semianalytic model to follow the formation of satellite galaxies. We find that in all 6 of our simulations, the 11 brightest satellites are indeed distributed along thin, disk-like structures analogous to that traced by the Milky Way's satellites. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhalos within it which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhalos but is similar to that of the subset of subhalos that had the most massive progenitors at earlier times. The elongated disk-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I and Frenk, Carlos S and Cole, Shaun and Helly, John C and Jenkins, Adrian and Navarro, Julio F and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Aguero2016, -abstract = {We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75{\%} of the hosts), with a bar (44{\%} weak, 37{\%} strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem not to be important for the appearance of CNRs, which appear to be more related to intrinsic properties of the host galaxies or to minor merger processes; 2) the proportion of weak bars in galaxies with a CNR is higher than expected; 3) the incidence of Seyfert (Sy) activity coeval with CNRs is significantly larger than the rate expected from the morphological distribution of the host galaxies; 4) the rate of Sy 2 to Sy 1 type galaxies with CNRs is about three times larger than the expected ratio for galaxies without CNRs and is opposite to that predicted by the geometric paradigm of the classical unified model for AGNs, although it does support the hypothesis that Sy 2 activity is linked to circumnuclear star formation. The possible selection effects of the sample are discussed, and we conclude that the detected trends are strong enough to justify high quality observations of as large as possible set of galaxies with circumnuclear rings and their matched control samples.}, -author = {Ag{\"{u}}ero, Mar{\'{i}}a P and D{\'{i}}az, Rub{\'{e}}n J and Dottori, Horacio}, -doi = {10.4236/ijaa.2016.63018}, -issn = {2161-4717}, -journal = {International Journal of Astronomy and Astrophysics}, -keywords = {active,dynamics,galaxies,nuclei,spiral,structure}, -number = {03}, -pages = {219--235}, -title = {{Nuclear Activity in Circumnuclear Ring Galaxies}}, -url = {http://www.scirp.org/journal/doi.aspx?DOI=10.4236/ijaa.2016.63018}, -volume = {06}, -year = {2016} -} -@article{Metcalf2018, -abstract = {Large-scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images, and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects, reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100 000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. Having multi-band, ground based data is found to be better for this purpose than single-band space based data with lower noise and higher resolution, suggesting that multi-colour data is crucial. Multi-band space based data will be superior to ground based data. The most difficult challenge for a lens finder is differentiating between rare, irregular and ring-like face-on galaxies and true gravitational lenses. The degree to which the efficiency and biases of lens finders can be quantified largely depends on the realism of the simulated data on which the finders are trained.}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R. B. and Meneghetti, M. and Avestruz, C. and Bellagamba, F. and Bom, C. R. and Bertin, E. and Cabanac, R. and Courbin, F. and Davies, A. and Decenci{\`{e}}re, E. and Flamary, R. and Gavazzi, R. and Geiger, M. and Hartley, P. and Huertas-Company, M. and Jackson, N. and Jacobs, C. and Jullo, E. and Kneib, J. P. and Koopmans, L. V.E. and Lanusse, F. and Li, C. L. and Ma, Q. and Makler, M. and Li, N. and Lightman, M. and Petrillo, C. E. and Serjeant, S. and Sch{\"{a}}fer, C. and Sonnenfeld, A. and Tagore, A. and Tortora, C. and Tuccillo, D. and Valent{\'{i}}n, M. B. and Velasco-Forero, S. and {Verdoes Kleijn}, G. A. and Vernardos, G.}, -doi = {10.1051/0004-6361/201832797}, -eprint = {1802.03609}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Metcalf et al. - 2019 - The strong gravitational lens finding challenge(2).pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Gravitational lensing: strong - methods: data anal}, -title = {{The strong gravitational lens finding challenge}}, -url = {http://arxiv.org/abs/1802.03609%0Ahttp://dx.doi.org/10.1051/0004-6361/201832797}, -volume = {625}, -year = {2019} -} -@article{Holl2012, -abstract = {The Gaia mission has been designed to perform absolute astrometric measurements with unprecedented accuracy; the end-of-mission parallax standard error is required to be 30 micro-arcseconds for a G2V type star of magnitude 15. These requirements set a stringent constraint on the accuracy of the estimation of the location of the stellar image on the CCD for each observation: e.g., 0.3 milli-arseconds (mas) or 0.005 pixels for the same V=15 G2V star. However the Gaia CCDs will suffer from charge transfer inefficiency (CTI) caused by radiation damage that will degrade the stellar image quality and may degrade the astrometric performance of Gaia if not properly addressed. For the first time at this level of detail, the potential impact of radiation damage on the performance of Gaia is investigated. In this first paper we focus on the evaluation of the CTI impact on the image location accuracy. We show that CTI decreases the stellar image signal-to-noise ratio and irreversibly degrades the image location estimation precision. As a consequence the location estimation standard errors increase by up to 6{\%} for a radiation damage level equivalent to the end-of-mission. In addition the CTI-induced image distortion introduces a systematic bias in the image location estimation (up to 0.05 pixels or 3 mas in the Gaia operating conditions). We present a novel approach to CTI mitigation that enables, without correction of the raw data, the unbiased estimation of the image location and flux from damaged observations. Its implementation reduces the maximum measured location bias for the faintest magnitude to 0.005 pixels ({\$\sim${}}4e-4 pixels at magnitude 15). In a second paper we will investigate how the CTI effects affect the final astrometric accuracy of Gaia by propagating residual errors through the astrometric solution.}, -archivePrefix = {arXiv}, -arxivId = {1110.1547}, -author = {Holl, B and Prod'homme, T and Lindegren, L and Brown, A G A}, -doi = {10.1111/j.1365-2966.2012.20429.x}, -eprint = {1110.1547}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: numerical,Space vehicles}, -number = {4}, -pages = {2786--2807}, -title = {{The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solution}}, -volume = {422}, -year = {2012} -} -@article{Siverd2009, -abstract = {We identify, categorize, and quantify alignment effects among host and satellite galaxies using a spectroscopically-confirmed, low-redshift (z{\textless}0.23) galaxy sample from the Sloan Digital Sky Survey Data Release 6. Consistent with other recent findings, we find that satellite galaxies (SGs) of red, centrally concentrated (elliptical) host galaxies (HGs) with radial velocity separation |Delta{\_}V|{\textless}600 km/s preferentially reside near the projected major axes of their HGs. Among these, this preference is strongest for highly concentrated, red SGs. We find that fractional anisotropy increases with decreasing {\$}\backslash{\$}Delta{\_}V and Delta{\_}R and is nearly 40{\%} greater among the closest SGs (Delta{\_}R{\textless}250 kpc/h) relative to more distant (Delta{\_}R{\textgreater}500 kpc/h) SGs. For highly concentrated SGs at small ({\textless}300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to {\textless}15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby ({\textless}40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ({\$\sim${}}3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R J and Ryden, B S and Gaudi, B S}, -eprint = {0903.2264}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series which re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science database, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies (CSRG). This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications, and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution which limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ("encounter-driven") rings (such as ring and polar ring galaxies) are recognized in less than 1$\backslash${\%} of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of $\sim$1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G. and Schaye, Joop and Frenk, Carlos S. and Theuns, Tom and Schaller, Matthieu and Crain, Robert A. and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an en(4).pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an en(5).pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Collett2014, -abstract = {We present constraints on the equation of state of dark energy, w, and the total matter density, $\Omega$M, derived from the double-source-plane strong lens SDSSJ0946+1006, the first cosmological measurement with a galaxy-scale double-source-plane lens. By modelling the primary lens with an elliptical power-law mass distribution, and including perturbative lensing by the first source, we are able to constrain the cosmological scaling factor in this system to be $\beta$-1 = 1.404 ± 0.016, which implies $\Omega$M = 0.33+0.33-0.26 for a flat $\delta$ cold dark matter ($\delta$ CDM) cosmology. Combining with a cosmic microwave background prior from Planck, we find w = -1.17+0.20-0.21 assuming a flat wCDM cosmology. This inference shifts the posterior by 1$\sigma$ and improves the precision by 30 per cent with respect to Planck alone, and demonstrates the utility of combining simple, galaxy-scale multiple-source-plane lenses with other cosmological probes to improve precision and test for residual systematic biases. {\textcopyright} 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.5278}, -author = {Collett, Thomas E. and Auger, Matthew W.}, -doi = {10.1093/mnras/stu1190}, -eprint = {1403.5278}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Gravitational lensing: strong}, -number = {2}, -pages = {969--976}, -title = {{Cosmological constraints from the double source plane lens SDSSJ0946+1006}}, -volume = {443}, -year = {2014} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ {\textgreater} 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright}2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{Lani2013, -abstract = {We present evidence for a strong relationship between galaxy size and environment for the quiescent population in the redshift range 1 < z < 2. Environments were measured using projected galaxy overdensities on a scale of 400 kpc, as determined from $\sim$96 000 K-bandselected galaxies from the UKIDSS Ultra Deep Survey (UDS). Sizes were determined from ground-based K-band imaging, calibrated using space-based CANDELS HST observations in the centre of the UDS field, with photometric redshifts and stellar masses derived from 11-band photometric fitting. From the resulting size-mass relation, we confirm that quiescent galaxies at a given stellar mass were typically $\sim$50 per cent smaller at z $\sim$ 1.4 compared to the present day. At a given epoch, however, we find that passive galaxies in denser environments are on average significantly larger at a given stellar mass. The most massive quiescent galaxies (Mz.ast; >2×1011M⊙) atz>1 are typically 50 per cent larger in the highest density environments compared to those in the lowest density environments. Using Monte Carlo simulations, we reject the null hypothesis that the size-mass relation is independent of environment at a significance >4.8s for the redshift range 1< z<2. In contrast, the evidence for a relationship between size and environment is much weaker for star-forming galaxies. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1307.3247}, -author = {Lani, Caterina and Almaini, Omar and Hartley, William G. and Mortlock, Alice and H{\"{a}}u{\ss}ler, Boris and Chuter, Robert W. and Simpson, Chris and {Van der Wel}, Arjen and Gr{\"{u}}tzbauch, Ruth and Conselice, Christopher J. and Bradshaw, Emma J. and Cooper, Michael C. and Faber, Sandra M. and Grogin, Norman A. and Kocevski, Dale D. and Koekemoer, Anton M. and Lai, Kamson}, -doi = {10.1093/mnras/stt1275}, -eprint = {1307.3247}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: groups: general,Galaxies: haloes,Galaxies: structure,Infrared: galaxies}, -number = {1}, -pages = {207--221}, -title = {{Evidence for a correlation between the sizes of quiescent galaxies and local environment to z$\sim$2}}, -volume = {435}, -year = {2013} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful number of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag limit of ∼24. However, gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z ∼ 5–7 for LSST. We find that the LSST Wide Fast Deep survey could detect up to 120 lensed Population (Pop) I and II SNe but no lensed Pop III SNe. Deep-drilling programs in 10 deg2 fields could detect Pop I and II core-collapse SNe at AB magnitudes of 27–28 and 26, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes-Erik and Whalen, Daniel J and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S}, -doi = {10.1093/mnras/stz3203}, -eprint = {1805.02662}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cos-,cosmology,dark ages,early universe,first stars,galaxies,gravitational lensing,high-redshift,mology,observations,population iii,reionization,stars,strong}, -number = {2}, -pages = {2447--2459}, -title = {{Detecting strongly lensed supernovae at z ∼ 5–7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {491}, -year = {2020} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Mendez-Abreu2016, -abstract = {We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area data release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log (M∗/MȮ) {\textgreater} 11), the galaxy population is dominated by galaxies modelled with a single S{\'{e}}rsic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T {\textgreater} 0.2. At intermediate masses (9.5 {\textless} log (M∗/MȮ) {\textless} 11), galaxies described with bulge+disc but B/T {\textless} 0.2 are preponderant, whereas, at the low mass end (log (M∗/MȮ) {\textless} 9.5), the prevailing population is constituted by galaxies modelled with either purediscs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57{\%} of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5 {\textless} log (M∗/MȮ) {\textless} 11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62{\%}, 28{\%}, and 10{\%} for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.}, -archivePrefix = {arXiv}, -arxivId = {1610.05324}, -author = {M{\'{e}}ndez-Abreu, J and Ruiz-Lara, T and S{\'{a}}nchez-Menguiano, L and {De Lorenzo-C{\'{a}}ceres}, A and Costantin, L and Catal{\'{a}}n-Torrecilla, C and Florido, E and Aguerri, J A L and Bland-Hawthorn, J and Corsini, E M and Dettmar, R J and Galbany, L and Garc{\'{i}}a-Benito, R and Marino, R A and M{\'{a}}rquez, I and Ortega-Minakata, R A and Papaderos, P and S{\'{a}}nchez, S F and S{\'{a}}nchez-Blazquez, P and Spekkens, K and {Van De Ven}, G and Wild, V and Ziegler, B}, -doi = {10.1051/0004-6361/201629525}, -eprint = {1610.05324}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -title = {{Two-dimensional multi-component photometric decomposition of CALIFA galaxies}}, -url = {http://arxiv.org/abs/1610.05324%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201629525}, -volume = {598}, -year = {2017} -} -@article{Fe, -author = {By, Llustrated}, -keywords = {pee r}, -number = {1987}, -pages = {3--6}, -title = {{P 2 P 2 P 2}}, -volume = {93}, -year = {2009} -} -@article{Kotilainen2018, -abstract = {Recently, the relation between the masses of the black hole (MBH) and the host galaxy (Mhost) in quasars has been probed down to the parameter space ofMBH {\$\sim${}} 108M⊙ and Mhost {\$\sim${}} 1011M⊙ at z {\textless} 0.5. In this study, we have investigated the MBH-Mhost log-linear relation for a sample of 37 quasars with low black hole masses (107M⊙ {\textless} MBH {\textless} 108.3M⊙) at 0.5 {\textless} z {\textless} 1.0. The black hole masses were derived using virial mass estimates from Sloan Digital Sky Survey (SDSS) optical spectra. For 25 quasars, we detected the presence of the host galaxy from deep near-infraredH-band imaging, whereas upper limits for the host galaxy luminosity (mass) were estimated for the 12 unresolved quasars. We combined our previous studies with the results from this work to create a sample of 89 quasars at z {\textless} 1.0 having a large range of black hole masses (107M⊙ {\textless} MBH {\textless} 1010M⊙) and host galaxy masses (1010M⊙ {\textless} Mhost {\textless} 1013M⊙). Most of the quasars at the low-mass end lie below the extrapolation of the local relation. This apparent break in the linearity of the entire sample is due to increasing fraction of discdominated host galaxies in the low-mass quasars. After correcting for the disc component, and considering only the bulge component, the bilinear regression for the entire quasar sample holds over 3.5 dex in both the black hole mass and the bulge mass, and is in very good agreement with the local relation. We advocate secular evolution of discs of galaxies being responsible for the relatively strong disc domination.}, -archivePrefix = {arXiv}, -arxivId = {1409.1948}, -author = {Sanghvi, J and Kotilainen, J K and Falomo, R and Decarli, R and Karhunen, K and Uslenghi, M}, -doi = {10.1093/mnras/stu1822}, -eprint = {1409.1948}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: high-redshift,Galaxies: nuclei,Quasars: general}, -number = {2}, -pages = {1261--1268}, -title = {{The black hole-host galaxy relation for very low mass quasars}}, -volume = {445}, -year = {2014} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ({\$}z = 1.489{\$}), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5{\$}+{\$}2223 ({\$}z = 0.542{\$}), published by Grillo et al. (2016), and explore different {\$}\backslashLambda{\$}CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of {\$}H{\_}{\{}0{\}}{\$} and {\$}\backslashOmega{\_}{\{}\backslashrm m{\}}{\$} with relative (1{\$}\backslashsigma{\$}) statistical errors of, respectively, 6{\%} (7{\%}) and 31{\%} (26{\%}) in flat (general) cosmological models, assuming a conservative 3{\%} uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of {\$}H{\_}{\{}0{\}}{\$}, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C and Rosati, P and Suyu, S H and Balestra, I and Caminha, G B and Halkola, A and Kelly, P L and Lombardi, M and Mercurio, A and Rodney, S A and Treu, T}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -number = {2}, -pages = {94}, -title = {{Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”}}, -url = {http://arxiv.org/abs/1802.01584}, -volume = {860}, -year = {2018} -} -@article{Hoyos2011, -abstract = {We present a catalogue of structural parameters for 8814 galaxies in the 25 fields of the Hubble Space Telescope/ACS Coma Treasury Survey. Parameters from S{\'{e}}rsic fits to the two-dimensional surface brightness distributions are given for all galaxies from our published Coma photometric catalogue with mean effective surface brightness brighter than 26.0magarcsec-2 and brighter than 24.5mag (equivalent to absolute magnitude -10.5), as given by the fits, all in F814W(AB). The sample comprises a mixture of Coma members and background objects; 424 galaxies have redshifts and of these 163 are confirmed members. The fits were carried out using both the gim2dand galfit codes. We provide the following parameters: galaxy ID, RA, Dec., the total corrected automatic magnitude from the photometric catalogue, the total magnitude of the model (F814WAB), the geometric mean effective radius Re, the mean surface brightness within the effective radius 〈$\mu$〉e, the S{\'{e}}rsic index n, the ellipticity and the source position angle. The selection limits of the catalogue and the errors listed for the S{\'{e}}rsic parameters come from extensive simulations of the fitting process using synthetic galaxy models. The agreement between gim2d and galfit parameters is sensitive to details of the fitting procedure; for the settings employed here the agreement is excellent over the range of parameters covered in the catalogue. We define and present two goodness-of-fit indices which quantify the degree to which the image can be approximated by a S{\'{e}}rsic model with concentric, coaxial elliptical isophotes; such indices may be used to objectively select galaxies with more complex structures such as bulge-disc, bars or nuclear components. We make the catalogue available in electronic format at astro-wise and MAST. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1010.2352}, -author = {Hoyos, Carlos and {Den Brok}, Mark and Kleijn, Gijs Verdoes and Carter, David and Balcells, Marc and Guzm{\'{a}}n, Rafael and Peletier, Reynier and Ferguson, Henry C. and Goudfrooij, Paul and Graham, Alister W. and Hammer, Derek and Karick, Arna M. and Lucey, John R. and Matkovi{\'{c}}, Ana and Merritt, David and Mouhcine, Mustapha and Valentijn, Edwin}, -doi = {10.1111/j.1365-2966.2010.17855.x}, -eprint = {1010.2352}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: individual: Coma,Galaxies: dwarf,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: fundamental parameters}, -month = {mar}, -number = {4}, -pages = {2439--2460}, -title = {{The HST/ACS Coma Cluster Survey - III. Structural parameters of galaxies using single S{\'{e}}rsic fits}}, -volume = {411}, -year = {2011} -} -@article{Mandelbaum2017, -abstract = {Weak gravitational lensing, the deflection of light by mass, is one of the best tools to constrain the growth of cosmic structure with time and reveal the nature of dark energy. I discuss the sources of systematic uncertainty in weak lensing measurements and their theoretical interpretation, including our current understanding and other options for future improvement. These include long-standing concerns such as the estimation of coherent shears from galaxy images or redshift distributions of galaxies selected on the basis of photometric redshifts, along with systematic uncertainties that have received less attention to date because they are subdominant contributors to the error budget in current surveys. I also discuss methods for automated systematics detection using survey data of the 2020s. The goal of this review is to describe the current state of the field and what must be done so that if weak lensing measurements lead toward surprising conclusions about key questions such as the nature of dark energy, those conclusions will be credible.}, -archivePrefix = {arXiv}, -arxivId = {1710.03235}, -author = {Mandelbaum, Rachel}, -doi = {10.1146/annurev-astro-081817-051928}, -eprint = {1710.03235}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Mandelbaum - 2018 - Weak Lensing for Precision Cosmology.pdf:pdf}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {cosmological parameters,cosmology: observations,gravitational lensing,methods: data analysis,methods: statistical,techniques: image processing}, -number = {1}, -pages = {393--433}, -title = {{Weak Lensing for Precision Cosmology}}, -url = {http://arxiv.org/abs/1710.03235%0Ahttp://dx.doi.org/10.1146/annurev-astro-081817-051928}, -volume = {56}, -year = {2018} -} -@article{Barnabe2007, -abstract = {Gravitational lensing and stellar dynamics are two independent methods, based solely on gravity, to study the mass distributions of galaxies. Both methods suffer from degeneracies, however, that are difficult to break. In this paper, we present a new framework that self-consistently unifies gravitational lensing and stellar dynamics. This approach breaks some of classical degeneracies that have limited their individual usage, in particular in the study of high-redshift galaxies. The methodology is based on the premise that, for any given galaxy potential, the mapping of both the unknown lensed source brightness distribution and the stellar phase-space distribution function on to the photometric and kinematic observables, can be cast as a single set of coupled linear equations. This set of linear equations is solved, maximizing the likelihood penalty function. The evidence penalty function, as derived from Bayesian statistics, subsequently allows the best potential-model parameters to be found and potential-model families, or other model assumptions (e.g. PSF), to be quantitatively ranked. We have implemented a fast algorithm that solves for the maximum-likelihood pixelized lensed source brightness distribution and the two-integral stellar phase-space distribution function f(E, Lz), assuming axisymmetric potentials. To make the method practical, we have devised a new Monte-Carlo approach to Schwarzschild's orbital superposition method, based on the superposition of two-integral (E and Lz) toroidal components, to find the maximum-likelihood two-integral distribution function in a matter of seconds in any axisymmetric potential. The non-linear parameters of the potential are subsequently found through a hybrid MCMC and Simplex optimization of the evidence. (Abridged)}, -author = {Barnabe, Matteo and Koopmans, Leon V. E.}, -doi = {10.1086/520495}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Gravitational Lensing,Galaxies: Elliptical and Lenticular,Galaxies: Structure,Stellar Dynamics,cD}, -month = {sep}, -number = {2}, -pages = {726--746}, -title = {{A Unifying Framework for Self‐consistent Gravitational Lensing and Stellar Dynamics Analyses of Early‐Type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/666/i=2/a=726}, -volume = {666}, -year = {2007} -} -@article{Bois2011, -abstract = {We study the formation of early-type galaxies (ETGs) through mergers with a sample of 70 high-resolution (softening length <60pc and 12 × 10 6 particles) numerical simulations of binary mergers of disc galaxies (with 10 per cent of gas) and 16 simulations of ETG remergers. These simulations, designed to accompany observations and models conducted within the ATLAS 3D project, encompass various mass ratios (from 1:1 to 6:1), initial conditions and orbital parameters. The progenitor disc galaxies are spiral-like with bulge-to-disc ratios typical of Sb and Sc galaxies and high central baryonic angular momentum. We find that binary mergers of disc galaxies with mass ratios of 3:1 and 6:1 are nearly always classified as fast rotators according to the ATLAS 3D criterion (based on the $\lambda$ R parameter - ATLAS 3D Paper III): they preserve the structure of the input fast rotating spiral progenitors. They have intrinsic ellipticities larger than 0.5, cover intrinsic $\lambda$ R values between 0.2 and 0.6, within the range of observed fast rotators. The distribution of the observed fastest rotators does in fact coincide with the distribution of our disc progenitors. Major disc mergers (mass ratios of 2:1 and 1:1) lead to both fast and slow rotators. Most of the fast rotators produced in major mergers have intermediate flattening, with ellipticities $\epsilon$ between 0.4 and 0.6. Most slow rotators formed in these binary disc mergers hold a stellar kinematically distinct core (KDC) in their $\sim$1-3 central kiloparsec: these KDCs are built from the stellar components of the progenitors. However, these remnants are still very flat with $\epsilon$ often larger than 0.45 and sometimes as high as 0.65. Besides a handful of specific observed systems - the counter-rotating discs (2$\sigma$ galaxies, ATLAS 3D Paper II) - these therefore cannot reproduce the observed population of slow rotators in the nearby Universe. This sample of simulations supports the notion of slow and fast rotators: these two families of ETGs present distinct characteristics in term of their angular momentum content (at all radii) and intrinsic properties - the slow rotators are not simply velocity-scaled down versions of fast rotators. The mass ratio of the progenitors is a fundamental parameter for the formation of slow rotators in these binary mergers, but it also requires a retrograde spin for the earlier-type (Sb) progenitor galaxy with respect to the orbital angular momentum. We also study remergers of these merger remnants: these produce relatively round fast rotators or systems near the threshold for slow rotators. In such cases, the orbital angular momentum dominates the central region, and these systems no longer exhibit a KDC, as KDCs are destroyed during the remergers and do not re-form in these relatively dry events. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1105.4076}, -author = {Bois, Maxime and Emsellem, Eric and Bournaud, Fr{\'{e}}d{\'{e}}ric and Alatalo, Katherine and Blitz, Leo and Bureau, Martin and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Khochfar, Sadegh and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19113.x}, -eprint = {1105.4076}, -isbn = {9781595937629}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: formation,Galaxies: interactions,Galaxies: kinematics and dynamics,Methods: numerical}, -month = {sep}, -number = {3}, -pages = {1654--1679}, -title = {{The ATLAS 3D project - VI. Simulations of binary galaxy mergers and the link with fast rotators, slow rotators and kinematically distinct cores}}, -url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.19113.x%5Cnhttp://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.19113.x/full}, -volume = {416}, -year = {2011} -} -@article{Hopkins2006, -abstract = {We present an evolutionary model for starbursts, quasars, and spheroidal galaxies in which mergers between gas-rich galaxies drive nuclear inflows of gas, producing intense starbursts and feeding the buried growth of supermassive black holes (BHs) until feedback expels gas and renders a briefly visible optical quasar. The quasar lifetime and obscuring column density depend on both the instantaneous and peak luminosity of the quasar, and we determine this dependence using a large set of simulations of galaxy mergers varying host galaxy properties, orbital geometry, and gas physics. We use these fits to deconvolve observed quasar luminosity functions (LFs) and obtain the evolution of the formation rate of quasars with a certain peak luminosity, n(L{\_}peak,z). Quasars spend extended periods of time at luminosities well below peak, and so n(L{\_}peak) has a maximum corresponding to the 'break' in the observed LF, falling off at both brighter and fainter luminosities. From n(L{\_}peak) and our simulation results, we obtain self-consistent fits to hard and soft X-ray and optical quasar LFs and predict many observables, including: column density distributions of optical and X-ray samples, the LF of broad-line quasars in X-ray samples and the broad-line fraction as a function of luminosity, active BH mass functions, the distribution of Eddington ratios at z{\$\sim${}}0-2, the z=0 mass function of relic BHs and total mass density of BHs, and the cosmic X-ray background. In every case, our predictions agree well with observed estimates, and unlike previous modeling attempts, we are able to reproduce them without invoking any ad hoc assumptions about source properties or distributions. We provide a library of Monte Carlo realizations of our models for comparison with observations. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506398}, -author = {Hopkins, Philip F and Hernquist, Lars and Cox, Thomas J and {Di Matteo}, Tiziana and Robertson, Brant and Springel, Volker}, -doi = {10.1086/499298}, -eprint = {0506398}, -isbn = {doi:10.1086/499298}, -issn = {0067-0049}, -journal = {The Astrophysical Journal Supplement Series}, -number = {1}, -pages = {1--49}, -primaryClass = {astro-ph}, -title = {{A Unified, Merger-Driven Model for the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes and Galaxy Spheroids}}, -url = {http://arxiv.org/abs/astro-ph/0506398%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/499298}, -volume = {163}, -year = {2005} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P{\_}KS $\backslash$simeq 1.5 $\backslash$times 10{\^{}}{\{}-4{\}}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability $\backslash$simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R and Kravtsov, Andrey V and Gnedin, Oleg Y and Klypin, Anatoly A}, -doi = {10.1086/431355}, -eprint = {0502496}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z{\$\sim${}}2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and Sersic index distributions obtained from 2D structural fits to {\$\sim${}}40,000{\$} nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However the distribution of Sersic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own.}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful numbers of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag 24 - 25 limits. But gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z {\$\sim${}} 5 - 7 for LSST. We find that the LSST main survey could detect {\$\sim${}} 1 - 2 lensed Population III (Pop III) SN but 130-1400 Pop I/II SNe. An alternative deep survey with a one-year cadence could find {\$\sim${}}10 Pop III SNe with an 84h exposure and {\$\sim${}}50 SNe with a 420h exposure.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes-Erik and Whalen, Daniel J and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S}, -eprint = {1805.02662}, -keywords = {cos-,cosmology,dark ages,early universe,first stars,galaxies,gravitational lensing,high-redshift,mology,observations,population iii,reionization,stars,strong}, -number = {May}, -pages = {1--12}, -title = {{Detecting strongly lensed supernovae at z {\$\sim${}} 5-7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {12}, -year = {2018} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned r- and g-band images from a sample of 45 508 galaxies from Sloan Digital Sky Survey Data Release 9 in the redshift range 0.06≤z≤0.1 and in the mass range 1010.0M⊙ {\textless}M* {\textless} 1011.4M⊙.We derive surface brightness profiles to a depth of almost $\mu$r ̃ 32 mag arcsec-2. We find that the ellipticity of the stellar halo is a function of galaxy stellar mass and that the haloes of high-concentration galaxies are more elliptical than those of low-concentration galaxies. Where the g - r colour of the stellar halo can be measured, we find that the stellar light is always bluer than in the main galaxy. The colour of the stellar halo is redder for more massive galaxies. We further demonstrate that the full two-dimensional surface intensity distribution of our galaxy stacks can only be fit through multicomponent S{\'{e}}rsic models. Using the fraction of light in the outer component of the models as a proxy for the fraction of accreted stellar light, we show that this fraction is a function of stellar mass and galaxy type. The fraction of accreted stellar light rises from 30 to 70 per cent and from 2 to 25 per cent for high- and low-concentration galaxies, respectively, over the mass range 1010.0-1011.4M⊙. {\textcopyright}2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1404.2123}, -author = {D'Souza, Richard and Kauffman, Guinevere and Wang, Jing and Vegetti, Simona}, -doi = {10.1093/mnras/stu1194}, -eprint = {1404.2123}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: halo,Galaxy: structure}, -number = {2}, -pages = {1433--1450}, -title = {{Parametrizing the stellar haloes of galaxies}}, -volume = {443}, -year = {2014} -} -@article{Peng2010, -abstract = {We present a two-dimensional (2D) fitting algorithm (GALFIT, ver. 3) with new capabilities to study the structural components of galaxies and other astronomical objects in digital images. Our technique improves on previous 2D fitting algorithms by allowing for irregular, curved, logarithmic and power-law spirals, ring, and truncated shapes in otherwise traditional parametric functions like the S{\'{e}}rsic, Moffat, King, Ferrer, etc., profiles. One can mix and match these new shape features freely, with or without constraints, and apply them to an arbitrary number of model components of numerous profile types, so as to produce realistic-looking galaxy model images. Yet, despite the potential for extreme complexity, the meaning of the key parameters like the S{\'{e}}rsic index, effective radius, or luminosity remains intuitive and essentially unchanged. The new features have an interesting potential for use to quantify the degree of asymmetry of galaxies, to quantify low surface brightness tidal features beneath and beyond luminous galaxies, to allow more realistic decompositions of galaxy subcomponents in the presence of strong rings and spiral arms, and to enable ways to gauge the uncertainties when decomposing galaxy subcomponents. We illustrate these new features by way of several case studies that display various levels of complexity. {\textcopyright}2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0912.0731}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans Walter}, -doi = {10.1088/0004-6256/139/6/2097}, -eprint = {0912.0731}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Galaxies: bulges,Galaxies: fundamental parameters,Galaxies: structure,Techniques: image processing,Techniques: photometric}, -number = {6}, -pages = {2097--2129}, -title = {{Detailed decomposition of galaxy images. II. beyond axisymmetric models}}, -volume = {139}, -year = {2010} -} -@article{Pulsoni2017, -abstract = {Wolbachia is an intracellular endosymbiont that induces a variety of reproductive alterations in diverse arthropods. The almond moth, Cadra cautella, is double infected with two Wolbachia variants, wCauA and wCauB, and expresses complete cytoplasmic incompatibility (CI). The individual contribution of wCauA and wCauB to the expression of CI are unclear, however, because the two variants have not been separated in this host. The effect of wCauA is of particular interest because it induces male killing when transferred into the Mediterranean flour moth, Ephestia kuehniella. In the present study, we generated C. cautella infected with only wCauA by treating double-infected insects with tetracycline. Single-infected C. cautella exhibited strong CI, demonstrating that wCauA induces two distinct reproductive phenotypes in different hosts: CI in C. cautella and male killing in E. kuehniella. CI was also observed in the cross of double-infected males and single-infected females. Comparison of the single- and double-infected insects by real-time quantitative polymerase chain reaction suggested that the wCauA density is not affected much by the presence or absence of wCauB. {\textcopyright} 2005 Nature Publishing Group All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {http://www.R-project.org}, -author = {Sasaki, T. and Massaki, N. and Kubo, T.}, -doi = {10.1038/sj.hdy.6800737}, -eprint = {/www.R-project.org}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sasaki, Massaki, Kubo - 2005 - Wolbachia variant that induces two distinct reproductive phenotypes in different hosts.pdf:pdf}, -isbn = {0018-067X}, -issn = {0018067X}, -journal = {Heredity}, -keywords = {Cadra cautella,Cytoplasmic incompatibility,Double infection,Male killing,Real-time quantitative PCR,Wolbachia}, -number = {5}, -pages = {389--393}, -pmid = {16106260}, -primaryClass = {http:}, -title = {{Wolbachia variant that induces two distinct reproductive phenotypes in different hosts}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/16106260}, -volume = {95}, -year = {2005} -} -@article{Yan2016a, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R$\sim$2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is $\sim$73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R. and Bershady, Matthew A. and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M. and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R. and Thomas, Daniel and Wake, David A. and Weijmans, Anne-Marie and Westfall, Kyle B. and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A. and Blanton, Michael R. and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T. and Goddard, Daniel and Gunn, James E. and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R. and Oravetz, Daniel and Pan, Kaike and Parejko, John K. and Sanchez, Sebastian F. and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yan et al. - 2016 - SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY.pdf:pdf}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {6}, -pages = {197}, -title = {{SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY}}, -url = {http://arxiv.org/abs/1607.08613%0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {152}, -year = {2016} -} -@article{Peng2002, -abstract = {We present a two-dimensional (2-D) fitting algorithm (GALFIT) designed to extract structural components from galaxy images, with emphasis on closely modeling light profiles of spatially well-resolved, nearby galaxies observed with the Hubble Space Telescope. Our algorithm improves on previous techniques in two areas, by being able to simultaneously fit a galaxy with an arbitrary number of components, and with optimization in computation speed, suited for working on large galaxy images. We use 2-D models such as the ``Nuker'' law, the Sersic (de Vaucouleurs) profile, an exponential disk, and Gaussian or Moffat functions. The azimuthal shapes are generalized ellipses that can fit disky and boxy components. Many galaxies with complex isophotes, ellipticity changes, and position-angle twists can be modeled accurately in 2-D. When examined in detail, we find that even simple-looking galaxies generally require at least three components to be modeled accurately, rather than the one or two components more often employed. We illustrate this by way of 7 case studies, which include regular and barred spiral galaxies, highly disky lenticular galaxies, and elliptical galaxies displaying various levels of complexities. A useful extension of this algorithm is to accurately extract nuclear point sources in galaxies. We compare 2-D and 1-D extraction techniques on simulated images of galaxies having nuclear slopes with different degrees of cuspiness, and we then illustrate the application of the program to several examples of nearby galaxies with weak nuclei.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0204182}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans-Walter}, -doi = {10.1086/340952}, -eprint = {0204182}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {1}, -pages = {266--293}, -primaryClass = {astro-ph}, -title = {{Detailed Structural Decomposition of Galaxy Images}}, -url = {http://arxiv.org/abs/astro-ph/0204182%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/340952}, -volume = {124}, -year = {2002} -} -@inproceedings{MartinNavarro2013, -abstract = {We have developed an innovative 'index scanning technique” to map the stellar kinematics of early-type galaxies by measuring for the first time the absorption line strength of the near-IR CaII triplet with the Red Tunable Filters of OSIRIS at GTC. Unlike classical spectroscopy, these filters allow us to perform a two-dimensional study, taking advantage of a 10.4 meter class telescope with a unvignetted field of view of 7.8 × 7.8 arcmin. We show the velocity fields obtained for two Virgo elliptical galaxies of very different masses and their globular cluster systems reaching galactocentric distances beyond 2 effective radii.}, -author = {Mart{\'{i}}n-Navarro, Ignacio and Vazdekis, Alexander and Bongiovanni, {\'{A}}ngel and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and Cepa, Jordi and Cenarro, Javier and S{\'{a}}nchez-Bl{\'{a}}zquez, Patricia}, -booktitle = {Proceedings of the 10th Scientific Meeting of the Spanish Astronomical Society - Highlights of Spanish Astrophysics VII, SEA 2012}, -editor = {Guirado, J.$\sim$C. and Lara, L.$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable filters at gtc: A novel approach}}, -year = {2020} -} -@article{Deason2011, -abstract = {We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the gimic suite of simulations. gimic consists of resimulations of five cosmologically representative regions from the Millennium Simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r∼ 0.1r200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r∼r200). Misalignments of {\textgreater}45° are seen in ∼30 per cent of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20 per cent of the satellite systems with 10 bright galaxies within r200 exhibit a polar spatial alignment with respect to the galaxy - an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction (∼10 per cent) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z= 0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation - the memory of their accretion history can remain intact to z= 0. Understanding the phase-space distribution of the z= 0 satellite population is key for studies that estimate the host halo mass from the line-of-sight velocities and projected positions of satellite galaxies. We quantify the effects of such systematics in estimates of the host halo mass from the satellite population. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A J and Mccarthy, I G and Font, A S and Evans, N W and Frenk, C S and Belokurov, V and Libeskind, N I and Crain, R A and Theuns, T}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Greene2017b, -abstract = {The "kinematic" morphology-density relation for early-type galaxies posits that those galaxies with low angular momentum are preferentially found in the highest-density regions of the universe. We use a large sample of galaxy groups with halo masses 10{\^{}}12.5 {\textless}M{\_}halo {\textless}10{\^{}}14.5 M{\_}sun/h observed with the Mapping Nearby Galaxies at APO (MaNGA) survey to examine whether there is a correlation between local environment and rotational support that is independent of stellar mass. We find no compelling evidence for a relationship between the angular momentum content of early-type galaxies and either local overdensity or radial position within the group at fixed stellar mass.}, -archivePrefix = {arXiv}, -arxivId = {1708.07843}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Goddard, D and Ge, J and Andrews, B H and Brinkman, J and Brownstein, J R and Greco, J P and Law, D and Lin, Y -T. and Masters, K L and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Yan, R and Drory, N}, -doi = {10.3847/2041-8213/aa8ace}, -eprint = {1708.07843}, -issn = {2041-8213}, -pages = {1--6}, -title = {{Probing the kinematic morphology-density relation of early-type galaxies with MaNGA}}, -url = {http://arxiv.org/abs/1708.07843%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa8ace}, -year = {2017} -} -@article{Sales2012a, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V. and Navarro, Julio F. and Theuns, Tom and Schaye, Joop and White, Simon D.M. and Frenk, Carlos S. and Crain, Robert A. and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sales et al. - 2012 - The origin of discs and spheroids in simulated galaxies(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z > 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G.}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2006 - Breaking the hierarchy of galaxy formation(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -month = {aug}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -volume = {370}, -year = {2006} -} -@article{De-Lucia:2007aa, -abstract = {We use semi-analytic techniques to study the formation and evolution of brightest cluster galaxies (BCGs). We show the extreme hierarchical nature of these objects and discuss the limitations of simple ways to capture their evolution. In a model where cooling flows are suppressed at late times by active galactic nucleus (AGN) activity, the stars of BCGs are formed very early (50 per cent at z ∼ 5, 80 per cent at z ∼ 3) and in many small galaxies. The high star formation rates in these high-z progenitors are fuelled by rapid cooling, not by merger-triggered starbursts. We find that model BCGs assemble surprisingly late: half their final mass is typically locked up in a single galaxy after z ∼ 0.5. Because most of the galaxies accreted on to BCGs have little gas content and red colours, late mergers do not change the apparent age of BCGs. It is this accumulation of a large number of old stellar populations - driven mainly by the merging history of the dark matter halo itself - that yields the observed homogeneity of BCG properties. In the second part of the paper, we discuss the evolution of BCGs to high redshifts, from both observational and theoretical viewpoints. We show that our model BCGs are in qualitative agreement with high-z observations. We discuss the hierarchical link between high-z BCGs and their local counterparts. We show that high-z BCGs belong to the same population as the massive end of local BCG progenitors, although they are not in general the same galaxies. Similarly, high-z BCGs end up as massive galaxies in the local Universe, although only a fraction of them are actually BCGs of massive clusters. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0606519}, -author = {{De Lucia}, Gabriella and Blaizot, J{\'{e}}r{\'{e}}my}, -doi = {10.1111/j.1365-2966.2006.11287.x}, -eprint = {0606519}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/De Lucia, Blaizot - 2007 - The hierarchical formation of the brightest cluster galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: stellar content}, -month = {feb}, -number = {1}, -pages = {2--14}, -primaryClass = {astro-ph}, -title = {{The hierarchical formation of the brightest cluster galaxies}}, -volume = {375}, -year = {2007} -} -@article{Kochanek2004, -abstract = {The new edition of this international bestseller continues to throw light on the world of statistics for health care professionals and medical students. Revised throughout, the 11th edition features new material in the areas of relative risk, absolute risk and numbers needed to treat diagnostic tests, sensitivity, specificity, ROC curves free statistical software The popular self-testing exercises at the end of every chapter are strengthened by the addition of new sections on reading and reporting statistics and formula appreciation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407232}, -author = {Middleton, D.}, -doi = {10.1136/bmj.2.6042.1008-b}, -eprint = {0407232}, -issn = {00071447}, -journal = {British Medical Journal}, -number = {6042}, -pages = {1008--1009}, -primaryClass = {astro-ph}, -title = {{“Statistics at square one”}}, -url = {http://arxiv.org/abs/astro-ph/0407232}, -volume = {2}, -year = {1976} -} -@article{Tran2022, -abstract = {We present spectroscopic confirmation of candidate strong gravitational lenses using the Keck Observatory and Very Large Telescope as part of our ASTRO 3D Galaxy Evolution with Lenses ( AGEL ) survey. We confirm that (1) search methods using convolutional neural networks (CNNs) with visual inspection successfully identify strong gravitational lenses and (2) the lenses are at higher redshifts relative to existing surveys due to the combination of deeper and higher-resolution imaging from DECam and spectroscopy spanning optical to near-infrared wavelengths. We measure 104 redshifts in 77 systems selected from a catalog in the DES and DECaLS imaging fields ( r ≤ 22 mag). Combining our results with published redshifts, we present redshifts for 68 lenses and establish that CNN-based searches are highly effective for use in future imaging surveys with a success rate of at least 88% (defined as 68/77). We report 53 strong lenses with spectroscopic redshifts for both the deflector and source ( z src > z defl ), and 15 lenses with a spectroscopic redshift for either the deflector ( z defl > 0.21) or source ( z src ≥ 1.34). For the 68 lenses, the deflectors and sources have average redshifts and standard deviations of 0.58 ± 0.14 and 1.92 ± 0.59 respectively, and corresponding redshift ranges of z defl = 0.21–0.89 and z src = 0.88–3.55. The AGEL systems include 41 deflectors at z defl ≥ 0.5 that are ideal for follow-up studies to track how mass density profiles evolve with redshift. Our goal with AGEL is to spectroscopically confirm ∼100 strong gravitational lenses that can be observed from both hemispheres throughout the year. The AGEL survey is a resource for refining automated all-sky searches and addressing a range of questions in astrophysics and cosmology.}, -archivePrefix = {arXiv}, -arxivId = {2205.05307}, -author = {Tran, Kim-Vy H. and Harshan, Anishya and Glazebrook, Karl and {Vasan G. C.}, Keerthi and Jones, Tucker and Jacobs, Colin and Kacprzak, Glenn G. and Barone, Tania M. and Collett, Thomas E. and Gupta, Anshu and Henderson, Astrid and Kewley, Lisa J. and Lopez, Sebastian and Nanayakkara, Themiya and Sanders, Ryan L. and Sweet, Sarah M.}, -doi = {10.3847/1538-3881/ac7da2}, -eprint = {2205.05307}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Tran2022AGEL.pdf:pdf}, -issn = {0004-6256}, -journal = {AJ}, -keywords = {Galaxy evolution,Galaxy formation,Optical astronomy,Redshift surveys,Spectroscopy,Strong gravitational lensing}, -number = {4}, -pages = {148}, -publisher = {IOP Publishing}, -title = {{The AGEL Survey: Spectroscopic Confirmation of Strong Gravitational Lenses in the DES and DECaLS Fields Selected Using Convolutional Neural Networks}}, -url = {http://dx.doi.org/10.3847/1538-3881/ac7da2}, -volume = {164}, -year = {2022} -} -@article{MacArthur2009a, -abstract = {RESUMEN Presentar el caso de un paciente canino, con enfermedad hep{\'{a}}tica, asociada a carcinoma hepatocelular. Fue estudiado el caso de un paciente canino de raza Pitt bull de 10 a{\~{n}}os de edad, al que se le encontraron m{\'{u}}ltiples n{\'{o}}dulos distribuidos en todo el par{\'{e}}nquima hep{\'{a}}tico, con diagnostico histopatol{\'{o}}gico de carcinoma hepatocelular. Se expone el caso cl{\'{i}}nico de un paciente canino de raza Pitt bull, que es presentado a consulta externa por presentar decaimiento y distensi{\'{o}}n abdominal, una vez realizado el examen f{\'{i}}sico sistem{\'{a}}tico se evidenci{\'{o}} hepatomegalia y un crecimiento anormal hacia la regi{\'{o}}n del mesogastrio derecho. Los ex{\'{a}}menes paraclinicos e histopatol{\'{o}}gicos demostraron la presencia de enfermedad hep{\'{a}}tica asociada a carcinoma hepatocelular. El carcinoma hepatocelular es una entidad de rara presentaci{\'{o}}n, cl{\'{i}}nicamente cursa con signos muy similares a otras alteraciones tumorales de compromiso hep{\'{a}}tico, su diagn{\'{o}}stico suele ser histopatol{\'{o}}gico.}, -archivePrefix = {arXiv}, -arxivId = {0901.4135}, -author = {{Edwin Buritic{\'{a}}}, G and {Ximena Barbosa}, S and {Diego Echeverry}, B}, -doi = {10.1111/j.1365-2966.2009.14519.x}, -eprint = {0901.4135}, -issn = {19090544}, -journal = {Revista MVZ Cordoba}, -keywords = {Canine,Carcinoma,Hepatocelullar}, -number = {2}, -pages = {1756--1761}, -title = {{Carcinoma hepatocelular canino: Reporte de un caso}}, -volume = {14}, -year = {2009} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -publisher = {MNRAS}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Birrer2020, -abstract = {The H0LiCOW collaboration inferred via strong gravitational lensing time delays a Hubble constant value of H0 = 73.3-1.8+1.7 km s-1 Mpc-1, describing deflector mass density profiles by either a power-law or stars (constant mass-to-light ratio) plus standard dark matter halos. The mass-sheet transform (MST) that leaves the lensing observables unchanged is considered the dominant source of residual uncertainty in H0. We quantify any potential effect of the MST with a flexible family of mass models, which directly encodes it, and they are hence maximally degenerate with H0. Our calculation is based on a new hierarchical Bayesian approach in which the MST is only constrained by stellar kinematics. The approach is validated on mock lenses, which are generated from hydrodynamic simulations. We first applied the inference to the TDCOSMO sample of seven lenses, six of which are from H0LiCOW, and measured H0 = 74.5-6.1+5.6 km s-1 Mpc-1. Secondly, in order to further constrain the deflector mass density profiles, we added imaging and spectroscopy for a set of 33 strong gravitational lenses from the Sloan Lens ACS (SLACS) sample. For nine of the 33 SLAC lenses, we used resolved kinematics to constrain the stellar anisotropy. From the joint hierarchical analysis of the TDCOSMO+SLACS sample, we measured H0 = 67.4-3.2+4.1 km s-1 Mpc-1. This measurement assumes that the TDCOSMO and SLACS galaxies are drawn from the same parent population. The blind H0LiCOW, TDCOSMO-only and TDCOSMO+SLACS analyses are in mutual statistical agreement. The TDCOSMO+SLACS analysis prefers marginally shallower mass profiles than H0LiCOW or TDCOSMO-only. Without relying on the form of the mass density profile used by H0LiCOW, we achieve a ∼5% measurement of H0. While our new hierarchical analysis does not statistically invalidate the mass profile assumptions by H0LiCOW - and thus the H0 measurement relying on them - it demonstrates the importance of understanding the mass density profile of elliptical galaxies. The uncertainties on H0 derived in this paper can be reduced by physical or observational priors on the form of the mass profile, or by additional data.}, -archivePrefix = {arXiv}, -arxivId = {2007.02941}, -author = {Birrer, S. and Shajib, A. J. and Galan, A. and Millon, M. and Treu, T. and Agnello, A. and Auger, M. and Chen, G. C.F. and Christensen, L. and Collett, T. and Courbin, F. and Fassnacht, C. D. and Koopmans, L. V.E. and Marshall, P. J. and Park, J. W. and Rusu, C. E. and Sluse, D. and Spiniello, C. and Suyu, S. H. and Wagner-Carena, S. and Wong, K. C. and Barnab{\`{e}}, M. and Bolton, A. S. and Czoske, O. and Ding, X. and Frieman, J. A. and {Van De Vyvere}, L.}, -doi = {10.1051/0004-6361/202038861}, -eprint = {2007.02941}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Birrer2020TDCOSMOSIVH0.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Cosmological parameters,Cosmology: observations,Distance scale,Galaxies: general,Galaxies: kinematics and dynamics,Gravitational lensing: strong}, -number = {Refsdal 1964}, -title = {{TDCOSMO: IV. Hierarchical time-delay cosmography - Joint inference of the Hubble constant and galaxy density profiles}}, -volume = {643}, -year = {2020} -} -@article{Schaller2015, -abstract = {We use the `Evolution and assembly of galaxies and their environments' (EAGLE) cosmological simulation to investigate the effect of baryons on the density profiles of rich galaxy clusters. We focus on EAGLE clusters with M200 > 1014 M⊙ of which we have six examples. The central brightest cluster galaxies (BCGs) in the simulation have steep stellar density profiles, $\rho$*(r) ∝ r-3. Stars dominate the mass density for r < 10 kpc, and, as a result, the total mass density profiles are steeper than the Navarro-Frenk-White (NFW) profile, in remarkable agreement with observations. The dark matter halo itself closely follows the NFW form at all resolved radii (r ≳ 3.0 kpc). The EAGLE BCGs have similar surface brightness and line-of-sight velocity dispersion profiles as the BCGs in the sample of Newman et al., which have the most detailed measurements currently available. After subtracting the contribution of the stars to the central density, Newman et al. infer significantly shallower slopes than the NFW value, in contradiction with the EAGLE results. We discuss possible reasons for this discrepancy, and conclude that an inconsistency between the kinematical model adopted by Newman et al. for their BCGs, which assumes isotropic stellar orbits, and the kinematical structure of the EAGLE BCGs, in which the orbital stellar anisotropy varies with radius and tends to be radially biased, could explain at least part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1409.8297}, -author = {Schaller, Matthieu and Frenk, Carlos S. and Bower, Richard G. and Theuns, Tom and Trayford, James and Crain, Robert A. and Furlong, Michelle and Schaye, Joop and {Dalla Vecchia}, Claudio and McCarthy, I. G.}, -doi = {10.1093/mnras/stv1341}, -eprint = {1409.8297}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: clusters: general,galaxies: haloes}, -month = {sep}, -number = {1}, -pages = {343--355}, -title = {{The effect of baryons on the inner density profiles of rich clusters}}, -url = {http://adsabs.harvard.edu/abs/2014arXiv1409.8297S}, -volume = {452}, -year = {2015} -} -@article{Hopkins2009, -abstract = {Transformation of disks into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in halos according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the over-production of spheroids: low and intermediate-mass galaxies are predicted to be bulge-dominated (B/T{\$\sim${}}0.5 at {\textless}10{\^{}}10 M{\_}sun), with almost no bulgeless systems), even if they have avoided major mergers. Including the different physical behavior of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T{\$\sim${}}0.1 at {\textless}10{\^{}}10 M{\_}sun, with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behavior of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests.}, -archivePrefix = {arXiv}, -arxivId = {0901.4111}, -author = {Hopkins, Philip F and Somerville, Rachel S and Cox, Thomas J and Hernquist, Lars and Jogee, Shardha and Kere{\v{s}}, Dusan and Ma, Chung Pei and Robertson, Brant and Stewart, Kyle}, -doi = {10.1111/j.1365-2966.2009.14983.x}, -eprint = {0901.4111}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Galaxies: spiral}, -number = {2}, -pages = {802--814}, -title = {{The effects of gas on morphological transformation in mergers: Implications for bulge and disc demographics}}, -volume = {397}, -year = {2009} -} -@article{Agustsson2007a, -abstract = {We investigate the locations of the satellites of relatively isolated host galaxies in the Sloan Digital Sky Survey and the Millennium Run simulation. Provided we use two distinct prescriptions to embed luminous galaxies within the simulated dark matter halos (ellipticals share the shapes of their halos, while disks have angular momenta that are aligned with the net angular momenta of their halos), we find a fair agreement between observation and theory. Averaged over scales rp 500 kpc, the satellites of red, high-mass hosts with low star formation rates are found preferentially near the major axes of their hosts. In contrast, the satellites of blue, low-mass hosts with low star formation rates show little to no anisotropy when averaged over the same scale. The difference between the locations of the satellites of red and blue hosts cannot be explained by the effects of interlopers in the data. Instead, it is caused primarily by marked differences in the dependence of the mean satellite location, $\phi$, on the projected distance at which the satellites are found. We also find that the locations of red, high-mass satellites with low star formation rates show considerably more anisotropy than do the locations of blue, low-mass satellites with high star formation rates. There are two contributors to this result. First, the blue satellites have only recently arrived within their hosts' halos, while the red satellites arrived in the far distant past. Second, the sample of blue satellites is heavily contaminated by interlopers, which suppresses the measured anisotropy compared to the intrinsic anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {0704.3441}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G.}, -doi = {10.1088/0004-637X/709/2/1321}, -eprint = {0704.3441}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Agustsson, Brainerd - 2010 - Anisotropic locations of satellite galaxies Clues to the orientations of galaxies within their dark matter.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: dwarf,Galaxies: fundamental parameters,Galaxies: halos,Galaxies: structure}, -number = {2}, -pages = {1321--1336}, -title = {{Anisotropic locations of satellite galaxies: Clues to the orientations of galaxies within their dark matter halos}}, -url = {http://arxiv.org/abs/0704.3441%0Ahttp://dx.doi.org/10.1088/0004-637X/709/2/1321}, -volume = {709}, -year = {2010} -} -@article{Ikarashi2014, -abstract = {We report the source size distribution, as measured by ALMA millimetric continuum imaging, of a sample of 13 AzTEC-selected submillimeter galaxies (SMGs) at zphot ∼ 3-6. Their infrared luminosities and star formation rates (SFRs) are LIR∼ 2-6 × 1012 L⊙ and ∼200-600 M⊙ yr1, respectively. The sizes of these SMGs range from 0″ 10 to 0″ 38, with a median of 0″ 20 -0″05+0″03 (FWHM), corresponding to a median circularized effective radius (Rc,e) of 0.67-0.14+0.13 kpc, comparable to the typical size of the stellar component measured in compact quiescent galaxies at z ∼ 2 (cQGs)-Re ∼ 1 kpc. The median surface SFR density of our SMGs is 100-26+42 M yr1 kpc2, comparable to that seen in local merger-driven (U)LIRGs rather than in extended disk galaxies at low and high redshifts. The discovery of compact starbursts in z ≳ 3 SMGs strongly supports a massive galaxy formation scenario wherein z ∼ 3-6 SMGs evolve into the compact stellar components of z ∼ 2 cQGs. These cQGs are then thought to evolve into the most massive ellipticals in the local universe, mostly via dry mergers. Our results thus suggest that z ≳ 3 SMGs are the likely progenitors of massive local ellipticals, via cQGs, meaning that we can now trace the evolutionary path of the most massive galaxies over a period encompassing ∼90% of the age of the universe.}, -archivePrefix = {arXiv}, -arxivId = {1411.5038}, -author = {Ikarashi, Soh and Ivison, R. J. and Caputi, Karina I. and Aretxaga, Itziar and Dunlop, James S. and Hatsukade, Bunyo and Hughes, David H. and Iono, Daisuke and Izumi, Takuma and Kawabe, Ryohei and Kohno, Kotaro and Lagos, Claudia D.P. and Motohara, Kentaro and Nakanishi, Kouichiro and Ohta, Kouji and Tamura, Yoichi and Umehata, Hideki and Wilson, Grant W. and Yabe, Kiyoto and Yun, Min S.}, -doi = {10.1088/0004-637X/810/2/133}, -eprint = {1411.5038}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: high-redshift,submillimeter: galaxies}, -number = {2}, -pages = {133}, -title = {{Compact starbursts in z ∼ 3-6 submillimeter galaxies revealed by ALMA}}, -url = {http://stacks.iop.org/0004-637X/810/i=2/a=133?key=crossref.086f0a3643102b0606542cef2c0a73d3}, -volume = {810}, -year = {2015} -} -@article{Krist2004, -abstract = {Point spread function (PSF) models are critical to Hubble Space Telescope (HST) data analysis. Astronomers unfamiliar with optical simulation techniques need access to PSF models that properly match the conditions of their observations, so any HST modeling software needs to be both easy-to-use and have detailed information on the telescope and instruments. The Tiny Tim PSF simulation software package has been the standard HST modeling software since its release in early 1992. We discuss the evolution of Tiny Tim over the years as new instruments and optical properties have been incorporated. We also demonstrate how Tiny Tim PSF models have been used for HST data analysis. Tiny Tim is freely available from tinytim.stsci.edu.}, -author = {Krist, John E. and Hook, Richard N. and Stoehr, Felix}, -doi = {10.1117/12.892762}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Krist, Hook, Stoehr - 2011 - 20 years of Hubble Space Telescope optical modeling using Tiny Tim.pdf:pdf}, -isbn = {9780819487377}, -issn = {0277786X}, -journal = {Optical Modeling and Performance Predictions V}, -keywords = {hubble space telescope,point spread function}, -number = {2004}, -pages = {81270J}, -title = {{20 years of Hubble Space Telescope optical modeling using Tiny Tim}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.892762}, -volume = {8127}, -year = {2011} -} -@article{Jacobs2019, -abstract = {We search Dark Energy Survey (DES) Year 3 imaging data for galaxy-galaxy strong gravitational lenses using convolutional neural networks. We generate 250 000 simulated lenses at redshifts > 0.8 from which we create a data set for training the neural networks with realistic seeing, sky and shot noise. Using the simulations as a guide, we build a catalogue of 1.1 million DES sources with 1.8 < g − i < 5, 0.6 < g − r < 3, r mag > 19, g mag > 20, and i mag > 18.2. We train two ensembles of neural networks on training sets consisting of simulated lenses, simulated non-lenses, and real sources. We use the neural networks to score images of each of the sources in our catalogue with a value from 0 to 1, and select those with scores greater than a chosen threshold for visual inspection, resulting in a candidate set of 7301 galaxies. During visual inspection, we rate 84 as 'probably' or 'definitely' lenses. Four of these are previously known lenses or lens candidates. We inspect a further 9428 candidates with a different score threshold, and identify four new candidates. We present 84 new strong lens candidates, selected after a few hours of visual inspection by astronomers. This catalogue contains a comparable number of high-redshift lenses to that predicted by simulations. Based on simulations, we estimate our sample to contain most discoverable lenses in this imaging and at this redshift range.}, -archivePrefix = {arXiv}, -arxivId = {1811.03786}, -author = {Jacobs, C. and Collett, T. and Glazebrook, K. and McCarthy, C. and Qin, A. K. and Abbott, T. M.C. and Abdalla, F. B. and Annis, J. and Avila, S. and Bechtol, K. and Bertin, E. and Brooks, D. and Buckley-Geer, E. and Burke, D. L. and {Carnero Rosell}, A. and {Carrasco Kind}, M. and Carretero, J. and {Da Costa}, L. N. and Davis, C. and {De Vicente}, J. and Desai, S. and Diehl, H. T. and Doel, P. and Eifler, T. F. and Flaugher, B. and Frieman, J. and Garc{\'{i}}a-Bellido, J. and Gaztanaga, E. and Gerdes, D. W. and Goldstein, D. A. and Gruen, D. and Gruendl, R. A. and Gschwend, J. and Gutierrez, G. and Hartley, W. G. and Hollowood, D. L. and Honscheid, K. and Hoyle, B. and James, D. J. and Kuehn, K. and Kuropatkin, N. and Lahav, O. and Li, T. S. and Lima, M. and Lin, H. and Maia, M. A.G. and Martini, P. and Miller, C. J. and Miquel, R. and Nord, B. and Plazas, A. A. and Sanchez, E. and Scarpine, V. and Schubnell, M. and Serrano, S. and Sevilla-Noarbe, I. and Smith, M. and Soares-Santos, M. and Sobreira, F. and Suchyta, E. and Swanson, M. E.C. and Tarle, G. and Vikram, V. and Walker, A. R. and Zhang, Y. and Zuntz, J.}, -doi = {10.1093/mnras/stz272}, -eprint = {1811.03786}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Jacbos2019SLDES.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Gravitational lensing: strong,Methods: statistical}, -number = {4}, -pages = {5330--5349}, -title = {{Finding high-redshift strong lenses in DES using convolutional neural networks}}, -volume = {484}, -year = {2019} -} -@article{Peterson2004, -abstract = {We present improved black hole masses for 35 active galactic nuclei (AGNs) based on a complete and consistent reanalysis of broad emission-line reverberation-mapping data. From objects with multiple line measurements, we find that the highest precision measure of the virial product is obtained by using the cross-correlation function centroid (as opposed to the cross-correlation function peak) for the time delay and the line dispersion (as opposed to full width half maximum) for the line width and by measuring the line width in the variable part of the spectrum. Accurate line-width measurement depends critically on avoiding contaminating features, in particular the narrow components of the emission lines. We find that the precision (or random component of the error) of reverberation-based black hole mass measurements is typically around 30%, comparable to the precision attained in measurement of black hole masses in quiescent galaxies by gas or stellar dynamical methods. Based on results presented in a companion paper by Onken et al., we provide a zero-point calibration for the reverberation-based black hole mass scale by using the relationship between black hole mass and host-galaxy bulge velocity dispersion. The scatter around this relationship implies that the typical systematic uncertainties in reverberation-based black hole masses are smaller than a factor of three. We present a preliminary version of a mass-luminosity relationship that is much better defined than any previous attempt. Scatter about the mass-luminosity relationship for these AGNs appears to be real and could be correlated with either Eddington ratio or object inclination.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407299}, -author = {Peterson, B. M. and Ferrarese, L. and Gilbert, K. M. and Kaspi, S. and Malkan, M. A. and Maoz, D. and Merritt, D. and Netzer, H. and Onken, C. A. and Pogge, R. W. and Vestergaard, M. and Wandel, A.}, -doi = {10.1086/423269}, -eprint = {0407299}, -isbn = {0407299v114}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Seyfert — quasars,Subject heading gs,active — galaxies,emission lines Online material,galaxies,machine-readable tables,nuclei — galaxies}, -month = {oct}, -number = {2}, -pages = {682--699}, -primaryClass = {astro-ph}, -title = {{Central Masses and Broad‐Line Region Sizes of Active Galactic Nuclei. II. A Homogeneous Analysis of a Large Reverberation‐Mapping Database}}, -url = {http://arxiv.org/abs/astro-ph/0407299%0Ahttp://dx.doi.org/10.1086/423269}, -volume = {613}, -year = {2004} -} -@article{Rocha2013, -abstract = {We use cosmological simulations to study the effects of self-interacting dark matter (SIDM) on the density profiles and substructure counts of dark-matter haloes from the scales of spiral galaxies to galaxy clusters, focusing explicitly on models with cross-sections over dark-matter particle mass $\sigma$/m = 1 and 0.1 cm2 g-1. Our simulations rely on a new SIDM N-body algorithm that is derived self-consistently from the Boltzmann equation and that reproduces analytic expectations in controlled numerical experiments. We find that well-resolved SIDM haloes have constant-density cores, with significantly lower central densities than their cold dark matter (CDM) counterparts. In contrast, the subhalo content of SIDM haloes is only modestly reduced compared to CDM, with the suppression greatest for large hosts and small halo-centric distances. Moreover, the large-scale clustering and halo circular velocity functions in SIDM are effectively identical to CDM, meaning that all of the large-scale successes of CDM are equally well matched by SIDM. From our largest cross-section runs, we are able to extract scaling relations for core sizes and central densities over a range of halo sizes and find a strong correlation between the core radius of an SIDM halo and the NFW scale radius of its CDM counterpart. We construct a simple analytic model, based on CDM scaling relations, that captures all aspects of the scaling relations for SIDM haloes. Our results show that halo core densities in $\sigma$/m = 1 cm2 g-1 models are too low to match observations of galaxy clusters, low surface brightness spirals (LSBs) and dwarf spheroidal galaxies. However, SIDM with $\sigma$/m ≃ 0.1 cm2 g-1 appears capable of reproducing reported core sizes and central densities of dwarfs, LSBs and galaxy clusters without the need for velocity dependence. Higher resolution simulations over a wider range of masses will be required to confirm this expectation. We discuss constraints arising from the Bullet cluster observations, measurements of dark-matter density on small scales and subhalo survival requirements, and show that SIDM models with $\sigma$/m ≃ 0.1 cm2 g-1 ≃ 0.2 barn GeV-1 are consistent with all observational constraints. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1208.3025}, -author = {Rocha, Miguel and Peter, Annika H.G. and Bullock, James S. and Kaplinghat, Manoj and Garrison-kimmel, Shea and O{\~{n}}orbe, Jose and Moustakas, Leonidas A.}, -doi = {10.1093/mnras/sts514}, -eprint = {1208.3025}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Methods: numerical}, -number = {1}, -pages = {81--104}, -title = {{Cosmological simulations with self-interacting dark matter - I. Constant-density cores and substructure}}, -url = {http://arxiv.org/abs/1208.3025}, -volume = {430}, -year = {2013} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned r- and g-band images from a sample of 45 508 galaxies from Sloan Digital Sky Survey Data Release 9 in the redshift range 0.06≤z≤0.1 and in the mass range 1010.0M⊙ {\textless}M* {\textless} 1011.4M⊙.We derive surface brightness profiles to a depth of almost $\mu$r ̃ 32 mag arcsec-2. We find that the ellipticity of the stellar halo is a function of galaxy stellar mass and that the haloes of high-concentration galaxies are more elliptical than those of low-concentration galaxies. Where the g - r colour of the stellar halo can be measured, we find that the stellar light is always bluer than in the main galaxy. The colour of the stellar halo is redder for more massive galaxies. We further demonstrate that the full two-dimensional surface intensity distribution of our galaxy stacks can only be fit through multicomponent S{\'{e}}rsic models. Using the fraction of light in the outer component of the models as a proxy for the fraction of accreted stellar light, we show that this fraction is a function of stellar mass and galaxy type. The fraction of accreted stellar light rises from 30 to 70 per cent and from 2 to 25 per cent for high- and low-concentration galaxies, respectively, over the mass range 1010.0-1011.4M⊙. {\textcopyright}2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1404.2123}, -author = {D'Souza, Richard and Kauffman, Guinevere and Wang, Jing and Vegetti, Simona}, -doi = {10.1093/mnras/stu1194}, -eprint = {1404.2123}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: halo,Galaxy: structure}, -number = {2}, -pages = {1433--1450}, -title = {{Parametrizing the stellar haloes of galaxies}}, -volume = {443}, -year = {2014} -} -@article{VandeSande2016, -abstract = {Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h3 ({\$\sim${}}skewness) and h4 ({\$\sim${}}kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using 2D integral field data from the SAMI Galaxy Survey. A proxy for the spin parameter ({\$}\backslashlambda{\_}{\{}R{\_}e{\}}{\$}) and ellipticity ({\$}\backslashepsilon{\_}e{\$}) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h3 versus {\$}V/\backslashsigma{\$} anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h3 and {\$}V/\backslashsigma{\$}. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h3 versus {\$}V/\backslashsigma{\$} signatures. We identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar {\$}\backslashlambda{\_}{\{}R{\_}e{\}}-\backslashepsilon{\_}e{\$} values can show distinctly different h3-{\$}V/\backslashsigma{\$} signatures. Class 5 objects are previously unidentified fast rotators that show a weak h3 versus {\$}V/\backslashsigma{\$} anti-correlation. These objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h3 versus {\$}V/\backslashsigma{\$} as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.}, -archivePrefix = {arXiv}, -arxivId = {1611.07039}, -author = {van de Sande, Jesse and Bland-Hawthorn, Joss and Fogarty, Lisa M R and Cortese, Luca and D'Eugenio, Francesco and Croom, Scott M and Scott, Nicholas and Allen, James T and Brough, Sarah and Bryant, Julia J and Cecil, Gerald and Colless, Matthew and Couch, Warrick J and Davies, Roger and Elahi, Pascal J and Foster, Caroline and Goldstein, Gregory and Goodwin, Michael and Groves, Brent and Ho, I-Ting and Jeong, Hyunjin and Jones, D Heath and Konstantopoulos, Iraklis S and Lawrence, Jon S and Leslie, Sarah K and L{\'{o}}pez-S{\'{a}}nchez, {\'{A}}ngel R and McDermid, Richard M and McElroy, Rebecca and Medling, Anne M and Oh, Sree and Owers, Matt S and Richards, Samuel N and Schaefer, Adam L and Sharp, Rob and Sweet, Sarah M and Taranu, Dan and Tonini, Chiara and Walcher, C Jakob and Yi, Sukyoung K}, -doi = {10.3847/1538-4357/835/1/104}, -eprint = {1611.07039}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cosmology,dynamics,evolution,formation,galaxies,kinematics and,observations,stellar content,structure}, -number = {1}, -pages = {104}, -title = {{the Sami Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics}}, -url = {http://arxiv.org/abs/1611.07039%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/835/1/104}, -volume = {835}, -year = {2017} -} -@article{Bingham2019, -abstract = {Pyro is a probabilistic programming language built on Python as a platform for developing advanced probabilistic models in AI research. To scale to large data sets and high-dimensional models, Pyro uses stochastic variational inference algorithms and probability distributions built on top of PyTorch, a modern GPU-accelerated deep learning framework. To accommodate complex or model-specific algorithmic behavior, Pyro leverages Poutine, a library of composable building blocks for modifying the behavior of probabilistic programs.}, -archivePrefix = {arXiv}, -arxivId = {1810.09538}, -author = {Bingham, Eli and Chen, Jonathan P and Jankowiak, Martin and Obermeyer, F and Pradhan, Neeraj and Karaletsos, Theofanis and Singh, Rohit and Szerlip, Paul and Horsfall, Paul and Goodman, Noah D}, -eprint = {1810.09538}, -issn = {15337928}, -journal = {Journal of Machine Learning Research}, -keywords = {Approximate Bayesian inference,Deep learning,Generative models,Graphical models,Probabilistic programming}, -number = {Xxxx}, -pages = {0--5}, -title = {{Pyro: Deep universal probabilistic programming}}, -volume = {20}, -year = {2019} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10% of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1138?key=crossref.6ebb2a01dc7b45f1fa5c66089a37542b}, -volume = {709}, -year = {2010} -} -@article{Keeton1997, -abstract = {Galaxies modeled as singular isothermal ellipsoids with an axis ratio distribution similar to the observed axis ratio distribution of E and S0 galaxies are statistically consistent with both the observed numbers of two-image and four-image lenses and the inferred ellipticities of individual lenses. However, no four-image lens is well fit by the model (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 20{\$}), the axis ratio of the model can be significantly different from that of the observed lens galaxy, and the major axes of the model and the galaxy may be slightly misaligned. We found that models with a second, independent, external shear axis could fit the data well (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 1{\$}), while adding the same number of extra parameters to the radial mass distribution does not produce such a dramatic improvement in the fit. An independent shear axis can be produced by misalignments between the luminous galaxy and its dark matter halo, or by external shear perturbations due to galaxies and clusters correlated with the primary lens or along the line of sight. We estimate that the external shear perturbations have no significant effect on the expected numbers of two-image and four-image lenses, but that they can be important perturbations in individual lens models. However, the amplitudes of the external shears required to produce the good fits are larger than our estimates for typical external shear perturbations (10-15{\%} shear instead of 1-3{\%} shear) suggesting that the origin of the extra angular structure must be intrinsic to the primary lens galaxy in most cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610163}, -author = {Keeton, C R and Kochanek, C S and Seljak, U}, -doi = {10.1086/304172}, -eprint = {9610163}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Elliptical and Lenticular,cD,cosmology: theory}, -number = {2}, -pages = {604--620}, -primaryClass = {astro-ph}, -title = {{Shear and Ellipticity in Gravitational Lenses}}, -url = {http://arxiv.org/abs/astro-ph/9610163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/304172}, -volume = {482}, -year = {1997} -} -@article{Bolton2006, -abstract = {The Sloan Lens ACS (SLACS) Survey is an efficient Hubble Space Telescope (HST) Snapshot imaging survey for new galaxy-scale strong gravitational lenses. The targeted lens candidates are selected spectroscopically from the Sloan Digital Sky Survey (SDSS) database of galaxy spectra for having multiple nebular emission lines at a redshift significantly higher than that of the SDSS target galaxy. The SLACS survey is optimized to detect bright early-type lens galaxies with faint lensed sources in order to increase the sample of known gravitational lenses suitable for detailed lensing, photometric, and dynamical modeling. In this paper, the first in a series on the current results of our HST Cycle 13 imaging survey, we present a catalog of 19 newly discovered gravitational lenses, along with nine other observed candidate systems that are either possible lenses, nonlenses, or nondetections. The survey efficiency is thus ≥68%. We also present Gemini 8 m and Magellan 6.5 m integral-field spectroscopic data for nine of the SLACS targets, which further support the lensing interpretation. A new method for the effective subtraction of foreground galaxy images to reveal faint background features is presented. We show that the SLACS lens galaxies have colors and ellipticities typical of the spectroscopic parent sample from which they are drawn (SDSS luminous red galaxies and quiescent MAIN sample galaxies), but are somewhat brighter and more centrally concentrated. Several explanations for the latter bias are suggested. The SLACS survey provides the first statistically significant and homogeneously selected sample of bright early-type lens galaxies, furnishing a powerful probe of the structure of early-type galaxies within the half-light radius. The high confirmation rate of lenses in the SLACS survey suggests consideration of spectroscopic lens discovery as an explicit science goal of future spectroscopic galaxy surveys. {\textcopyright} 2006. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511453}, -author = {Bolton, Adam S. and Burles, Scott and Koopmans, Leon V. E. and Treu, Tommaso and Moustakas, Leonidas A.}, -doi = {10.1086/498884}, -eprint = {0511453}, -issn = {0004-637X}, -journal = {ApJ}, -number = {2}, -pages = {703--724}, -primaryClass = {astro-ph}, -title = {{The Sloan Lens ACS Survey. I. A Large Spectroscopically Selected Sample of Massive Early‐Type Lens Galaxies}}, -url = {http://stacks.iop.org/0004-637X/638/i=2/a=703}, -volume = {638}, -year = {2006} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of {\$\sim${}}3692 galaxies, with -18.5 {\textless}= M{\_}g {\textless} -22.0 mag and redshift 0.01 {\textless}= z {\textless} 0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of {\$\sim${}}2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined ({\textgreater}60 degrees) systems, we find the following results. (1) The optical r-band fraction (f{\_}opt-r) of barred galaxies is {\$\sim${}}48{\%}-52{\%}. (2) When galaxies are separated according to normalized half light radius (r{\_}e/R{\_}24), a remarkable result is seen: f{\_}opt-r rises sharply, from {\$\sim${}}40{\%} in galaxies that have small r{\_}e/R{\_}24 and visually appear to host prominent bulges, to {\$\sim${}}70{\%} for galaxies that have large r{\_}e/R{\_}24 and appear disk-dominated. (3) f{\_}opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that {\$\sim${}}20{\%} of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity {\textgreater}=0.4) and large enough (semi-major axis {\textgreater}=1.5 kpc) to be reliably characterized via ellipse-fitting out to z{\$\sim${}}0.8, we get an optical r-band fraction for strong bars f{\_}opt-s of {\$\sim${}}34{\%}. This value is higher only by a modest factor of 1.4, compared to the value of {\$\sim${}}24{\%}+-4{\%} reported at z{\$\sim${}}0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z{\$\sim${}}0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Johnson, Crockett}, -doi = {10.2307/3616804}, -eprint = {0802.3961}, -issn = {00255572}, -journal = {The Mathematical Gazette}, -keywords = {Astrophysics}, -number = {407}, -pages = {17}, -title = {{A Construction for a Regular Heptagon}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {59}, -year = {1975} -} -@article{Mcconnell2011, -abstract = {Observational work conducted over the past few decades indicates that all massive galaxies have supermassive black holes at their centres. Although the luminosities and brightness fluctuations of quasars in the early Universe suggest that some were powered by black holes with masses greater than 10 billion solar masses, the remnants of these objects have not been found in the nearby Universe. The giant elliptical galaxy Messier 87 hosts the hitherto most massive known black hole, which has a mass of 6.3 billion solar masses. Here we report that NGC 3842, the brightest galaxy in a cluster at a distance from Earth of 98 megaparsecs, has a central black hole with a mass of 9.7 billion solar masses, and that a black hole of comparable or greater mass is present in NGC 4889, the brightest galaxy in the Coma cluster (at a distance of 103 megaparsecs). These two black holes are significantly more massive than predicted by linearly extrapolating the widely used correlations between black-hole mass and the stellar velocity dispersion or bulge luminosity of the host galaxy. Although these correlations remain useful for predicting black-hole masses in less massive elliptical galaxies, our measurements suggest that different evolutionary processes influence the growth of the largest galaxies and their black holes. {\textcopyright} 2011 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1112.1078}, -author = {Mcconnell, Nicholas J. and Ma, Chung Pei and Gebhardt, Karl and Wright, Shelley A. and Murphy, Jeremy D. and Lauer, Tod R. and Graham, James R. and Richstone, Douglas O.}, -doi = {10.1038/nature10636}, -eprint = {1112.1078}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/McConnel2011x2MAssiveBHs.pdf:pdf}, -issn = {00280836}, -journal = {Nature}, -number = {7376}, -pages = {215--218}, -title = {{Two ten-billion-solar-mass black holes at the centres of giant elliptical galaxies}}, -volume = {480}, -year = {2011} -} -@article{Schaller2015b, -abstract = {We use the 'Evolution and Assembly of GaLaxies and their Environments' (eagle) suite of hydrodynamical cosmological simulations to measure offsets between the centres of stellar and dark matter components of galaxies. We find that the vast majority (>95 per cent) of the simulated galaxies display an offset smaller than the gravitational softening length of the simulations (Plummer-equivalent $\epsilon$= 700 pc), both for field galaxies and satellites in clusters and groups. We also find no systematic trailing or leading of the dark matter along a galaxy's direction of motion. The offsets are consistent with being randomly drawn from a Maxwellian distribution with $\sigma$≤ 196pc. Since astrophysical effects produce no feasible analogues for the 1.62+0.47-0.49kpc offset recently observed in Abell 3827, the observational result is in tension with the collisionless cold dark matter model assumed in our simulations.}, -archivePrefix = {arXiv}, -arxivId = {1505.05470}, -author = {Schaller, Matthieu and Robertson, Andrew and Massey, Richard and Bower, Richard G. and Eke, Vincent R.}, -doi = {10.1093/mnrasl/slv104}, -eprint = {1505.05470}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Astroparticle physics,Cosmology: theory,Dark matter}, -month = {oct}, -number = {1}, -pages = {L58--L62}, -title = {{The offsets between galaxies and their dark matter in $\Lambda$ cold dark matter}}, -volume = {453}, -year = {2015} -} -@article{Genel2017, -abstract = {We analyse scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, star formation rate and redshift are reproduced, and a quantitative comparison of projected r band sizes at 0 ≲ z ≲ 2 shows agreement to much better than 0.25 dex. We follow populations of z = 0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M*, z = 0 ≳ 109.5 M⊙, the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z = 0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M*, M*, z = 0 ≳ 109.5 M⊙ experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies withM*, z = 0 ≳ 1011 M⊙, the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z = 0.}, -archivePrefix = {arXiv}, -arxivId = {1707.05327}, -author = {Genel, Shy and Nelson, Dylan and Pillepich, Annalisa and Springel, Volker and Pakmor, R{\"{u}}diger and Weinberger, Rainer and Hernquist, Lars and Naiman, Jill and Vogelsberger, Mark and Marinacci, Federico and Torrey, Paul}, -doi = {10.1093/mnras/stx3078}, -eprint = {1707.05327}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Genel et al. - 2018 - The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Galaxies: structure,Methods: numerical}, -number = {3}, -pages = {3976--3996}, -title = {{The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation}}, -url = {http://arxiv.org/abs/1707.05327}, -volume = {474}, -year = {2018} -} -@article{Perlmutter1997, -abstract = {We have developed a technique to systematically discover and study high-redshift supernovae that can be used to measure the cosmological parameters. We report here results based on the initial seven of more than 28 supernovae discovered to date in the high-redshift supernova search of the Supernova Cosmology Project. We find an observational dispersion in peak magnitudes of $\sigma$ MB = 0.27; this dispersion narrows to $\sigma$ MB.corr = 0.19 after "correcting" the magnitudes using the light-curve "widthluminosity" relation found for nearby (z ≤ 0.1) Type la supernovae from the Cal{\'{a}}n/Tololo survey (Hamuy et al). Comparing light-curve width-corrected magnitudes as a function of redshift of our distant (z = 0.35-0.46) supernovae to those of nearby Type la supernovae yields a global measurement of the mass density, $\Omega$ M = 0.88 -0.60 +0.69 for a $\Lambda$ = 0 cosmology. For a spatially flat universe (i.e., $\Omega$ M + $\Omega$ $\Lambda$ = 1), we find $\Omega$ M = 0.94 -0.28 +0.34 or equivalently, a measurement of the cosmological constant, $\Omega$ $\Lambda$ = 0.06 -0.34 +0.28 ( {\textless} 0.51 at the 95{\%} confidence level). For the more general Friedmann-Lema{\^{i}}tre cosmologies with independent $\Omega$ M and $\Omega$ $\Lambda$ , the results are presented as a confidence region on the $\Omega$ M -$\Omega$ $\Lambda$ plane. This region does not correspond to a unique value of the deceleration parameter q 0 . We present analyses and checks for statistical and systematic errors and also show that our results do not depend on the specifics of the width-luminosity correction. The results for $\Omega$ $\Lambda$ -versus-$\Omega$ M are inconsistent with $\Lambda$-dominated, low-density, flat cosmologies that have been proposed to reconcile the ages of globular cluster stars with higher Hubble constant values. {\textcopyright}1997. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9608192}, -author = {Perlmutter, S and Gabi, S and Goldhaber, G and Goobar, A and Groom, D E and Hook, I M and Kim, A G and Kim, M Y and Lee, J C and Pain, R and Pennypacker, C R and Small, I A and Ellis, R S and McMahon, R G and Boyle, B J and Bunclark, P S and Carter, D and Irwin, M J and Glazebrook, K and Newberg, H J M and Filippenko, A V and Matheson, T and Dopita, M and Couch, W J}, -doi = {10.1086/304265}, -eprint = {9608192}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {3-Pronto,Cosmology,Dark Energy}, -month = {jul}, -number = {2}, -pages = {565--581}, -primaryClass = {astro-ph}, -title = {{Measurements of the Cosmological Parameters $\Omega$ and $\Lambda$ from the First Seven Supernovae at {\textless}i{\textgreater}z{\textless}/i{\textgreater} ≥ 0.35}}, -url = {http://stacks.iop.org/0004-637X/483/i=2/a=565}, -volume = {483}, -year = {1997} -} -@article{Pillepich2017, -abstract = {We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multimode feedback. In this paper, we give a comprehensive description of the physical and numerical advances that form the core of the IllustrisTNG (The Next Generation) framework.We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black-hole-driven kinetic feedback at low accretion rates, magnetohydrodynamics and improvements to the numerical scheme. Using a suite of (25Mpc h-1)3 cosmological boxes, we assess the outcome of the new model at our fiducial resolution. The presence of a selfconsistently amplified magnetic field is shown to have an important impact on the stellar content of 1012M⊙ haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low-mass end of the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {1703.02970}, -author = {Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R{\"{u}}diger and Hernquist, Lars and Torrey, Paul and Vogelsberger, Mark and Weinberger, Rainer and Marinacci, Federico}, -doi = {10.1093/mnras/stx2656}, -eprint = {1703.02970}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pillepich et al. - 2018 - Simulating galaxy formation with the IllustrisTNG model.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {4077--4106}, -title = {{Simulating galaxy formation with the IllustrisTNG model}}, -url = {http://arxiv.org/abs/1703.02970%0Ahttp://dx.doi.org/10.1093/mnras/stx2656}, -volume = {473}, -year = {2018} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and S{\'{e}}rsic index distributions obtained from two-dimensional structural fits to 40, 000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of S{\'{e}}rsic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. {\textcopyright}2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, Jenny E and Leauthaud, Alexie and Emsellem, Eric and Ge, J and Arag'on-Salamanca, A and Greco, J P and Lin, Y -T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -pages = {1--23}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -year = {2017} -} -@article{Chirivi2017, -abstract = {Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we aim to present the first attempt at modelling line-of-sight (LOS) mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We have focussed on the Hubble Frontier Field cluster MACS J0416.1-2403, and our multi-plane model reproduces the observed image positions with a rms offset of {\$\sim${}}0.′′53. Starting from this best-fitting model, we simulated a mock cluster that resembles MACS J0416.1-2403 in order to explore the effects of LOS structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms {\$\sim${}}0.′′3); accounting for LOS galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factor of the lensed multiple images are recovered within {\$\sim${}}10{\%} for {\$\sim${}}95{\%} of them, those {\$\sim${}}5{\%} that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models. In addition, LOS galaxies cannot explain the apparent discrepancy in the properties of massive sub-halos between MACS J0416.1-2403 and N-body simulated clusters. Since our model of MACS J0416.1-2403 with LOS galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities would be needed in future models of MACS J0416.1-2403.}, -archivePrefix = {arXiv}, -arxivId = {1706.07815}, -author = {Chiriv{\`{i}}, G and Suyu, S H and Grillo, C and Halkola, A and Balestra, I and Caminha, G B and Mercurio, A and Rosati, P}, -doi = {10.1051/0004-6361/201731433}, -eprint = {1706.07815}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Dark matter,Galaxies: clusters: general,Galaxies: clusters: individual: MACS J0416.1-2403,Gravitational lensing: strong}, -pages = {1--29}, -title = {{MACS J0416.1-2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters}}, -url = {http://arxiv.org/abs/1706.07815%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731433}, -volume = {614}, -year = {2018} -} -@article{Krist2004a, -author = {Krist, John and Hook, Richard and Tim, Tiny}, -journal = {Changes}, -number = {June}, -pages = {1--35}, -title = {{The Tiny Tim User ' s Guide}}, -url = {http://tinytim.stsci.edu/static/tinytim.pdf%7B%5C%25%7D5Cnpapers2://publication/uuid/994E8BF5-B9AC-489B-A26F-2AE8BC664FEE}, -year = {2004} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z > 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G.}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2006 - Breaking the hierarchy of galaxy formation(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, n = 10 cm −3 , results in strong expansion of the DM halo in galaxies with stellar masses in the range 10 7.5 ∼ {\textless}M star ∼ {\textless}10 9.5 M ⊙. We find that lower thresholds such as n = 0.1 (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e., ∼ {\textless}50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with n = 10 have gas fractions of ≃ 0.2 and variations of ≃ 0.1, while n = 0.1 simulations have order of magnitude lower gas fractions and hence do not expand the halo. Star formation rates are more variable for higher n, lower galaxy masses, and when star formation is measured on shorter time scales. Simulations with n = 10 have up to 0.4 dex higher scatter in specific star formation rates than simulations with n = 0.1. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with n = 0.1 and n = 1, but in reasonable agreement with n = 10. While the strong dependence of the halo response to n currently prevents a robust prediction for dark halo structure in CDM cosmologies, it is reassuring that different n result in testable predictions for the properties of gas and star formation, and thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625v1}, -author = {{Dutton 1⋆}, Aaron A and Macc{\`{i}}, Andrea V and Buck, Tobias and Dixon, Keri L and Blank, Marvin and Obreja, Aura}, -eprint = {1811.10625v1}, -keywords = {cosmology,formation-galaxies,kine-matics and dynamics-galaxies,numerical,structure-methods,theory-dark matter-galaxies}, -number = {November}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://popia.ft.uam.es/AMIGA}, -volume = {000}, -year = {2018} -} -@article{Goullaud2018, -abstract = {We present near-infrared observations of 35 of the most massive early-type galaxies in the local universe. The observations were made using the infrared channel of the Hubble Space Telescope Wide Field Camera 3 in the F110W (1.1 $\mu$m) filter. We measured surface brightness profiles and elliptical isophotal fit parameters from the nuclear regions out to a radius of $\sim$10 kpc in most cases. We find that 37% (13) of the galaxies in our sample have isophotal position angle rotations greater than 20 degrees over the radial range imaged by WFC3/IR, which is often due to the presence of neighbors or multiple nuclei. Most galaxies in our sample are significantly rounder near the center than in the outer regions. This sample contains six fast rotators and 28 slow rotators. We find that all fast rotators are either disky or show no measurable deviation from purely elliptical isophotes. Among slow rotators, significantly disky and boxy galaxies occur with nearly equal frequency. The galaxies in our sample often exhibit changing isophotal shapes, sometimes showing both significantly disky and boxy isophotes at different radii. The fact that parameters vary widely between galaxies and within individual galaxies is evidence that these massive galaxies have complicated formation histories, and some of them have experienced recent mergers and have not fully relaxed. These data demonstrate the value of high spatial resolution IR imaging of galaxies and provide measurements necessary for determining stellar masses, dynamics, and black hole masses in high mass galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1801.08245}, -author = {Goullaud, Charles F. and Jensen, Joseph B. and Blakeslee, John P. and Ma, Chung-Pei and Greene, Jenny E. and Thomas, Jens}, -doi = {10.3847/1538-4357/aab1f3}, -eprint = {1801.08245}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Goullaud et al. - 2018 - The MASSIVE Survey. IX. Photometric Analysis of 35 High-mass Early-type Galaxies with HST WFC3IR(2).pdf:pdf}, -issn = {1538-4357}, -journal = {ApJ}, -keywords = {cd,elliptical and lenticular,galaxies,photometry,structure}, -number = {1}, -pages = {11}, -title = {{The MASSIVE Survey. IX. Photometric Analysis of 35 High-mass Early-type Galaxies with HST WFC3/IR}}, -url = {http://arxiv.org/abs/1801.08245%0Ahttp://dx.doi.org/10.3847/1538-4357/aab1f3}, -volume = {856}, -year = {2018} -} -@article{Sales2012a, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Murray2013, -abstract = {A multi-level clocking scheme has been developed to improve the parallel CTE of four-phase CCDs by suppressing the effects of traps located in the transport channel under barrier phases by inverting one of these phases throughout the transfer sequence. In parallel it was apparent that persistence following optical overload in Euclid VIS detectors would lead to undesirable signal released in subsequent rows and frames and that a suitable scheme for flushing this signal would be required. With care, the negatively biased electrodes during the multi-level transfer sequence can be made to pin the entire surface, row-by-row, and annihilate the problematic charges. This process can also be extended for use during integration to significantly reduce the unusable area of the detector, as per the clocked anti-blooming techniques developed many years ago; however, with the four-phase electrodes architecture of modern CCDs, we can take precautionary measures to avoid the problem of charge pumping and clock induced charge within the science frames. Clock induced charge is not all bad! We also propose the use of on-orbit trap-pumping for Euclid VIS to provide calibration input to ground based correction algorithms and as such a uniform, low noise background is require. Clock induced charge can be manipulated to provide a very suitable, low signal and noise background to the imaging array. Here we describe and present results of multi-level parallel clocking schemes for use in four-phase CCDs that could improve performance of high precision astronomy applications such as Euclid VIS. ? 2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Holland, Andrew D and Stefanov, Konstantin D and Gow, Jason P D and MacCormick, Calum and Dryer, Ben J and Allanwood, Edgar A H}, -doi = {10.1117/12.2024839}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {Blooming,CAB,CCD,CIC,CTE,Euclid VIS,Mu,[BFW}, -pages = {88600K}, -title = {{Multi-level parallel clocking of CCDs for: improving charge transfer efficiency, clearing persistence, clocked anti-blooming, and generating low-noise backgrounds for pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024839}, -volume = {8860}, -year = {2013} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio M/L and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R,z) and characterized by the classic anisotropy parameter beta{\_}z=1-sigma{\_}z{\^{}}2/sigma{\_}R{\^{}}2. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters (beta{\_}z and the inclination) the models generally provide remarkably good descriptions of the shape of the first (V) and second (V{\_}rms=sqrt{\{}V{\^{}}2+sigma{\^{}}2{\}}) velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the simple dynamical structure of these objects. With the observationally-motivated assumption that beta{\_}z{\textgreater}0, the method is able to recover the inclination. The technique can be used to determine the dynamical mass-to-light ratios and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modeling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy, and multiple kinematic components.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Wood2014, -abstract = {The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D. and Hall, D. J. and Murray, N. J. and Gow, J. P.D. and Holland, A. and Turner, P. and Burt, D.}, -doi = {10.1088/1748-0221/9/12/C12028}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wood et al. - 2014 - Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap pumping techn(2).pdf:pdf}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv, visible and ir photons (s}, -number = {12}, -pages = {C12028----C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{Deason2011, -abstract = {(Abridged) We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the GIMIC suite of simulations. GIMIC consists of re-simulations of 5 cosmologically representative regions from the Millennium simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r {\$\sim${}} 0.1r200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r {\$\sim${}} r200). Misalignments of {\textgreater}45 deg are seen in {\$\sim${}} 30{\%} of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20{\%} of the satellite systems with ten bright galaxies within r200 exhibit a polar spatial alignment with respect to the galaxy an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction ({\$\sim${}}10{\%}) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z=0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation the memory of their accretion history can remain intact to z=0.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A J and Mccarthy, I G and Font, A S and Evans, N W and Frenk, C S and Belokurov, V and Libeskind, N I and Crain, R A and Theuns, T}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Morishita2018a, -abstract = {Observations have revealed log M*/Msun {\textgreater}11 galaxies that were already dead when the universe was only {\$\sim${}}2Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interests. In this paper, we study star formation and metallicity enrichment histories of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple HST surveys allows robust determination of their SEDs. Our new SED modeling provides mass accumulation/stellar metallicity enrichment histories of those galaxies over the past {\$\sim${}}3Gyr, with no functional assumptions on their star formation histories. We find that most of our massive galaxies have formed {\textgreater}50{\%} of their extant masses by {\$\sim${}}1.5Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Most of our galaxies already have stellar metallicities compatible with, or even higher than, those of local early-type galaxies, with a median value of log Z*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. By using reconstructed star formation history, we reveal their rapid metallicity enrichment history from z{\$\sim${}}5.5 to 2.2 at a rate of {\$\sim${}}0.2dex/Gyr in logZ*/Zsun. The inferred metallicities are on average {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies at the time of formation. This supports a view where quenched galaxies continue to form stars at low-level until recently, rather than abrupt termination of star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -eprint = {1812.06980}, -keywords = {evolution,formation,galaxies,star formation}, -title = {{Massive Dead Galaxies at z{\$\sim${}}2 with HST Grism Spectroscopy I. Star Formation and Metallicity Enrichment Histories}}, -url = {http://arxiv.org/abs/1812.06980}, -year = {2018} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ {\textgreater} 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright}2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -volume = {786}, -year = {2014} -} -@article{Waczynski2001, -abstract = {We examine proton-damaged charge-coupled devices (CCDs) and compare the charge transfer efficiency (CTE) degradation using extended pixel edge response, first pixel response, and 55 Fe X-ray measurements. CTEs measured on Marconi and Fairchild imaging sensors CCDs degrade similarly at all signal levels, though some of the Fairchild CCDs had a supplementary buried channel.}, -author = {Waczynski, Augustyn and Polidan, Elizabeth J. and Marshall, Paul W. and Reed, Robert A. and Johnson, Scott D. and Hill, Robert J. and Delo, Gregory S. and Wassell, Edward J. and Cheng, Edward S.}, -doi = {10.1109/23.983134}, -isbn = {0018-9499 VO - 48}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {CTE,CTE noise,EEPR,EEV,FPR,Minichannel,Proton radiation damage,Radiation testing,SBC,Scientific CCD,WFC3}, -month = {dec}, -number = {6 I}, -pages = {1807--1814}, -title = {{A comparison of charge transfer efficiency measurement techniques on proton damaged n-channel CCDs for the hubble space telescope wide-field camera 3}}, -volume = {48}, -year = {2001} -} -@article{Cautun2015a, -abstract = {We investigate the angular and kinematic distributions of satellite galaxies around a large sample of bright isolated primaries in the spectroscopic and photometric catalogues of the Sloan Digital Sky Survey (SDSS). We detect significant anisotropy in the spatial distribution of satellites. To test whether this anisotropy could be related to the rotating discs of satellites recently found by Ibata et al. in a sample of SDSS galaxies, we repeat and extend their analysis. Ibata et al. found an excess of satellites on opposite sides of their primaries having anticorrelated radial velocities. We find that this excess is sensitive to small changes in the sample selection criteria which can greatly reduce its significance. In addition, we find no evidence for correspondingly correlated velocities for satellites observed on the same side of their primaries, which would be expected for rotating discs of satellites. We conclude that the detection of rotating planes of satellites in the observational sample of Ibata et al. is not robust to changes in the sample selection criteria. We compare our data to the $\Lambda$ cold dark matter Millennium simulations populated with galaxies according to the semi-analytic model of Guo et al. We find excellent agreement with the spatial distribution of satellites in the SDSS data and the lack of a strong signal from coherent rotation.}, -archivePrefix = {arXiv}, -arxivId = {1410.7778}, -author = {Cautun, Marius and Wang, Wenting and Frenk, Carlos S. and Sawala, Till}, -doi = {10.1093/mnras/stv490}, -eprint = {1410.7778}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cautun et al. - 2015 - A new spin on discs of satellite galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {3}, -pages = {2576--2587}, -title = {{A new spin on discs of satellite galaxies}}, -volume = {449}, -year = {2015} -} -@article{Planck2015, -abstract = {The objective of this case study was to obtain some first-hand information about the functional consequences of a cosmetic tongue split operation for speech and tongue motility. One male patient who had performed the operation on himself was interviewed and underwent a tongue motility assessment, as well as an ultrasound examination. Tongue motility was mildly reduced as a result of tissue scarring. Speech was rated to be fully intelligible and highly acceptable by 4 raters, although 2 raters noticed slight distortions of the sibilants /s/ and /z/. The 3-dimensional ultrasound demonstrated that the synergy of the 2 sides of the tongue was preserved. A notably deep posterior genioglossus furrow indicated compensation for the reduced length of the tongue blade. It is concluded that the tongue split procedure did not significantly affect the participant's speech intelligibility and tongue motility.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {ونهال, أريج}, -doi = {10.1007/s13398-014-0173-7.2}, -eprint = {arXiv:1011.1669v3}, -isbn = {9780874216561}, -issn = {0717-6163}, -journal = {Uma {\'{e}}tica para quantos?}, -keywords = {12,2007,3,Adolescence,Adolescencia,Adolescent,Adolescent Behavior,Adolescent Behavior: psychology,Adult,Agresiones al cuerpo,Attachment to the body,Attaque au corps,Autolesiones deliberadas,Automutilation d{\'{e}}lib{\'{e}}r{\'{e}}e,Body Piercing,Body Piercing: psychology,Body Piercing: statistics & numerical data,Body image,CUERPO,Chile,Chile: epidemiology,Cornway,Corporate Finance,Cosmetic Techniques,Deliberate self-harm,Epidemiologic Methods,Female,Humans,Image corporelle,Imagen corporal,Industrial Organization,J.,JUVENTUD,Lumb,MODIFICACIONES CORPORALES,Male,Masood,Motivation,Movement,Public,R.,Risk-Taking,S.,S.K.,Self Mutilation,Self Mutilation: physiopathology,Self Mutilation: ultrasonography,Sex Distribution,Skan,Speech Articulation Tests,Speech Intelligibility,Tattooing,Tattooing: psychology,Tattooing: statistics & numerical data,Tongue,Tongue: injuries,Tongue: physiopathology,Tongue: ultrasonography,advantages,aesthetics,and e-banking,and on cor-,anomaly detection,as none were found,authentication,autoinjury and health,body,business model,candidate,classification,collaboration,competition,complications did not,complications from inserting a,constituci{\'{o}}n del yo,control postural- estabilizaci{\'{o}}n- v{\'{i}}as,corporal modifications,corps,credit access,credit financing,credit score,credit scoring,critical success factors,cuerpo,culturas juveniles,cultures juv{\'{e}}niles,customer satisfaction,customer scoring,data mining,decision tree,department of economics at,e-,e- banking,e-banking,e-commerce,e-payment,e-trading,electronic communication and computation,emergency,endogenous tie,epidural,esth{\'{e}}tique,est{\'{e}}tica,feature sim-,finance includes e-payment,financial fervices technology,financial services innovation,find any reports of,fintech,fintech analysis,fintech start-ups,functions,genetic programming,global fintech comparison,high resolution images,if neuraxial anes-,in practice,indonesia,information technology,ing with neuraxial anesthesia,internet bank,internet primary bank,jarunee wonglimpiyarat,jeunesse,jibc december 2007,juvenile cultures,juventud,limitations,luation of non-urgent visits,m-commerce,mecanismos de anteroalimentaci{\'{o}}n y,modificacio -,multimodal biometric,needle through a,nes corporales,network security,networks,neural networks,no,patents analysis,perforaci{\'{o}}n corporal,piel,professor of marketing,professor of marketing at,pr{\'{a}}ctica autolesiva,psicoan{\'{a}}lisis,recommender system,research,retroalimentaci{\'{o}}n,risks management,segunda piel,sensitivas y motoras,smart cards,social network analysis,social networks,social status,spinal,strategic,strategy,support vector machine,sustainable reconstruction,sydney fintech,sydney start-ups,tattoo,tattooing,tattoos,tatuaje,the literature on tattoos,the university of pennsylvania,the wharton school of,to a busy urban,traditional banking services,unimodal biometric,university of pennsylvania,vol,was reviewed to see,youth}, -month = {feb}, -number = {2}, -pages = {81--87}, -pmid = {15003161}, -title = {اختبار كلام}, -url = {http://www.americanbanker.com/issues/179_124/which-city-is-the-next-big-fintech-hub-new-york-stakes-its-claim-1068345-1.html%5Cnhttp://www.ncbi.nlm.nih.gov/pubmed/15003161%5Cnhttp://cid.oxfordjournals.org/lookup/doi/10.1093/cid/cir991%5Cnhttp://www.scielo}, -volume = {XXXIII}, -year = {2014} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G.}, -doi = {10.1086/507084}, -eprint = {0505272}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Agustsson, Brainerd - 2006 - The Locations of Satellite Galaxies in a $\Lambda$CDM Universe(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Fe, -author = {By, Llustrated}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/By - 2009 - P 2 P 2 P 2(2).pdf:pdf}, -keywords = {pee r}, -number = {1987}, -pages = {3--6}, -title = {{P 2 P 2 P 2}}, -volume = {93}, -year = {2009} -} -@article{Inoue2012, -abstract = {We explore the weak lensing effect by line-of-sight haloes and subhaloes with a mass of M ≲ 10 7M ⊙ in Quasi-Stellar Object (QSO)-galaxy strong lens systems with quadruple images in a concordant $\Lambda$ cold dark matter universe. Using a polynomially fitted non-linear power spectrum P(k) obtained from N-body simulations that can resolve haloes with a mass of M ∼ 10 5M ⊙, or structures with a comoving wavenumber of k ∼ 3 × 10 2hMpc -1, we find that the ratio of magnification perturbation due to intervening haloes to that of a primary lens is typically ∼10 per cent and the predicted values agree well with the estimated values for six observed QSO-galaxy lens systems with quadruple images in the mid-infrared band without considering the effects of substructures inside a primary lens. We also find that the estimated amplitudes of convergence perturbation for the six lenses increase with the source redshift as predicted by theoretical models. Using an extrapolated matter power spectrum, we demonstrate that small haloes or subhaloes in the line of sight with a mass of M = 10 3-10 7M ⊙, or structures with a comoving wavenumber of k = 3 × 10 2-10 4hMpc -1, can significantly affect the magnification ratios of the lensed images. Flux-ratio anomalies in QSO-galaxy strong lens systems offer us a unique probe into the clustering property of minihaloes with a mass of M < 10 6M ⊙. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1207.2139v2}, -author = {Inoue, Kaiki Taro and Takahashi, Ryuichi}, -doi = {10.1111/j.1365-2966.2012.21915.x}, -eprint = {arXiv:1207.2139v2}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: formation}, -number = {4}, -pages = {2978--2993}, -title = {{Weak lensing by line-of-sight haloes as the origin of flux-ratio anomalies in quadruply lensed QSOs}}, -volume = {426}, -year = {2012} -} -@article{Bode2001, -abstract = {Discrepancies have emerged between the predictions of standard cold dark matter (CDM) theory and observations of clustering on sub-galactic scales. Warm dark matter (WDM) is a simple modification of CDM in which the dark matter particles have initial velocities due either to their having decoupled as thermal relics, or having been formed via non-equilibrium decay. We investigate the nonlinear gravitational clustering of WDM with a high resolution N-body code, and identify a number of distinctive observational signatures. Relative to CDM, halo concentrations and core densities are lowered, core radii are increased, and large halos emerge with far fewer low mass satellites. The number of small halos is suppressed, and those present are formed by `top down' fragmentation of caustics, as part of a `cosmic web' connecting massive halos. Few small halos form outside this web. If we identify small halos with dwarf galaxies, their number, spatial distribution, and formation epoch appear in better agreement with the observations for WDM than they are for CDM.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0010389}, -author = {Bode, Paul and Ostriker, Jeremiah P. and Turok, Neil}, -doi = {10.1086/321541}, -eprint = {0010389}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Subject headings,cosmology,formation {\`{E}} galaxies,halos {\`{E}} methods,numerical,theory {\`{E}} dark matter {\`{E}} galaxies}, -month = {jul}, -number = {1}, -pages = {93--107}, -primaryClass = {astro-ph}, -title = {{Halo Formation in Warm Dark Matter Models}}, -url = {http://arxiv.org/abs/astro-ph/0010389%0Ahttp://dx.doi.org/10.1086/321541}, -volume = {556}, -year = {2001} -} -@article{Weijmans2014, -abstract = {We use the ATLAS3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation $\sigma$q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and $\sigma$q = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrizations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P T and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F and Davies, Roger L and Davis, Timothy A and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular,Galaxies,Structure,cD- galaxies}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Jimenez-Vicente2019, -abstract = {We present a new approach in the study of the Initial Mass function (IMF) in external galaxies based on quasar microlensing observations. We use measurements of quasar microlensing magnifications in 24 lensed quasars to estimate the average mass of the stellar population in the lens galaxies without any a priori assumption on the shape of the IMF. The estimated mean mass of the stars is {\$}\backslashlangle M \backslashrangle =0.16{\^{}}{\{}+0.05{\}}{\_}{\{}-0.08{\}} M{\_}\backslashodot{\$} (at 68$\backslash${\%} confidence level). We use this average mass to put constraints into two important parameters characterizing the IMF of lens galaxies: the low-mass slope, {\$}\backslashalpha{\_}2{\$}, and the low-mass cutoff, {\$}M{\_}{\{}low{\}}{\$}. Combining these constraints with prior information based on lensing, stellar dynamics, and absorption spectral feature analysis, we calculate the posterior probability distribution for the parameters {\$}M{\_}{\{}low{\}}{\$} and {\$}\backslashalpha{\_}2{\$}. We estimate values for the low-mass end slope of the IMF {\$}\backslashlangle \backslashalpha{\_}2\backslashrangle=-2.6\backslashpm 0.9{\$} (heavier than that of the Milky Way) and for the low-mass cutoff {\$}\backslashlangle M{\_}{\{}low{\}}\backslashrangle=0.13\backslashpm0.07{\$}. These results are in good agreement with previous studies on these parameters and remain stable against the choice of different suitable priors.}, -archivePrefix = {arXiv}, -arxivId = {1910.10509}, -author = {Jim{\'{e}}nez-Vicente, J and Mediavilla, E}, -doi = {10.3847/1538-4357/ab46b8}, -eprint = {1910.10509}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {75}, -title = {{The Initial Mass Function of Lens Galaxies from Quasar Microlensing}}, -url = {http://arxiv.org/abs/1910.10509%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/ab46b8}, -volume = {885}, -year = {2019} -} -@article{Greene2017b, -abstract = {The "kinematic" morphology-density relation for early-type galaxies posits that those galaxies with low angular momentum are preferentially found in the highest-density regions of the universe. We use a large sample of galaxy groups with halo masses 10{\^{}}12.5 {\textless} M{\_}halo {\textless} 10{\^{}}14.5 M{\_}sun/h observed with the Mapping Nearby Galaxies at APO (MaNGA) survey to examine whether there is a correlation between local environment and rotational support that is independent of stellar mass. We find no compelling evidence for a relationship between the angular momentum content of early-type galaxies and either local overdensity or radial position within the group at fixed stellar mass.}, -archivePrefix = {arXiv}, -arxivId = {1708.07843}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Goddard, D and Ge, J and Andrews, B H and Brinkman, J and Brownstein, J R and Greco, J and Law, D and Lin, Y.-T. and Masters, K L and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Yan, R and Drory, N}, -doi = {10.3847/2041-8213/aa8ace}, -eprint = {1708.07843}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L33}, -title = {{SDSS-IV MaNGA: Probing the Kinematic Morphology–Density Relation of Early-type Galaxies with MaNGA}}, -url = {http://arxiv.org/abs/1708.07843%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa8ace}, -volume = {851}, -year = {2017} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Seabroke2011, -abstract = {Gaia will only achieve its unprecedented measurement accuracy requirements with detailed calibration and correction for radiation damage. We present our Silvaco 3D engineering software model of the Gaia CCD pixel and two of its applications for Gaia: (1) physically interpreting supplementary buried channel (SBC) capacity measurements (pocket-pumping and first pixel response) in terms of e2v manufacturing doping alignment tolerances; and (2) deriving electron densities within a charge packet as a function of the number of constituent electrons and 3D position within the charge packet as input to microscopic models being developed to simulate radiation damage. {\textcopyright}EAS, EDP Sciences 2011.}, -archivePrefix = {arXiv}, -arxivId = {1009.2431}, -author = {Seabroke, G M and Prod'homme, T and Hopkinson, G and Burt, D and Robbins, M and Holland, A}, -doi = {10.1051/eas/1045077}, -eprint = {1009.2431}, -isbn = {9782759806089}, -issn = {16334760}, -journal = {EAS Publications Series}, -pages = {433--436}, -title = {{Modelling Gaia CCD pixels with silvaco 3D engineering software}}, -url = {http://www.eas-journal.org/10.1051/eas/1045077}, -volume = {45}, -year = {2011} -} -@article{Aguero2016, -abstract = {We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75% of the hosts), with a bar (44% weak, 37% strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem not to be important for the appearance of CNRs, which appear to be more related to intrinsic properties of the host galaxies or to minor merger processes; 2) the proportion of weak bars in galaxies with a CNR is higher than expected; 3) the incidence of Seyfert (Sy) activity coeval with CNRs is significantly larger than the rate expected from the morphological distribution of the host galaxies; 4) the rate of Sy 2 to Sy 1 type galaxies with CNRs is about three times larger than the expected ratio for galaxies without CNRs and is opposite to that predicted by the geometric paradigm of the classical unified model for AGNs, although it does support the hypothesis that Sy 2 activity is linked to circumnuclear star formation. The possible selection effects of the sample are discussed, and we conclude that the detected trends are strong enough to justify high quality observations of as large as possible set of galaxies with circumnuclear rings and their matched control samples.}, -author = {Ag{\"{u}}ero, Mar{\'{i}}a P. and D{\'{i}}az, Rub{\'{e}}n J. and Dottori, Horacio}, -doi = {10.4236/ijaa.2016.63018}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ag{\"{u}}ero, D{\'{i}}az, Dottori - 2016 - Nuclear Activity in Circumnuclear Ring Galaxies(2).pdf:pdf}, -issn = {2161-4717}, -journal = {International Journal of Astronomy and Astrophysics}, -keywords = {active,dynamics,galaxies,nuclei,spiral,structure}, -number = {03}, -pages = {219--235}, -title = {{Nuclear Activity in Circumnuclear Ring Galaxies}}, -url = {http://www.scirp.org/journal/doi.aspx?DOI=10.4236/ijaa.2016.63018}, -volume = {06}, -year = {2016} -} -@article{Wood2014, -abstract = {The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D and Hall, D J and Murray, N J and Gow, J P D and Holland, A and Turner, P and Burt, D}, -doi = {10.1088/1748-0221/9/12/C12028}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv,visible and ir photons (s}, -number = {12}, -pages = {C12028----C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{Khochfar2011, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* > 1010.5M⊙ contributing $\sim$20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between $\sim$50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z > 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) > 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z < 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive (>1010M⊙) fast rotators being more than one order of magnitude more frequent at z$\sim$ 2. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R. and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Khochfar et al. - 2011 - The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies.pdf:pdf}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: structure}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Kennicutt, -abstract = {We review progress over the past decade in observations of large-scale star formation, with a focus on the interface between extragalactic and Galactic studies. Methods of measuring gas contents and star-formation rates are discussed, and updated prescriptions for calculating star-formation rates are provided. We review relations between star formation and gas on scales ranging from entire galaxies to individual molecular clouds. Copyright {\textcopyright} 2012 by Annual Reviews.}, -archivePrefix = {arXiv}, -arxivId = {1204.3552}, -author = {Kennicutt, Robert C. and Evans, Neal J.}, -doi = {10.1146/annurev-astro-081811-125610}, -eprint = {1204.3552}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kennicutt, Evans - 2012 - Star formation in the milky way and nearby galaxies.pdf:pdf}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {clouds,evolution,interstellar medium (ISM),molecules}, -number = {1}, -pages = {531--608}, -title = {{Star formation in the milky way and nearby galaxies}}, -url = {http://arxiv.org/abs/1204.3552%0Ahttp://dx.doi.org/10.1146/annurev-astro-081811-125610}, -volume = {50}, -year = {2012} -} -@article{Cautun2015a, -abstract = {We investigate the angular and kinematic distributions of satellite galaxies around a large sample of bright isolated primaries in the spectroscopic and photometric catalogues of the Sloan Digital Sky Survey (SDSS). We detect significant anisotropy in the spatial distribution of satellites. To test whether this anisotropy could be related to the rotating discs of satellites recently found by Ibata et al. in a sample of SDSS galaxies, we repeat and extend their analysis. Ibata et al. found an excess of satellites on opposite sides of their primaries having anticorrelated radial velocities. We find that this excess is sensitive to small changes in the sample selection criteria which can greatly reduce its significance. In addition, we find no evidence for correspondingly correlated velocities for satellites observed on the same side of their primaries, which would be expected for rotating discs of satellites. We conclude that the detection of rotating planes of satellites in the observational sample of Ibata et al. is not robust to changes in the sample selection criteria. We compare our data to the $\Lambda$ cold dark matter Millennium simulations populated with galaxies according to the semi-analytic model of Guo et al. We find excellent agreement with the spatial distribution of satellites in the SDSS data and the lack of a strong signal from coherent rotation.}, -archivePrefix = {arXiv}, -arxivId = {1410.7778}, -author = {Cautun, Marius and Wang, Wenting and Frenk, Carlos S and Sawala, Till}, -doi = {10.1093/mnras/stv490}, -eprint = {1410.7778}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {3}, -pages = {2576--2587}, -title = {{A new spin on discs of satellite galaxies}}, -volume = {449}, -year = {2015} -} -@article{Bruce2012, -abstract = {We have used high-resolution, HST WFC3/IR, near-infrared imaging to conduct a detailed bulge-disk decomposition of the morphologies of ≃ 200 of the most massive (M * > 1011 M{\textperiodcentered}) galaxies at 1 < z < 3 in the CANDELS-UDS field. We find that, while such massive galaxies at low redshift are generally bulge-dominated, at redshifts 1 2 they are mostly disk-dominated. Interestingly, we find that while most of the quiescent galaxies are bulge-dominated, a significant fraction (25-40%) of the most quiescent galaxies, have disk-dominated morphologies. Thus, our results suggest that the physical mechanisms which quench star-formation activity are not simply connected to those responsible for the morphological transformation of massive galaxies. {\textcopyright} 2013 International Astronomical Union.}, -archivePrefix = {arXiv}, -arxivId = {1206.4322}, -author = {Bruce, V. A. and Dunlop, J. S. and Cirasuolo, M. and McLure, R. J. and Targett, T. A. and Bell, E. F. and Croton, D. J. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and Lai, K. and Lotz, J. M. and McGrath, E. J. and Newman, J. A. and {Van Der Wel}, A.}, -doi = {10.1017/S1743921313004237}, -eprint = {1206.4322}, -isbn = {9781107033849}, -issn = {17439213}, -journal = {Proceedings of the International Astronomical Union}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: high-redshift,galaxies: structure}, -month = {dec}, -number = {S295}, -pages = {49--52}, -title = {{The morphologies of massive galaxies at 1500 kpc/h) SGs. For highly concentrated SGs at small (<300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to <15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby (<40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ($\sim$3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R. J. and Ryden, B. S. and Gaudi, B. S.}, -eprint = {0903.2264}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Siverd, Ryden, Gaudi - 2009 - Galaxy Orientation and Alignment Effects in the SDSS DR6.pdf:pdf}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently-discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially-interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorised according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}10{\^{}}11 Msun to {\textgreater}10{\^{}}13 Msun. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}10{\^{}}11 Msun. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW05). The two low-mass outliers are J0206-095 (SW19) and J2217+015 (SW42); if these two are indeed lenses, they probe an interesting regime of very low star-formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of supermassive black hole (SMBH) formation and evolution is used, as in Tremmel et al., allowing us to explicitly follow the SMBH dynamics at the centre of galaxies. A high SIDM constant cross-section is chosen, $\sigma$ = 10 cm2gr-1, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in cold dark matter (CDM), with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals, the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80 per cent of the SMBH population is offcentred in the SIDM case, as opposed to the CDM case in which {\$\sim${}}90 per cent of SMBHs have reached their host's centre. SMBHs are found as far as {\$\sim${}}9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction time-scale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in core stalling. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to the SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series which re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science database, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies (CSRG). This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications, and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution which limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ("encounter-driven") rings (such as ring and polar ring galaxies) are recognized in less than 1{\$}\backslash{\$}{\%} of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the haloes' virial radius while describing the infalling matter via fluxes through a spherical shell; we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP first described in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one and two points statistics.The infall takes place preferentially in the plane perpendicular to the direction defined by the halo's spin. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be {\$\sim${}}15 {\%}. The substructures have their spin orthogonal to their velocity vector in the halo's rest frame at a level of about 5{\%}, suggestive of an image of a flow along filamentary structures which provides an explanation for the measured anisotropy. We conclude that a halo does not see its environment as an isotropic perturbation, investigate how the anisotropy is propagated inwards using perturbation theory, and discuss briefly implications for weak lensing, warps and the thickness of galactic disks.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D and Pichon, C and Colombi, S}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Shu2016, -abstract = {We introduce the Baryon Oscillation Spectroscopic Survey (BOSS) Emission-Line Lens Survey (BELLS) for GALaxy-Ly$\alpha$ EmitteR sYstems (BELLS GALLERY) Survey, which is a Hubble Space Telescope program to image a sample of galaxy-scale strong gravitational lens candidate systems with high-redshift Ly$\alpha$ emitters (LAEs) as the background sources. The goal of the BELLS GALLERY Survey is to illuminate dark substructures in galaxy-scale halos by exploiting the small-scale clumpiness of rest-frame far-UV emission in lensed LAEs, and to thereby constrain the slope and normalization of the substructure-mass function. In this paper, we describe in detail the spectroscopic strong-lens selection technique, which is based on methods adopted in the previous Sloan Lens ACS (SLACS) Survey, BELLS, and SLACS for the Masses Survey. We present the BELLS GALLERY sample of the 21 highest-quality galaxy--LAE candidates selected from $\approx 1.4 \times 10^6$ galaxy spectra in the BOSS of the Sloan Digital Sky Survey III. These systems consist of massive galaxies at redshifts of approximately 0.5 strongly lensing LAEs at redshifts from 2--3. The compact nature of LAEs makes them an ideal probe of dark substructures, with a substructure-mass sensitivity that is unprecedented in other optical strong-lens samples. The magnification effect from lensing will also reveal the structure of LAEs below 100 pc scales, providing a detailed look at the sites of the most concentrated unobscured star formation in the universe. The source code used for candidate selection is available for download as a part of this release.}, -archivePrefix = {arXiv}, -arxivId = {1604.01842}, -author = {Shu, Yiping and Bolton, Adam S. and Kochanek, Christopher S. and Oguri, Masamune and P{\'{e}}rez-Fournon, Ismael and Zheng, Zheng and Mao, Shude and Montero-Dorta, Antonio D. and Brownstein, Joel R. and Marques-Chaves, Rui and M{\'{e}}nard, Brice}, -doi = {10.3847/0004-637x/824/2/86}, -eprint = {1604.01842}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shu et al. - 2016 - THE BOSS EMISSION-LINE LENS SURVEY. III. STRONG LENSING OF Ly $\alpha$ EMITTERS BY INDIVIDUAL GALAXIES(2).pdf:pdf}, -isbn = {0004-637x}, -issn = {1538-4357}, -journal = {ApJ}, -number = {2}, -pages = {86}, -title = {{THE BOSS EMISSION-LINE LENS SURVEY. III. STRONG LENSING OF Ly $\alpha$ EMITTERS BY INDIVIDUAL GALAXIES}}, -url = {http://arxiv.org/abs/1604.01842%0Ahttp://dx.doi.org/10.3847/0004-637X/824/2/86}, -volume = {824}, -year = {2016} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance LCDM cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for `radio' feedback from those AGN that lie at the centre of a quasistatic X-ray emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models which might explain the accretion rate scalings required for our phenomenological `radio mode' model to be successful.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J and Springel, Volker and White, Simon D M and {De Lucia}, G and Frenk, C S and Gao, L and Jenkins, A and Kauffmann, G and Navarro, J F and Yoshida, N}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Morishita2018a, -abstract = {Observations have revealed massive (logM*/Msun>11) galaxies that were already dead when the universe was only $\sim$2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6 50% of their extant masses by $\sim$1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of $\sim$0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z$\sim$5.5 to $\sim$2.2 at a rate of $\sim$0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, $\sim$0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T. and Abramson, L. E. and Treu, T. and Brammer, G. B. and Jones, T. and Kelly, P. and Stiavelli, M. and Trenti, M. and Vulcani, B. and Wang, X.}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Morishita et al. - 2019 - Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrich.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {evolution,formation,galaxies,star formation}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Bentabol2016, -abstract = {We examine a sample of 1495 galaxies in the CANDELS fields to determine the evolution of two component galaxies, including bulges and discs, within massive galaxies at the epoch 1 {\textless} z {\textless} 3 when the Hubble sequence forms. We fit all of our galaxies' light profiles with a single S$\backslash$'ersic fit, as well as with a combination of exponential and S$\backslash$'ersic profiles. The latter is done in order to describe a galaxy with an inner and an outer component, or bulge and disc component. We develop and use three classification methods (visual, F-test and the RFF) to separate our sample into 1-component galaxies (disc/spheroids-like galaxies) and 2-component galaxies (galaxies formed by an 'inner part' or bulge and an 'outer part' or disc). We then compare the results from using these three different ways to classify our galaxies. We find that the fraction of galaxies selected as 2-component galaxies increases on average 50 per cent from the lowest mass bin to the most massive galaxies, and decreases with redshift by a factor of four from z = 1 to z = 3. We find that single S$\backslash$'ersic 'disc-like' galaxies have the highest relative number densities at all redshifts, and that 2-component galaxies have the greatest increase and become at par with S$\backslash$'ersic discs by z = 1. We also find that the systems we classify as 2-component galaxies have an increase in the sizes of their outer components, or 'discs', by about a factor of three from z = 3 to z = 1.5, while the inner components or 'bulges' stay roughly the same size. This suggests that these systems are growing from the inside out, whilst the bulges or protobulges are in place early in the history of these galaxies. This is also seen to a lesser degree in the growth of single 'disc-like' galaxies vs. 'spheroid-like' galaxies over the same epoch.}, -archivePrefix = {arXiv}, -arxivId = {1606.07405}, -author = {Margalef-Bentabol, Berta and Conselice, Christopher J and Mortlock, Alice and Hartley, Will and Duncan, Kenneth and Ferguson, Harry C and Dekel, Avishai and Primack, Joel R}, -doi = {10.1093/mnras/stw1451}, -eprint = {1606.07405}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure}, -number = {3}, -pages = {1--21}, -title = {{The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z {\textless} 3}}, -volume = {461}, -year = {2016} -} -@article{Rusu2019, -abstract = {We present the lens mass model of the quadruply-imaged gravitationally lensed quasar WFI2033-4723, and perform a blind cosmographical analysis based on this system. Our analysis combines (1) time-delay measurements from 14 years of data obtained by the COSmological MOnitoring of GRAvItational Lenses (COSMOGRAIL) collaboration, (2) high-resolution {\$}\backslashtextit{\{}Hubble Space Telescope{\}}{\$} imaging, (3) a measurement of the velocity dispersion of the lens galaxy based on ESO-MUSE data, and (4) multi-band, wide-field imaging and spectroscopy characterizing the lens environment. We account for all known sources of systematics, including the influence of nearby perturbers and complex line-of-sight structure, as well as the parametrization of the light and mass profiles of the lensing galaxy. After unblinding, we determine the effective time-delay distance to be {\$}4784{\_}{\{}-248{\}}{\^{}}{\{}+399{\}}{\\sim{}}\backslashmathrm{\{}Mpc{\}}{\$}, an average precision of {\$}6.6\backslash{\%}{\$}. This translates to a Hubble constant {\$}H{\_}{\{}0{\}} = 71.6{\_}{\{}-4.9{\}}{\^{}}{\{}+3.8{\}}{\\sim{}}\backslashmathrm{\{}km{\\sim{}}s{\^{}}{\{}-1{\}}{\\sim{}}Mpc{\^{}}{\{}-1{\}}{\}}{\$}, assuming a flat {\$}\backslashLambda{\$}CDM cosmology with a uniform prior on {\$}\backslashOmega{\_}\backslashmathrm{\{}m{\}}{\$} in the range [0.05, 0.5]. This work is part of the {\$}H{\_}0{\$} Lenses in COSMOGRAIL's Wellspring (H0LiCOW) collaboration, and the full time-delay cosmography results from a total of six strongly lensed systems are presented in a companion paper (Wong et. al. 2019, in preparation).}, -archivePrefix = {arXiv}, -arxivId = {1905.09338}, -author = {Rusu, Cristian E and Wong, Kenneth C and Bonvin, Vivien and Sluse, Dominique and Suyu, Sherry H and Fassnacht, Christopher D and Chan, James H H and Hilbert, Stefan and Auger, Matthew W and Sonnenfeld, Alessandro and Birrer, Simon and Courbin, Frederic and Treu, Tommaso and Chen, Geoff C -F. and Halkola, Aleksi and Koopmans, Leon V E and Marshall, Philip J and Shajib, Anowar J}, -eprint = {1905.09338}, -keywords = {cosmological parameters,cosmology,distance scale}, -pages = {0--29}, -title = {{H0LiCOW XII. Lens mass model of WFI2033-4723 and blind measurement of its time-delay distance and {\$}H{\_}0{\$}}}, -url = {http://arxiv.org/abs/1905.09338}, -year = {2019} -} -@article{Seabroke2011, -abstract = {Gaia will only achieve its unprecedented measurement accuracy requirements with detailed calibration and correction for radiation damage. We present our Silvaco 3D engineering software model of the Gaia CCD pixel and two of its applications for Gaia: (1) physically interpreting supplementary buried channel (SBC) capacity measurements (pocket-pumping and first pixel response) in terms of e2v manufacturing doping alignment tolerances; and (2) deriving electron densities within a charge packet as a function of the number of constituent electrons and 3D position within the charge packet as input to microscopic models being developed to simulate radiation damage. {\textcopyright}EAS, EDP Sciences 2011.}, -archivePrefix = {arXiv}, -arxivId = {1009.2431}, -author = {Seabroke, G M and Prod'homme, T and Hopkinson, G and Burt, D and Robbins, M and Holland, A}, -doi = {10.1051/eas/1045077}, -eprint = {1009.2431}, -isbn = {9782759806089}, -issn = {16334760}, -journal = {EAS Publications Series}, -pages = {433--436}, -title = {{Modelling Gaia CCD pixels with silvaco 3D engineering software}}, -url = {http://www.eas-journal.org/10.1051/eas/1045077}, -volume = {45}, -year = {2011} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9602085}, -author = {Baugh, C. M. and Cole, S. and Frenk, C. S.}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Baugh, Cole, Frenk - 1996 - Evolution of the Bubble sequence in hierarchical models for galaxy formation(2).pdf:pdf}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function, mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{Ullio2002, -abstract = {We investigate the prospects of detecting weakly interacting massive particle (WIMP) dark matter by measuring the contribution to the extragalactic gamma-ray radiation induced, in any dark matter halo and at all redshifts, by WIMP pair annihilations into high-energy photons. We perform a detailed analysis of the very distinctive spectral features of this signal, recently proposed in a short letter by three of the authors: The gamma-ray flux which arises from the decay of $\pi$0 mesons produced in the fragmentation of annihilation final states shows a severe cutoff close to the value of the WIMP mass. An even more spectacular signature appears for the monochromatic gamma-ray components, generated by WIMP annihilations into two-body final states containing a photon: the combined effect of cosmological redshift and absorption along the line of sight produces sharp bumps, peaked at the rest frame energy of the lines and asymmetrically smeared to lower energies. The level of the flux depends both on the particle physics scenario for WIMP dark matter (we consider, as our template case, the lightest supersymmetric particle in a few supersymmetry breaking schemes), and on the question of how dark matter clusters. Uncertainties introduced by the latter are thoroughly discussed implementing a realistic model inspired by results of the state-of-the-art N-body simulations and semianalytic modeling in the cold dark matter structure formation theory. We also address the question of the potential gamma-ray background originating from active galaxies, presenting a novel calculation and critically discussing the assumptions involved and the induced uncertainties. Furthermore, we apply a realistic model for the absorption of gamma-rays on the optical and near-IR intergalactic radiation field to derive predictions for both the signal and background. Comparing the two, we find that there are viable configurations, in the combined parameter space defined by the particle physics setup and the structure formation scenario, for which the WIMP induced extragalactic gamma-ray signal will be detectable in the new generation of gamma-ray telescopes such as GLAST.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0207125v1}, -author = {Ullio, Piero and Bergstr{\"{o}}m, Lars and Edsj{\"{o}}, Joakim and Lacey, Cedric}, -doi = {10.1103/PhysRevD.66.123502}, -eprint = {0207125v1}, -issn = {05562821}, -journal = {Physical Review D}, -number = {12}, -pages = {123502}, -primaryClass = {arXiv:astro-ph}, -title = {{Cosmological dark matter annihilations into $\gamma$ rays: A closer look}}, -volume = {66}, -year = {2002} -} -@article{Abadi2010, -abstract = {We use N-body/gasdynamical cosmological simulations to examine the effect of the assembly of a central galaxy on the shape and mass profile of its surrounding dark matter halo. Two series of simulations are compared; one that follows only the evolution of the dark matter component of individual haloes in the proper $\Lambda$cold dark matter ($\Lambda$CDM) cosmological context, and a second series where a baryonic component is added and followed hydrodynamically. The simulations with baryons include radiative cooling but neglect the formation of stars and their feedback. The efficient, unimpeded cooling that results leads most baryons to collect at the halo centre in a centrifugally supported disc which, due to angular momentum losses, is too small and too massive when compared with typical spiral galaxies. This admittedly unrealistic model allows us, nevertheless, to gauge the maximum effect that galaxies may have in transforming their surrounding dark haloes. We find, in agreement with earlier work, that the shape of the halo becomes more axisymmetric: post galaxy assembly, haloes are transformed from triaxial into essentially oblate systems, with well-aligned isopotential contours of roughly constant flattening (〈/a〉∼ 0.85). Haloes always contract as a result of galaxy assembly, but the effect is substantially less pronounced than predicted by the traditional 'adiabatic-contraction' hypothesis. The reduced contraction helps to reconcile $\Lambda$CDM haloes with constraints on the dark matter content inside the solar circle and should alleviate the longstanding difficulty of matching simultaneously the scaling properties of galaxy discs and the galaxy luminosity function. The halo contraction we report is also less pronounced than found in earlier simulations, a disagreement which suggests that halo contraction is not solely a function of the initial and final distribution of baryons. Not only how much baryonic mass has been deposited at the centre of a halo matters, but also the mode of its deposition. Although simple formulae might work in particular cases where galaxies form nearly adiabatically, in general it might prove impossible to predict the halo response to galaxy formation without a detailed understanding of a galaxy's detailed assembly history. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0902.2477}, -author = {Abadi, Mario G. and Navarro, Julio F. and Fardal, Mark and Babul, Arif and Steinmetz, Matthias}, -doi = {10.1111/j.1365-2966.2010.16912.x}, -eprint = {0902.2477}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: disc,Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {sep}, -number = {1}, -pages = {435--446}, -title = {{Galaxy-induced transformation of dark matter haloes}}, -volume = {407}, -year = {2010} -} -@article{Jaelani2023, -abstract = {We apply a novel model based on convolutional neural networks (CNNs) to identify gravitationally-lensed galaxies in multi-band imaging of the Hyper Suprime Cam Subaru Strategic Program (HSC-SSP) Survey. The trained model is applied to a parent sample of 2 350 061 galaxies selected from the $\sim$ 800 deg$^2$ Wide area of the HSC-SSP Public Data Release 2. The galaxies in HSC Wide are selected based on stringent pre-selection criteria, such as multiband magnitudes, stellar mass, star formation rate, extendedness limit, photometric redshift range, etc. Initially, the CNNs provide a total of 20 241 cutouts with a score greater than 0.9, but this number is subsequently reduced to 1 522 cutouts by removing definite non-lenses for further inspection by human eyes. We discover 43 definite and 269 probable lenses, of which 97 are completely new. In addition, out of 880 potential lenses, we recovered 289 known systems in the literature. We identify 143 candidates from the known systems that had higher confidence in previous searches. Our model can also recover 285 candidate galaxy-scale lenses from the Survey of Gravitationally lensed Objects in HSC Imaging (SuGOHI), where a single foreground galaxy acts as the deflector. Even though group-scale and cluster-scale lens systems were not included in the training, a sample of 32 SuGOHI-c (i.e., group/cluster-scale systems) lens candidates was retrieved. Our discoveries will be useful for ongoing and planned spectroscopic surveys, such as the Subaru Prime Focus Spectrograph project, to measure lens and source redshifts in order to enable detailed lens modelling.}, -archivePrefix = {arXiv}, -arxivId = {2312.07333}, -author = {Jaelani, Anton T. and More, Anupreeta and Wong, Kenneth C. and Inoue, Kaiki T. and Chao, Dani C. -Y. and Premadi, Premana W. and Ca{\~{n}}ameras, Raoul}, -eprint = {2312.07333}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Jaelani2023SLFindHSC.pdf:pdf}, -keywords = {analysis data,gravitational lensing,methods,strong}, -number = {December}, -pages = {1--11}, -title = {{Survey of Gravitationally lensed Objects in HSC Imaging (SuGOHI) $-$ X. Strong Lens Finding in The HSC-SSP using Convolutional Neural Networks}}, -url = {http://arxiv.org/abs/2312.07333}, -volume = {11}, -year = {2023} -} -@article{Amorisco:2017aa, -abstract = {The accreted component of stellar haloes is composed of the contributions of several satellites, falling on to their host with their different masses, at different times, on different orbits. This work uses a suite of idealized, collisionless N-body simulations of minor mergers and a particle-tagging technique to understand how these different ingredients shape each contribution to the accreted halo, in both density and kinematics. I find that more massive satellites deposit their stars deeper into the gravitational potential of the host, with a clear segregation enforced by dynamical friction. Earlier accretion events contribute more to the inner regions of the halo; more concentrated subhaloes sink deeper through increased dynamical friction. The orbital circularity of the progenitor at infall is only important for low-mass satellites: dynamical friction efficiently radializes the most massive minor mergers erasing the imprint of the infall orbit for satellite-to-host virial mass ratios ≳ 1/20. The kinematics of the stars contributed by each satellite is also ordered with satellite mass: low-mass satellites contribute fast-moving populations, in both ordered rotation and radial velocity dispersion. In turn, contributions by massive satellites have lower velocity dispersion and lose their angular momentum to dynamical friction, resulting in a strong radial anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {1511.08806}, -author = {Amorisco, N. C.}, -doi = {10.1093/mnras/stw2229}, -eprint = {1511.08806}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Amorisco - 2017 - Contributions to the accreted stellar halo An atlas of stellar deposition(3).pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Amorisco - 2017 - Contributions to the accreted stellar halo An atlas of stellar deposition(4).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: interactions,Galaxies: kinematics and dynamics,Galaxies: structure,Galaxy: halo}, -month = {jan}, -number = {3}, -pages = {2882--2895}, -title = {{Contributions to the accreted stellar halo: An atlas of stellar deposition}}, -url = {http://arxiv.org/abs/1511.08806%0Ahttp://dx.doi.org/10.1093/mnras/stw2229}, -volume = {464}, -year = {2017} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, $M_{BH}$, that had been imaged at $3.6\sim\mu m$ with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between $M_{ BH}$ and the host spheroid (and galaxy) luminosity, $L_{sph}$ (and $L_{gal}$), and also stellar mass, $M_{*,sph}$. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have $M_{BH} < 10^7\simM_\odot$, and allows us to better investigate the poorly studied low-mass end of the $M_{BH} - M_{*,sph}$ correlation. The bulges of early-type galaxies follow $M_{BH} \propto M_{*,sph}^{1.04 \pm 0.10}$ and define a tight red sequence with intrinsic scatter $\epsilon = 0.43 \pm 0.06\simdex$ and a median $M_{BH}/M_{*,sph}$ ratio of $0.68 \pm 0.04\%$, i.e.$\sim$a $\pm 2\sigma$ range of 0.1-5%. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with $M_{BH} \propto M_{*,sph}^{2-3}$, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index $n<2$, argued by some to be pseudo-bulges, are not offset to lower $M_{BH}$ from the correlation defined by the current bulge sample with $n>2$; and iii) $L_{sph}$ and $L_{gal}$ correlate equally well with $M_{BH}$, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with $L_{ sph}$ is better than that with $L_{gal}$.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A. D. and Graham, Alister W. and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Savorgnan et al. - 2016 - Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M ,Sph Diagr(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Powell2022, -abstract = {We investigate the mass structure of a strong gravitational lens galaxy at z = 0.350, taking advantage of the milliarcsecond (mas) angular resolution of very long baseline interferometric (VLBI) observations. In the first analysis of its kind at this resolution, we jointly infer the lens model parameters and pixellated radio source surface brightness. We consider several lens models of increasing complexity, starting from an elliptical power-law density profile. We extend this model to include angular multipole structures, a separate stellar mass component, additional nearby field galaxies, and/or a generic external potential. We compare these models using their relative Bayesian log-evidence (Bayes factor). We find strong evidence for angular structure in the lens; our best model is comprised of a power-law profile plus multipole perturbations and external potential, with a Bayes factor of +14984 relative to the elliptical power-law model. It is noteworthy that the elliptical power-law mass distribution is a remarkably good fit on its own, with additional model complexity correcting the deflection angles only at the ∼5 mas level. We also consider the effects of added complexity in the lens model on time-delay cosmography and flux-ratio analyses. We find that an overly simplistic power-law ellipsoid lens model can bias the measurement of H0 by ∼3 per cent and mimic flux ratio anomalies of ∼8 per cent. Our results demonstrate the power of high-resolution VLBI observations to provide strong constraints on the inner density profiles of lens galaxies.}, -archivePrefix = {arXiv}, -arxivId = {2207.03375}, -author = {Powell, Devon M. and Vegetti, Simona and McKean, J. P. and Spingola, Cristiana and Stacey, Hannah R. and Fassnacht, Christopher D.}, -doi = {10.1093/mnras/stac2350}, -eprint = {2207.03375}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Powell et al. - 2022 - A lensed radio jet at milliarcsecond resolution I Bayesian comparison of parametric lens models.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {galaxies: structure,gravitational lensing: strong,methods: data analysis,quasars: individual: MG J0751+2716,radio continuum: general}, -number = {2}, -pages = {1808--1828}, -title = {{A lensed radio jet at milliarcsecond resolution I: Bayesian comparison of parametric lens models}}, -volume = {516}, -year = {2022} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum {\$}j{\_}\backslashstar{\$} and the stellar mass {\$}M{\_}\backslashstar{\$} in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction {\$}f{\_}{\{}\backslashrm inf{\}}{\$} of baryons that infall toward the central regions of galaxies where star formation can occur. We find {\$}f{\_}{\{}\backslashrm inf{\}}\backslashapprox 1{\$} for LTGs and {\$}\backslashapprox 0.4{\$} for ETGs with an uncertainty of about {\$}0.25{\$} dex, consistent with a biased collapse. By comparing with the locally observed {\$}j{\_}\backslashstar{\$} vs. {\$}M{\_}\backslashstar{\$} relations for LTGs and ETGs we estimate the fraction {\$}f{\_}j{\$} of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find {\$}f{\_}j\backslashapprox 1.11{\^{}}{\{}+0.75{\}}{\_}{\{}-0.44{\}}{\$}, in line with the classic disc formation picture; for ETGs we infer {\$}f{\_}j\backslashapprox 0.64{\^{}}{\{}+0.20{\}}{\_}{\{}-0.16{\}}{\$}, that can be traced back to a {\$}z{\textless}1{\$} evolution via dry mergers. We also show that the observed scatter in the {\$}j{\_}{\{}\backslashstar{\}}{\$} vs. {\$}M{\_}{\{}\backslashstar{\}}{\$} relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at {\$}z\backslashsim 2{\$} is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, Jingjing and Lapi, Andrea and Mancuso, Claudia and Wang, Huiyuan and Danese, Luigi}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -issn = {1538-4357}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {1983}, -title = {{Angular Momentum of Early and Late Type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -year = {2017} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {SPIE High Energy, Optical and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Chen2018, -abstract = {At cosmological distances, gravitational lensing can provide a direct measurement of supermassive black hole (SMBH) masses irrespective of their luminosities. Here, we directly estimate the mass of a SMBH in the brightest cluster galaxy (BCG) of MACS J1149+2223.5 at $z=0.54$ through one of the multiply-lensed images of a background spiral galaxy at $z=1.49$ projected close to the BCG. In this particular image, an intrinsically compact region in one of the spiral arms is lensed into an arc that curves towards the BCG center. This arc has a radius of curvature of only $\sim$0."6, betraying the presence of a local compact deflector. Its curvature is most simply reproduced by a point-like object with a mass of $8.4^{+4.3}_{-1.8}\times10^{9}M_\odot$, similar to SMBH masses in local elliptical galaxies having comparable luminosities. The SMBH is noticeably offset by $4.4\pm0.3$ kpc from the BCG light centre, plausibly the result of a kick imparted $\sim2.0\times10^7$ years ago during the merger of two SMBHs, placing it just beyond the stellar core. A similar curvature can be produced by replacing the offset SMBH with a compact galaxy having a mass of $\sim2\times 10^{10}M_\odot$ within a cutoff radius of $<4$ kpc, and an unusually large $M/L>50(M/L)_\odot$ to make it undetectable in the deep Hubble Frontiers Fields image, at or close to the cluster redshift; such a lensing galaxy, however, perturbs the adjacent lensed images in an undesirable way.}, -archivePrefix = {arXiv}, -arxivId = {1805.05051}, -author = {Chen, Mandy C. and Broadhurst, Tom and Lim, Jeremy and Diego, Jose M. and Ohyama, Youichi and Ford, Holland and Ben{\'{i}}tez, Narciso}, -doi = {10.3847/1538-4357/aad17b}, -eprint = {1805.05051}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Chen2018SMBHSL.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {2223,5,cD,cd,clusters,elliptical and lenticular,evolution,galaxies,galaxies: clusters: individual (MACS J1149.5+2223),galaxies: elliptical and lenticular,galaxies: evolution,galaxies: nuclei,gravitational lensing,gravitational lensing: strong,individual,macs j1149,nuclei,strong}, -number = {2}, -pages = {135}, -publisher = {IOP Publishing}, -title = {{A Likely Supermassive Black Hole Revealed by Its Einstein Radius in Hubble Frontier Fields Images}}, -url = {http://dx.doi.org/10.3847/1538-4357/aad17b}, -volume = {863}, -year = {2018} -} -@article{Pulsoni2017, -abstract = {Wolbachia is an intracellular endosymbiont that induces a variety of reproductive alterations in diverse arthropods. The almond moth, Cadra cautella, is double infected with two Wolbachia variants, wCauA and wCauB, and expresses complete cytoplasmic incompatibility (CI). The individual contribution of wCauA and wCauB to the expression of CI are unclear, however, because the two variants have not been separated in this host. The effect of wCauA is of particular interest because it induces male killing when transferred into the Mediterranean flour moth, Ephestia kuehniella. In the present study, we generated C. cautella infected with only wCauA by treating double-infected insects with tetracycline. Single-infected C. cautella exhibited strong CI, demonstrating that wCauA induces two distinct reproductive phenotypes in different hosts: CI in C. cautella and male killing in E. kuehniella. CI was also observed in the cross of double-infected males and single-infected females. Comparison of the single- and double-infected insects by real-time quantitative polymerase chain reaction suggested that the wCauA density is not affected much by the presence or absence of wCauB. {\textcopyright}2005 Nature Publishing Group All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {http://www.R-project.org}, -author = {Sasaki, T and Massaki, N and Kubo, T}, -doi = {10.1038/sj.hdy.6800737}, -eprint = {/www.R-project.org}, -isbn = {0018-067X}, -issn = {0018067X}, -journal = {Heredity}, -keywords = {Cadra cautella,Cytoplasmic incompatibility,Double infection,Male killing,Real-time quantitative PCR,Wolbachia}, -number = {5}, -pages = {389--393}, -pmid = {16106260}, -primaryClass = {http:}, -title = {{Wolbachia variant that induces two distinct reproductive phenotypes in different hosts}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/16106260}, -volume = {95}, -year = {2005} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M{\_}*/M{\_}sun) {\textgreater}11.5 (M{\_}K {\textless}-25.3 mag) and distance D {\textless}108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38{\$}\backslash{\$}pm6{\%} down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80{\$}\backslash{\$}pm10{\%} and 28{\$}\backslash{\$}pm6{\%}, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R{\_}e), and the gas morphologies are diverse, with 17/28 = 61{\$}\backslash{\$}pm9{\%} being centrally concentrated, 8/28 = 29{\$}\backslash{\$}pm9{\%} exhibiting clear rotation out to several kpc, and 3/28 = 11{\$}\backslash{\$}pm6{\%} being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly {\$\sim${}}10{\^{}}5M{\_}sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A and Blakeslee, John P and Goulding, Andy D and McConnell, Nicholas J and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{VanDeVoort2011, -abstract = {(Abridged) We study the rate at which gas accretes onto galaxies and haloes and investigate whether the accreted gas was shocked to high temperatures before reaching a galaxy. For this purpose we use a suite of large cosmological, hydrodynamical simulations from the OWLS project. We improve on previous work by considering a wider range of halo masses and redshifts, by distinguishing accretion onto haloes and galaxies, by including important feedback processes, and by comparing simulations with different physics. The specific rate of gas accretion onto haloes is, like that for dark matter, only weakly dependent on halo mass. For halo masses Mhalo>>10^11 Msun it is relatively insensitive to feedback processes. In contrast, accretion rates onto galaxies are determined by radiative cooling and by outflows driven by supernovae and active galactic nuclei. Galactic winds increase the halo mass at which the central galaxies grow the fastest by about two orders of magnitude to Mhalo$\sim$10^12 Msun. Gas accretion is bimodal, with maximum past temperatures either of order the virial temperature or <$\sim$10^5 K. The fraction of gas accreted on to haloes in the hot mode is insensitive to feedback and metal-line cooling. It increases with decreasing redshift, but is mostly determined by halo mass, increasing gradually from less than 10% for $\sim$10^11 Msun to greater than 90% at 10^13 Msun. In contrast, for accretion onto galaxies the cold mode is always significant and the relative contributions of the two accretion modes are more sensitive to feedback and metal-line cooling. The majority of stars present in any mass halo at any redshift were formed from gas accreted in the cold mode, although the hot mode contributes typically over 10% for Mhalo>$\sim$10^11 Msun. Galaxies, but not necessarily their gaseous haloes, are predominantly fed by gas that did not experience an accretion shock when it entered the host halo.}, -archivePrefix = {arXiv}, -arxivId = {1011.2491}, -author = {van de Voort, Freeke and Schaye, Joop and Booth, C. M. and Haas, Marcel R. and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2011.18565.x}, -eprint = {1011.2491}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Intergalactic medium}, -month = {jul}, -number = {3}, -pages = {2458--2478}, -title = {{The rates and modes of gas accretion on to galaxies and their gaseous haloes}}, -volume = {414}, -year = {2011} -} -@article{Liao2016, -abstract = {The standard galaxy formation theory assumes that baryons and dark matter are initially well mixed before becoming segregated due to radiative cooling. We use non-radiative hydrodynamical simulations to explicitly examine this assumption and find that baryons and dark matter can also be segregated due to different characteristics of gas and dark matter during the buildup of the halo. As a result, baryons in many haloes do not originate from the same Lagrangian region as the dark matter. When using the fraction of corresponding dark matter and gas particles in the initial conditions (the 'paired fraction') as a proxy of the dark matter and gas segregation strength of a halo, on average about 25 per cent of the baryonic and dark matter of the final halo are segregated in the initial conditions. This is at odds with the assumption of the standard galaxy formation model. A consequence of this effect is that the baryons and dark matter of the same halo initially experience different tidal torques and thus their angular momentum vectors are often misaligned. The degree of the misalignment is largely preserved during later halo assembly and can be understood with the tidal torque theory. The result challenges the precision of some semi-analytical approaches that utilize dark matter halo merger trees to infer properties of gas associated with dark matter haloes.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.07592}, -author = {Liao, Shihong and Gao, Liang and Frenk, Carlos S. and Guo, Qi and Wang, Jie}, -doi = {10.1093/mnras/stx1391}, -eprint = {1610.07592}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Liao et al. - 2017 - The segregation of baryons and dark matter during halo assembly(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {2}, -pages = {2262--2269}, -title = {{The segregation of baryons and dark matter during halo assembly}}, -url = {http://arxiv.org/abs/1610.07592}, -volume = {470}, -year = {2017} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a {\$}\backslashLambda{\$}CDM concordance cosmology. To that extent we use a large {\$}N{\$}-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as function of halo mass and galaxy color. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by {\$}\backslashsim 40{\^{}}{\{}\backslashcirc{\}}{\$} (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the color of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the color of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X and {Van Den Bosch}, Frank C and Yang, Xiaohu and Mao, Shude and Mo, H J and Li, Cheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@article{Vika2013, -abstract = {We demonstrate a new multiwavelength technique for two-dimensional parametric modelling of galaxy surface-brightness profiles,which we have incorporated into thewidely used software GALFIT. Our newmethod, named GALFITM, extends GALFIT3's current single-band fitting process by simultaneously using multiple images of the same galaxy to constrain a wavelengthdependent model. Each standard profile parameter may vary as a function of wavelength, with a user-definable degree of smoothness, from constant to fully free. The performance of GALFITM is evaluated by fitting elliptical S{\'{e}}rsic profiles to ugriz imaging data for 4026 galaxies, comprising the original Sloan Digital Sky Survey (SDSS) imaging for 163 lowredshift (v < 7000 km s-1) galaxies and 3863 artificially redshifted (0.01 < z < 0.25) images of the same galaxies. Comparing results from single-band and multiband techniques, we show that GALFITM significantly improves the extraction of information, particularly from bands with low signal-to-noise ratio (e.g. u and z SDSS bands) when combined with higher signal-tonoise images.We also study systematic trends in the recovered parameters, particularly S{\'{e}}rsic index, that appear when one performs measurements of the same galaxies at successively higher redshifts. We argue that it is vital that studies investigating the evolution of galaxy structure are careful to avoid or correct for these biases. The resulting multiband photometric structural parameters for our sample of 163 galaxies are provided. We demonstrate the importance of considering multiband measurements by showing that theS{\'{e}}rsic indices of spiral galaxies increase to redder wavelengths, as expected for composite bulge-disc systems. Finally, for the ellipticals in our sample, which should be well represented by single-S{\'{e}}rsic models, we compare our measured parameters to those from previous studies. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1307.4996}, -author = {Vika, Marina and Bamford, Steven P. and H{\"{a}}u{\ss}ler, Boris and Rojas, Alex L. and Borch, Andrea and Nichol, Robert C.}, -doi = {10.1093/mnras/stt1320}, -eprint = {1307.4996}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure,Methods: data analysis,Techniques: image processing}, -month = {oct}, -number = {1}, -pages = {623--649}, -title = {{MegaMorph-Multiwavelength measurement of galaxy structure. S{\'{e}}rsic profile fits to galaxies near and far}}, -volume = {435}, -year = {2013} -} -@article{Lilly2016, -abstract = {There are very strong observed correlations between the specific star-formation rates (sSFR) of galaxies and their mean surface mass densities, {\{}$\backslash$Sigma{\}}, as well as other aspects of their internal structure. These strong correlations have often been taken to indicate that the internal structure of a galaxy must play a major physical role, directly or indirectly, in the control of star-formation. In this paper we show by means of a very simple toy model that these correlations can arise naturally without any such physical role once the observed evolution of the size-mass relation for star-forming galaxies is taken into account. In particular, the model reproduces the sharp threshold in {\{}$\backslash$Sigma{\}} between galaxies that are star-forming and those that are quenched, and the evolution of this threshold with redshift. Similarly, it produces iso-quenched-fraction contours in the {\$}{\{}f{\_}Q(m,R{\_}e){\}}{\$} plane that are almost exactly parallel to lines of constant {\{}$\backslash$Sigma{\}} for centrals and shallower for satellites. It does so without any dependence on quenching on size or {\{}$\backslash$Sigma{\}}, and without invoking any differences between centrals and satellites, beyond the different mass-dependences of their quenching laws. The toy-model also reproduces several other observations, including the sSFR gradients within galaxies and the appearance of inside-out build-up of passive galaxies. Finally, it is shown that curvature in the Main Sequence sSFR-mass relation can produce curvature in the apparent B/T ratios with mass. Our analysis therefore suggests that many of the strong correlations that are observed between galaxy structure and sSFR may well be a consequence of things unrelated to quenching and should not be taken as evidence of the physical processes that drive quenching.}, -archivePrefix = {arXiv}, -arxivId = {1604.06459}, -author = {Lilly, Simon J and Carollo, C Marcella}, -doi = {10.3847/0004-637x/833/1/1}, -eprint = {1604.06459}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {1}, -pmid = {15540530}, -title = {{Surface Density Effects in Quenching: Cause or Effect?}}, -url = {http://arxiv.org/abs/1604.06459%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/833/1/1}, -volume = {833}, -year = {2016} -} -@article{Tonini2006, -abstract = {We propose that angular momentum transfer from the baryons to the dark matter (DM) during the early stages of galaxy formation can flatten the halo inner density profile and modify the halo dynamics. We compute the phase-space distribution function of DM halos that corresponds to the density and anisotropy profiles obtained from N-body simulations in the concordance cosmology. We then describe an injection of angular momentum into the halo by modifying the distribution function and show that the system evolves into a new equilibrium configuration; the latter features a constant central density and a tangentially dominated anisotropy profile in the inner regions, while the structure is nearly unchanged beyond 10% of the virial radius. Then we propose a toy model to account for such a halo evolution, based on the angular momentum exchange due to dynamical friction; at the epoch of galaxy formation this is efficiently exerted by the DM onto the gas clouds spiralling down the potential well. The comparison between the angular momentum profile gained by the halo through dynamical friction and that provided by the perturbed distribution function reveals a surprising similarity, hinting at the reliability of the process. {\textcopyright} 2006. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0603051}, -author = {Tonini, C. and Lapi, A. and Salucci, P.}, -doi = {10.1086/506431}, -eprint = {0603051}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {591--598}, -primaryClass = {astro-ph}, -title = {{Angular Momentum Transfer in Dark Matter Halos: Erasing the Cusp}}, -url = {http://stacks.iop.org/0004-637X/649/i=2/a=591}, -volume = {649}, -year = {2006} -} -@article{Veale2016, -abstract = {We present spatially resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (ETGs; MK ≲ -25.7 mag, stellar mass M* ≳ 1011.8 M⊙) of the volumelimited (D {\textless} 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650-5850 {\AA}from the 246-fibre Mitchell integral-field spectrograph at McDonald Observatory, covering a 107 arcsec×107 arcsec field of view(often reaching 2 to 3 effective radii).We measure the 2D spatial distribution of each galaxy's angular momentum ($\lambda$ and fast or slow rotator status), velocity dispersion ($\sigma$), and higher order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ({\$\sim${}}80 per cent) of slow and non-rotators with $\lambda$ ≲ 0.2. When combined with the lower mass ETGs in the ATLAS3D survey, we find the fraction of slow rotators to increase dramatically with galaxy mass, reaching {\$\sim${}}50 per cent at MK {\$\sim${}} -25.5 mag and {\$\sim${}}90 per cent at MK ≲ -26 mag. All of our fast rotators show a clear anticorrelation between h3 and V/$\sigma$, and the slope of the anticorrelation is steeper in more round galaxies. The radial profiles of s show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK ≲ -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat s profiles, whereas five of the seven 'isolated' galaxies are all fainter than MK = -25.8 mag and have falling $\sigma$. All of our galaxies have positive average h4; the most luminous galaxies have average h4 {\$\sim${}} 0.05, while less luminous galaxies have a range of values between 0 and 0.05. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising s profiles. We discuss the implications for the relationship among dynamical mass, $\sigma$, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E and McConnell, Nicholas J and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Report2011, -abstract = {Modelling students' behaviour in relation to tuition fees is a complex task since students' 'talent' is not common knowledge. Students observe a private noisy signal of their abilities, while university receives noisy information based on the quantitative and qualitative data provided by university applicants. In this article, we add the heterogeneity of the population to this model: we assume that this heterogeneity means that the perception of skills among a part of the population is biased and underestimates the capabilities of its members to succeed in the higher education system. Our conclusions differ from those derived in the literature and show in particular that the optimal tuition fees for a given number of students are lower than those obtained for a homogeneous population. {\textcopyright}2013 Copyright Taylor and Francis Group, LLC.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-$\alpha$ emission from the host galaxy of SDSS$\sim$J2222+2745, a strongly lensed quasar at $z = 2.8$. Spectroscopic follow-up clearly reveals extended Lyman-$\alpha$ in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as $\sim$200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-$\alpha$ emission to its physical origin on one side of the host galaxy at radii $\sim$0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-$\alpha$ and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-$\alpha$, host galaxy Lyman-$\alpha$, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B. and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D. and Rigby, Jane R. and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bayliss et al. - 2017 - Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy(2).pdf:pdf}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Bolton2008b, -abstract = {We use a sample of 53 massive early-type strong gravitational lens galaxies with well-measured redshifts (ranging from z=0.06 to 0.36) and stellar velocity dispersions (between 175 and 400 km/s) from the Sloan Lens ACS (SLACS) Survey to derive numerous empirical scaling relations. The ratio between central stellar velocity dispersion and isothermal lens-model velocity dispersion is nearly unity within errors. The SLACS lenses define a fundamental plane (FP) that is consistent with the FP of the general population of early-type galaxies. We measure the relationship between strong-lensing mass M_lens within one-half effective radius (R_e/2) and the dimensional mass variable M_dim = G^-1 sigma_e2^2 R_e/2 to be log_10 [M_lens/10^11 M_Sun] = (1.03 +/- 0.04) log_10 [M_dim/10^11 M_Sun] + (0.54 +/- 0.02) (where sigma_e2 is the projected stellar velocity dispersion within R_e/2). The near-unity slope indicates that the mass-dynamical structure of massive elliptical galaxies is independent of mass, and that the "tilt" of the SLACS FP is due entirely to variation in total (luminous plus dark) mass-to-light ratio with mass. Our results imply that dynamical masses serve as a good proxies for true masses in massive elliptical galaxies. Regarding the SLACS lenses as a homologous population, we find that the average enclosed 2D mass profile goes as log_10 [M( 20,000M⊙pc-2, which is in agreement with expections based on observations of galaxies that are much closer to the Earth.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0312136}, -author = {Winn, Joshua H. and Rusin, David and Kochanek, Christopher S.}, -doi = {10.1038/nature02279}, -eprint = {0312136}, -isbn = {0028-0836}, -issn = {00280836}, -journal = {Nature}, -number = {6975}, -pages = {613--615}, -pmid = {14961114}, -primaryClass = {astro-ph}, -title = {{The central image of a gravitationally lensed quasar}}, -url = {http://arxiv.org/abs/astro-ph/0312136}, -volume = {427}, -year = {2004} -} -@article{Marinoni2016, -abstract = {We present the results of the short-term constancy monitoring of candidate GaiaSpectrophotometric Standard Stars (SPSS). We obtained time series of typically 1.24 h - with sampling periods from 1-3 min to a few hours, depending on the case - to monitor the constancy of our candidate SPSS down to 10 mmag, as required for the calibration of Gaia photometric data. We monitored 162 out of a total of 212 SPSS candidates. The observing campaign started in 2006 and finished in 2015, using 143 observing nights on nine different instruments covering both hemispheres. Using differential photometry techniques, we built light curves with a typical precision of 4 mmag, depending on the data quality. As a result of our constancy assessment, 150 SPSS candidates were validated against short-term variability, and only 12 were rejected because of variability including some widely used flux standards such as BD+174708, SA 105-448, 1740346, and HD 37725.}, -archivePrefix = {arXiv}, -arxivId = {1608.00759}, -author = {Marinoni, S. and Pancino, E. and Altavilla, G. and Bellazzini, M. and Galleti, S. and Tessicini, G. and Valentini, G. and Cocozza, G. and Ragaini, S. and Braga, V. and Bragaglia, A. and Federici, L. and Schuster, W. J. and Carrasco, J. M. and Castro, A. and Figueras, F. and Jordi, C.}, -doi = {10.1093/mnras/stw1886}, -eprint = {1608.00759}, -isbn = {9788578110796}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Binaries: general,Stars: variables: general,Techniques: photometric}, -number = {4}, -pages = {3616--3627}, -pmid = {25246403}, -title = {{The Gaia spectrophotometric standard stars survey - III. Short-term variability monitoring}}, -url = {http://arxiv.org/abs/1608.00759%5Cnhttp://dx.doi.org/10.1093/mnras/stw1886}, -volume = {462}, -year = {2016} -} -@article{Spingola2019, -abstract = {Gravitational lensing is a powerful tool for quantifying the mass content and distribution in distant galaxies. By using milliarcsecond angular resolution observations of radio-loud gravitationally lensed sources it is also possible to detect and quantify small deviations from a smooth mass density distribution, which can be due to low mass substructures in the lensing galaxy. We present high-resolution global VLBI observations of the gravitationally lensed radio source MG J0751+2716 (at z = 3.2), that shows evidence of both compact and extended structure (core-jet morphology) across several gravitational arcs. These data provide a wealth of observational constraints that are used to determine the inner (baryonic and dark matter) mass profile of a group of galaxies and also investigate the smoothness of the dark matter distribution on mas-scales, which is sensitive to possible structures of 106-7 M within the lensing halo or along the line-of-sight. Our lens modelling finds evidence for astrometric anomalies in this system, which suggest presence of extra mass structure in the lens model. To date this kind of detailed studies of gravitational lensing systems like MG J0751+2716 has been limited by the currently small sample of radioloud gravitational lenses. In this context, we also present a new pilot gravitational lens search in the VLBI survey mJIVE-20, in perspective of future surveys with the next generation of radio interferometers.}, -archivePrefix = {arXiv}, -arxivId = {1902.07046}, -author = {Spingola, C. and McKean, J. P. and Deller, A. and Moldon, J.}, -doi = {10.22323/1.344.0033}, -eprint = {1902.07046}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Spingola2019SMBHVLBI.pdf:pdf}, -issn = {23318422}, -journal = {arXiv}, -number = {October}, -pages = {8--11}, -title = {{Gravitational lensing at milliarcsecond angular resolution with VLBI observations}}, -year = {2019} -} -@article{Pulsoni2017, -abstract = {Wolbachia is an intracellular endosymbiont that induces a variety of reproductive alterations in diverse arthropods. The almond moth, Cadra cautella, is double infected with two Wolbachia variants, wCauA and wCauB, and expresses complete cytoplasmic incompatibility (CI). The individual contribution of wCauA and wCauB to the expression of CI are unclear, however, because the two variants have not been separated in this host. The effect of wCauA is of particular interest because it induces male killing when transferred into the Mediterranean flour moth, Ephestia kuehniella. In the present study, we generated C. cautella infected with only wCauA by treating double-infected insects with tetracycline. Single-infected C. cautella exhibited strong CI, demonstrating that wCauA induces two distinct reproductive phenotypes in different hosts: CI in C. cautella and male killing in E. kuehniella. CI was also observed in the cross of double-infected males and single-infected females. Comparison of the single- and double-infected insects by real-time quantitative polymerase chain reaction suggested that the wCauA density is not affected much by the presence or absence of wCauB.}, -archivePrefix = {arXiv}, -arxivId = {http://www.R-project.org}, -author = {Sasaki, T and Massaki, N and Kubo, T}, -doi = {10.1038/sj.hdy.6800737}, -eprint = {/www.R-project.org}, -isbn = {0018-067X}, -issn = {0018-067X}, -journal = {Heredity}, -keywords = {Cadra cautella,Cytoplasmic incompatibility,Double infection,Male killing,Real-time quantitative PCR,Wolbachia}, -number = {5}, -pages = {389--393}, -pmid = {16106260}, -primaryClass = {http:}, -title = {{Wolbachia variant that induces two distinct reproductive phenotypes in different hosts.}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/16106260}, -volume = {95}, -year = {2005} -} -@article{Brainerd2005, -abstract = {The distribution of satellite galaxies relative to isolated host galaxies in the Sloan Digital Sky Survey (SDSS) is investigated. Host-satellite systems are selected using three different methods, yielding samples of {\$\sim${}}3300, {\$\sim${}}1600, and {\$\sim${}}950 satellites. In the plane of the sky, the distributions of all three samples show highly significant deviations from circular symmetry ({\textgreater}99.99{\%}, {\textgreater}99.99{\%}, and 99.79{\%} confidence levels, respectively), and the degree of anisotropy is a strong function of the projected radius, r p , at which the satellites are found. For r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 100 kpc, the SDSS satellites are aligned preferentially with the major axes of the hosts. This is in stark contrast to the Holmberg effect, in which satellites are aligned with the minor axes of host galaxies. The degree of anisotropy in the distribution of the SDSS satellites decreases with r p and is consistent with an isotropic distribution at of order the 1 $\sigma$ level for 250 kpc {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 500 kpc.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408559}, -author = {Brainerd, Tereasa G}, -doi = {10.1086/432713}, -eprint = {0408559}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L101----L104}, -primaryClass = {astro-ph}, -title = {{Anisotropic Distribution of SDSS Satellite Galaxies: Planar (Not Polar) Alignment}}, -url = {http://stacks.iop.org/1538-4357/628/i=2/a=L101}, -volume = {628}, -year = {2005} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless}M{\_}200b {\textless}10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater}10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20{\$}\backslash{\$}{\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, Jenny E and Leauthaud, Alexie and Emsellem, Eric and Ge, J and Arag'on-Salamanca, A and Greco, J P and Lin, Y -T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -pages = {1--23}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -year = {2017} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ($\rho\sim r^{-\gamma}$), we find that, although the zero cosmic curvature is still included within $2 \sigma$ confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile $\rho\sim r^{-\alpha}$ to be different from that of the total-mass density profile $\nu\sim r^{-\delta}$, a weaker constraint on the curvature ($\Omega_k<0.197$ at 68\% confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of $\Delta \Omega_k\simeq 10^{-3}$, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Qi et al. - 2018 - A revised test of cosmic curvature at high redshifts the distance sum rule(2).pdf:pdf}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{Buitrago2017a, -abstract = {Using the exquisite depth of the Hubble Ultra Deep Field (HUDF12 programme) data set, we explore the ongoing assembly of the outermost regions of the most massive galaxies (Mstellar ≥ 5× 1010 M) at z ≤ 1. The outskirts of massive objects, particularly early-type Galaxies (ETGs), are expected to suffer a dramatic transformation across cosmic time due to continuous accretion of small galaxies. HUDF imaging allows us to study this process at intermediate redshifts in six massive galaxies, exploring the individual surface brightness profiles out to ∼25 effective radii. We find that 5–20 per cent of the total stellar mass for the galaxies in our sample is contained within 10 {\textless} R {\textless} 50 kpc. These values are in close agreement with numerical simulations, and higher than those reported for local late-type galaxies (5 per cent). The fraction of stellar mass stored in the outer envelopes/haloes of massive ETGs increases with decreasing redshift, being 28.7 per cent at {\textless}z {\textgreater}= 0.1, 15.1 per cent at {\textless}z {\textgreater}= 0.65 and 3.5 per cent at {\textless}z {\textgreater}= 2. The fraction of mass in diffuse features linked with ongoing minor merger events is {\textgreater}1–2 per cent, very similar to predictions based on observed close pair counts. Therefore, the results for our small albeit meaningful sample suggest that the size and mass growth of the most massive galaxies have been solely driven by minor and major merging from z = 1 to today.}, -archivePrefix = {arXiv}, -arxivId = {1602.01846}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Curtis-Lake, Emma and Montes, Mireia and Cooper, Andrew P and Bruce, Victoria A and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Cirasuolo, Michele}, -doi = {10.1093/mnras/stw3382}, -eprint = {1602.01846}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: haloes,Galaxies: high-redshift,Galaxies: structure,cD}, -number = {4}, -pages = {4888--4903}, -title = {{The cosmic assembly of stellar haloes in massive early-type Galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3382}, -volume = {466}, -year = {2017} -} -@article{Bullock2005a, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print)$\backslash$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Ferrero2017, -abstract = {The Tully-Fisher relation (TFR) links the stellar mass of a disk galaxy, {\$}M{\_}{\{}\backslashbackslashrm str{\}}{\$}, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling ({\$}M\backslashbackslashpropto V{\^{}}3{\$}) of dark matter halos, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to be non-monotonic and rapidy evolving. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM cosmological simulations. Matching both relations requires disk sizes to satisfy constraints given by the concentration of halos and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to {\$}z=1{\$}. {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1607.03100}, -author = {Ferrero, Ismael and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw2691}, -eprint = {1607.03100}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {4}, -pages = {4736--4746}, -title = {{Size matters: Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE}}, -volume = {464}, -year = {2017} -} -@article{Veale2017a, -abstract = {We analyse the environmental properties of 370 local early-type galaxies (ETGs) in theMASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute K-band magnitude -21.5 ≳ MK ≳ -26.6, or stellar mass 8 × 109 ≲ M* ≲ 2 × 1012M⊙. We find these galaxies to reside in a diverse range of environments measured by four methods: group membership (whether a galaxy is a brightest group/cluster galaxy, satellite or isolated), halo mass, large-scale mass density (measured over a fewMpc) and local mass density (measured within the Nth neighbour). The spatially resolved IFS stellar kinematics provide robust measurements of the spin parameter $\lambda$e and enable us to examine the relationship among $\lambda$e, M* and galaxy environment. We find a strong correlation between $\lambda$e and M*, where the average $\lambda$e decreases from $\sim$0.4 to below 0.1 with increasing mass, and the fraction of slow rotators fslow increase from $\sim$10 to 90 per cent. We show for the first time that at fixed M*, there are almost no trends between galaxy spin and environment; the apparent kinematic morphology-density relation for ETGs is therefore primarily driven by M* and is accounted for by the joint correlations between M* and spin, and between M* and environment. A possible exception is that the increased fslow at high local density is slightly more than expected based only on these joint correlations. Our results suggest that the physical processes responsible for building up the present-day stellar masses of massive galaxies are also very efficient at reducing their spin, in any environment.}, -archivePrefix = {arXiv}, -arxivId = {1703.08573}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E. and Thomas, Jens and Blakeslee, John P. and McConnell, Nicholas and Walsh, Jonelle L. and Ito, Jennifer}, -doi = {10.1093/mnras/stx1639}, -eprint = {1703.08573}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Veale et al. - 2017 - The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxie.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {1428--1445}, -title = {{The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxies}}, -url = {http://arxiv.org/abs/1703.08573%0Ahttp://dx.doi.org/10.1093/mnras/stx1639}, -volume = {471}, -year = {2017} -} -@article{Boylan-Kolchin:2006aa, -abstract = {Several recent observations suggest that gas-poor (dissipationless) mergers of elliptical galaxies contribute significantly to the build-up of the massive end of the red sequence at z ≲ 1. We perform a series of major merger simulations to investigate the spatial and velocity structure of the remnants of such mergers. Regardless of orbital energy or angular momentum, we find that the stellar remnants lie on the fundamental plane defined by their progenitors, a result of virial equilibrium with a small tilt due to an increasing central dark matter fraction. However, the locations of merger remnants in the projections of the fundamental plane - the Faber-Jackson and R e-M* relations - depend strongly on the merger orbit, and the relations steepen significantly from the canonical scalings ( and ) for mergers on radial orbits. This steepening arises because stellar bulges on orbits with lower angular momentum lose less energy via dynamical friction on the dark matter haloes than do bulges on orbits with substantial angular momentum. This results in a less tightly bound remnant bulge with a smaller velocity dispersion and a larger effective radius. Our results imply that the projections of the fundamental plane - but not necessarily the plane itself - provide a powerful way of investigating the assembly history of massive elliptical galaxies, including the brightest cluster galaxies at or near the centres of galaxy clusters. We argue that most massive ellipticals are formed by anisotropic merging and that their fundamental plane projections should thus differ noticeably from those of lower mass ellipticals even though they should lie on the same fundamental plane. Current observations are consistent with this conclusion. The steepening in the L-$\sigma$e relation for luminous ellipticals may also be reflected in a corresponding steepening in the M BH-$\sigma$e relation for massive black holes. {\textcopyright} 2006 RAS.}, -author = {Boylan-Kolchin, Michael and Ma, Chung Pei and Quataert, Eliot}, -doi = {10.1111/j.1365-2966.2006.10379.x}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Boylan-Kolchin, Ma, Quataert - 2006 - Red mergers and the assembly of massive elliptical galaxies The fundamental plane and its projecti.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters}, -month = {jul}, -number = {3}, -pages = {1081--1089}, -title = {{Red mergers and the assembly of massive elliptical galaxies: The fundamental plane and its projections}}, -volume = {369}, -year = {2006} -} -@article{Casey2023, -abstract = {We present the survey design, implementation, and outlook for COSMOS-Web, a 255 hr treasury program conducted by the James Webb Space Telescope in its first cycle of observations. COSMOS-Web is a contiguous 0.54 deg 2 NIRCam imaging survey in four filters (F115W, F150W, F277W, and F444W) that will reach 5 $\sigma$ point-source depths ranging ∼27.5–28.2 mag. In parallel, we will obtain 0.19 deg 2 of MIRI imaging in one filter (F770W) reaching 5 $\sigma$ point-source depths of ∼25.3–26.0 mag. COSMOS-Web will build on the rich heritage of multiwavelength observations and data products available in the COSMOS field. The design of COSMOS-Web is motivated by three primary science goals: (1) to discover thousands of galaxies in the Epoch of Reionization (6 ≲ z ≲ 11) and map reionization's spatial distribution, environments, and drivers on scales sufficiently large to mitigate cosmic variance, (2) to identify hundreds of rare quiescent galaxies at z > 4 and place constraints on the formation of the universe's most-massive galaxies ( M ⋆ > 10 10 M ⊙ ), and (3) directly measure the evolution of the stellar-mass-to-halo-mass relation using weak gravitational lensing out to z ∼ 2.5 and measure its variance with galaxies' star formation histories and morphologies. In addition, we anticipate COSMOS-Web's legacy value to reach far beyond these scientific goals, touching many other areas of astrophysics, such as the identification of the first direct collapse black hole candidates, ultracool subdwarf stars in the Galactic halo, and possibly the identification of z > 10 pair-instability supernovae. In this paper we provide an overview of the survey's key measurements, specifications, goals, and prospects for new discovery.}, -archivePrefix = {arXiv}, -arxivId = {2211.07865}, -author = {Casey, Caitlin M. and Kartaltepe, Jeyhan S. and Drakos, Nicole E. and Franco, Maximilien and Harish, Santosh and Paquereau, Louise and Ilbert, Olivier and Rose, Caitlin and Cox, Isabella G. and Nightingale, James W. and Robertson, Brant E. and Silverman, John D. and Koekemoer, Anton M. and Massey, Richard and McCracken, Henry Joy and Rhodes, Jason and Akins, Hollis B. and Allen, Natalie and Amvrosiadis, Aristeidis and Arango-Toro, Rafael C. and Bagley, Micaela B. and Bongiorno, Angela and Capak, Peter L. and Champagne, Jaclyn B. and Chartab, Nima and {Ch{\'{a}}vez Ortiz}, {\'{O}}scar A. and Chworowsky, Katherine and Cooke, Kevin C. and Cooper, Olivia R. and Darvish, Behnam and Ding, Xuheng and Faisst, Andreas L. and Finkelstein, Steven L. and Fujimoto, Seiji and Gentile, Fabrizio and Gillman, Steven and Gould, Katriona M. L. and Gozaliasl, Ghassem and Hayward, Christopher C. and He, Qiuhan and Hemmati, Shoubaneh and Hirschmann, Michaela and Jahnke, Knud and Jin, Shuowen and Khostovan, Ali Ahmad and Kokorev, Vasily and Lambrides, Erini and Laigle, Clotilde and Larson, Rebecca L. and Leung, Gene C. K. and Liu, Daizhong and Liaudat, Tobias and Long, Arianna S. and Magdis, Georgios and Mahler, Guillaume and Mainieri, Vincenzo and Manning, Sinclaire M. and Maraston, Claudia and Martin, Crystal L. and McCleary, Jacqueline E. and McKinney, Jed and McPartland, Conor J. R. and Mobasher, Bahram and Pattnaik, Rohan and Renzini, Alvio and Rich, R. Michael and Sanders, David B. and Sattari, Zahra and Scognamiglio, Diana and Scoville, Nick and Sheth, Kartik and Shuntov, Marko and Sparre, Martin and Suzuki, Tomoko L. and Talia, Margherita and Toft, Sune and Trakhtenbrot, Benny and Urry, C. Megan and Valentino, Francesco and Vanderhoof, Brittany N. and Vardoulaki, Eleni and Weaver, John R. and Whitaker, Katherine E. and Wilkins, Stephen M. and Yang, Lilan and Zavala, Jorge A.}, -doi = {10.3847/1538-4357/acc2bc}, -eprint = {2211.07865}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Casey2022COSMOSWebOverview.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -number = {1}, -pages = {31}, -title = {{COSMOS-Web: An Overview of the JWST Cosmic Origins Survey}}, -volume = {954}, -year = {2023} -} -@article{Blumenthal1986, -abstract = {Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in. radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.}, -author = {Blumenthal, G. R. and Faber, S. M. and Flores, R. and Primack, J. R.}, -doi = {10.1086/163867}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -pages = {27}, -title = {{Contraction of dark matter galactic halos due to baryonic infall}}, -volume = {301}, -year = {1986} -} -@article{deNaray2008, -abstract = {We present high-resolution optical velocity fields from DensePak integral field spectroscopy, along with derived rotation curves, for a sample of low surface brightness galaxies. In the limit of no baryons, we fit the NFW and pseudoisothermal halo models to the data and find the rotation curve shapes and halo central densities to be better described by the isothermal halo. For those galaxies with photometry, we present halo fits for three assumptions of the stellar mass-to-light ratio. We find that the velocity contribution from the baryons is significant enough in the maximum disk case that maximum disk and the NFW halo are mutually exclusive. We find a substantial cusp mass excess at the centers of the galaxies, with at least two times more mass expected in the cuspy CDM halo than is allowed by the data. We also find that to reconcile the data with LCDM, {\$\sim${}}20 km/s noncircular motions are needed and/or the power spectrum has a lower amplitude on the scales we probe.}, -archivePrefix = {arXiv}, -arxivId = {0712.0860}, -author = {de Naray, Rachel Kuzio and McGaugh, Stacy S and de Blok, W J G}, -doi = {10.1086/527543}, -eprint = {0712.0860}, -issn = {0004-637X}, -journal = {$\backslash$Apj}, -keywords = {Cosmology: Dark Matter,Galaxies: Fundamental Parameters,Galaxies: Kinematics and Dynamics}, -month = {apr}, -pages = {920--943}, -title = {{Mass Models for Low Surface Brightness Galaxies with High Resolution Optical Velocity Fields}}, -url = {http://arxiv.org/abs/0712.0860%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/527543}, -volume = {676}, -year = {2007} -} -@article{Gow2016, -abstract = {{\textcopyright}2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P D and Murray, Neil J}, -doi = {10.1117/12.2232706}, -isbn = {9781510602090}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{Lauer2005, -abstract = {We present observations of 77 early-type galaxies imaged with the PC1 CCD of the Hubble Space Telescope (HST) WFPC2. "Nuker-law" parametric fits to the surface brightness profiles are used to classify the central structure into "core" or "power-law" forms. Core galaxies are typically rounder than power-law galaxies. Nearly all power-law galaxies with central ellipticities $\epsilon$ ≥ 0.3 have stellar disks, implying that disks are present in power-law galaxies with $\epsilon$ {\textless} 0.3 but are not visible because of unfavorable geometry. A few low-luminosity flattened core galaxies also have disks; these may be transition forms from power-law galaxies to more luminous core galaxies, which lack disks. Several core galaxies have strong isophote twists interior to their break radii, although power-law galaxies have interior twists of similar physical significance when the photometric perturbations implied by the twists are evaluated. Central color gradients are typically consistent with the envelope gradients; core galaxies have somewhat weaker color gradients than power-law galaxies. Nuclei are found in 29{\%} of the core galaxies and 60{\%} of the power-law galaxies. Nuclei are typically bluer than the surrounding galaxy. While some nuclei are associated with active galactic nuclei (AGNs), just as many are not; conversely, not all galaxies known to have a low-level AGN exhibit detectable nuclei in the broadband filters. NGC 4073 and 4382 are found to have central minima in their intrinsic starlight distributions; NGC 4382 resembles the double nucleus of M31. In general, the peak brightness location is coincident with the photocenter of the core to a typical physical scale of {\textless} 1 pc. Five galaxies, however, have centers significantly displaced from their surrounding cores; these may be unresolved asymmetric double nuclei. Finally, as noted by previous authors, central dust is visible in about half of the galaxies. The presence and strength of dust correlates with nuclear emission; thus, dust may outline gas that is falling into the central black hole. The prevalence of dust and its morphology suggest that dust clouds form, settle to the center, and disappear repeatedly on ∼ 10 8 yr timescales. We discuss the hypothesis that cores are created by the decay of a massive black hole binary formed in a merger. Apart from their brightness profiles, there are no strong differences between core galaxies and power-law galaxies that demand this scenario; however, the rounder shapes of core, their lack of disks, and their reduced color gradients may be consistent with it. {\textcopyright}2005. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0412040}, -author = {Lauer, Tod R and Faber, S M and Gebhardt, Karl and Richstone, Douglas and Tremaine, Scott and Ajhar, Edward A and Aller, M C and Bender, Ralf and Dressler, Alan and Filippenko, Alexei V and Green, Richard and Grillmair, Carl J and Ho, Luis C and Kormendy, John and Magorrian, John and Pinkney, Jason and Siopis, Christos}, -doi = {10.1086/429565}, -eprint = {0412040}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2138--2185}, -primaryClass = {arXiv:astro-ph}, -title = {{ The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry }}, -url = {http://stacks.iop.org/1538-3881/129/i=5/a=2138}, -volume = {129}, -year = {2005} -} -@article{Auger2009a, -abstract = {We use stellar masses, surface photometry, strong-lensing masses, and stellar velocity dispersions ($\sigma$e/2) to investigate empirical correlations for the definitive sample of 73 early-type galaxies (ETGs) that are strong gravitational lenses from the SLACS survey. The traditional correlations (fundamental plane (FP) and its projections) are consistent with those found for non-lens galaxies, supporting the thesis that SLACS lens galaxies are representative of massive ETGs (dimensional massMdim = 1011-1012 M⊙). The addition of high-precision stronglensing estimates of the total mass allows us to gain further insights into their internal structure: (1) the average slope of the total mass-density profile ($\rho$tot $\alpha$ r-$\gamma$') is ($\gamma$') = 2.078 ± 0.027 with an intrinsic scatter of 0.16 ± 0.02; (2) $\gamma$' correlates with effective radius (re) and central mass density, in the sense that denser galaxies have steeper profiles; (3) the dark matter (DM) fraction within r e/2 is a monotonically increasing function of galaxy mass and size (due to a mass-dependent central cold DM distribution or due to baryonic DM-stellar remnants or low-mass stars-if the initial mass function is non-universal and its normalization increases with mass); (4) the dimensional mass Mdim = 5re$\sigma$e/22/G is proportional to the total (lensing) mass Mre/2, and both increase more rapidly than stellar mass M* (M* $\alpha$ M0.8re/2); (5) the mass plane (MP), obtained by replacing surface brightness with surface mass density in the FP, is found to be tighter and closer to the virial relation than the FP and the M *.P, indicating that the scatter of those relations is dominated by stellar population effects; (6) we construct the fundamental hyper-plane by adding stellar masses to the MP and find the M* coefficient to be consistent with zero and no residual intrinsic scatter. Our results demonstrate that the dynamical structure of ETGs is not scale invariant and that it is fully specified by Mre/2, re, and $\sigma$e/2. Although the basic trends can be explained qualitatively in terms of varying star formation efficiency as a function of halo mass and as the result of dry and wet mergers, reproducing quantitatively the observed correlations and their tightness may be a significant challenge for galaxy formation models.}, -archivePrefix = {arXiv}, -arxivId = {1007.2880}, -author = {Auger, M. W. and Treu, T. and Bolton, A. S. and Gavazzi, R. and Koopmans, L. V.E. and Marshall, P. J. and Moustakas, L. A. and Burles, S.}, -doi = {10.1088/0004-637X/724/1/511}, -eprint = {1007.2880}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {CD,Dark matter,Galaxies: elliptical and lenticular,Galaxies: fundamental parameters,Galaxies: structure,Gravitational lensing: strong}, -number = {1}, -pages = {511--525}, -title = {{The sloan lens ACS survey. X. Stellar, dynamical, and total mass correlations of massive early-type galaxies}}, -url = {http://stacks.iop.org/0004-637X/724/i=1/a=511?key=crossref.2a8f66f24819ad7316941c9449a63c7f}, -volume = {724}, -year = {2010} -} -@article{Oriordan2020, -abstract = {We present a systematic analysis of the constraints $\sigma$$\gamma$ on the mass profile slope $\gamma$ obtainable when fitting a singular power-law ellipsoid model to a typical strong lensing observation of an extended source. These results extend our previous analysis of circular systems, Paper I. We draw our results from 676 mock observations covering a range of image configurations, each created with a fixed signal to noise ratio S = 100 in the images. We analyse the results using a combination of theory and a simplified model which identifies the contribution to the constraints of the individual fluxes and positions in each of the lensed images. The main results are: 1. For any lens ellipticity, the constraints $\sigma$$\gamma$ for two image systems are well described by the results of Paper I, transformed to elliptical coordinates; 2. We derive an analytical expression for $\sigma$$\gamma$ for systems with the source aligned with the axis of the lens; 3. For both two-image systems and aligned systems, $\sigma$$\gamma$ is limited by the flux uncertainties; 4. The constraints for off-axis four-image systems are a factor of two to eight better, depending on source size, than for two-image systems, and improve with increasing lens ellipticity. We show that the constraints on $\gamma$ in these systems derive from the complementary positional information of the images alone, without using flux. The complementarity improves as the offset of the source from the axis increases, such that the best constraints $\sigma$$\gamma$ < 0.01, for S = 100, occur when the source approaches the caustic.}, -archivePrefix = {arXiv}, -arxivId = {2004.13435}, -author = {O'Riordan, C. M. and Warren, S. J. and Mortlock, D. J.}, -doi = {10.1093/mnras/staa1697}, -eprint = {2004.13435}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/ORiodan2020BPL2.pdf:pdf}, -journal = {MNRAS}, -keywords = {gravitational lensing: strong}, -number = {3}, -pages = {3424--3435}, -title = {{Galaxy mass profiles from strong lensing II: The elliptical power-law model}}, -volume = {496}, -year = {2020} -} -@article{Gnedin2004, -abstract = {The cooling of gas in the centers of dark matter halos is expected to lead to a more concentrated dark matter distribution. The response of dark matter to the condensation of baryons is usually calculated using the model of adiabatic contraction, which assumes spherical symmetry and circular orbits. In contrast, halos in the hierarchical structure formation scenarios grow via multiple violent mergers and accretion along filaments, and particle orbits in the halos are highly eccentric. We study the effects of the cooling of gas in the inner regions of halos using high-resolution cosmological simulations which include gas dynamics, radiative cooling, and star formation. We find that the dissipation of gas indeed increases the density of dark matter and steepens its radial profile in the inner regions of halos compared to the case without cooling. For the first time, we test the adiabatic contraction model in cosmological simulations and find that the standard model systematically overpredicts the increase of dark matter density in the inner 5% of the virial radius. We show that the model can be improved by a simple modification of the assumed invariant from M(r)r to M(r_av)r, where r and r_av are the current and orbit-averaged particle positions. This modification approximately accounts for orbital eccentricities of particles and reproduces simulation profiles to within 10-20%. We present analytical fitting functions that accurately describe the transformation of the dark matter profile in the modified model and can be used for interpretation of observations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0406247}, -author = {Gnedin, Oleg Y. and Kravtsov, Andrey V. and Klypin, Anatoly A. and Nagai, Daisuke}, -doi = {10.1086/424914}, -eprint = {0406247}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Theory,Galaxies: Formation,Galaxies: Halos,Methods: Numerical}, -month = {nov}, -number = {1}, -pages = {16--26}, -primaryClass = {astro-ph}, -title = {{Response of Dark Matter Halos to Condensation of Baryons: Cosmological Simulations and Improved Adiabatic Contraction Model}}, -url = {http://arxiv.org/abs/astro-ph/0406247%0Ahttp://dx.doi.org/10.1086/424914}, -volume = {616}, -year = {2004} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. with the particle-tagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of ˜1900 massive dark matter haloes (1012-1014M⊙) from the Millennium II $\Lambda$ cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of Milky Way-like galaxies to the `cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a S{\`{e}}rsic profile, the radial scale and amplitude of which vary systematically with halo mass (M200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M⋆ and M200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z ≈ 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly.}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S and White, Simon D M}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Strauss2002, -abstract = {We describe the algorithm for selecting quasar candidates for optical spectroscopy in the Sloan Digital Sky Survey. Quasar candidates are selected via their non-stellar colors in "ugriz" broad-band photometry, and by matching unresolved sources to the FIRST radio catalogs. The automated algorithm is sensitive to quasars at all redshifts lower than z=5.8. Extended sources are also targeted as low-redshift quasar candidates in order to investigate the evolution of Active Galactic Nuclei (AGN) at the faint end of the luminosity function. Nearly 95% of previously known quasars are recovered (based on 1540 quasars in 446 square degrees). The overall completeness, estimated from simulated quasars, is expected to be over 90%, whereas the overall efficiency (quasars:quasar candidates) is better than 65%. The selection algorithm targets ultraviolet excess quasars to i^*=19.1 and higher-redshift (z>3) quasars to i^*=20.2, yielding approximately 18 candidates per square degree. In addition to selecting ``normal'' quasars, the design of the algorithm makes it sensitive to atypical AGN such as Broad Absorption Line quasars and heavily reddened quasars.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202251}, -author = {Richards, Gordon T. and Fan, Xiaohui and Newberg, Heidi Jo and Strauss, Michael A. and {Vanden Berk}, Daniel E. and Schneider, Donald P. and Yanny, Brian and Boucher, Adam and Burles, Scott and Frieman, Joshua A. and Gunn, James E. and Hall, Patrick B. and Ivezi{\'{c}}, {\v{Z}}eljko and Kent, Stephen and Loveday, Jon and Lupton, Robert H. and Rockosi, Constance M. and Schlegel, David J. and Stoughton, Chris and SubbaRao, Mark and York, Donald G.}, -doi = {10.1086/340187}, -eprint = {0202251}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {10 5 quasars,10 6 galaxies and,Galaxies: Distances and Redshifts,Galaxies: Photometry,Surveys,complete within precisely defined,distances and redshifts,follow-up spec-,galactic cap and a,galaxies,photometry,selection criteria,steradians in the north,surveys,the,troscopic survey of roughly}, -number = {6}, -pages = {2945--2975}, -pmid = {16084653}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection in the Sloan Digital Sky Survey: The Quasar Sample}}, -url = {http://arxiv.org/abs/astro-ph/0202251%0Ahttp://dx.doi.org/10.1086/340187}, -volume = {123}, -year = {2002} -} -@article{Dekel2014, -abstract = {We study the origin of high-redshift, compact, quenched spheroids (red nuggets) through the dissipative shrinkage of gaseous discs into compact star-forming systems (blue nuggets). The discs, fed by cold streams, undergo violent disc instability that drives gas into the centre (along with mergers). The inflow is dissipative when its time-scale is shorter than the star formation time-scale. This implies a threshold of $\sim$0.28 in the cold-to-total mass ratio within the disc radius. For the typical gas fraction $\sim$0.5 at z $\sim$ 2, this threshold is traced back to a maximum spin parameter of $\sim$0.05, implying that $\sim$half the star-forming galaxies contract to blue nuggets, while the rest form extended stellar discs. Thus, the surface density of blue galaxies is expected to be bimodal about $\sim$109M⊙ kpc-2, slightly increasing with mass. The blue nuggets are expected to be rare at low z when the gas fraction is low. The blue nuggets quench to red nuggets by complementary internal and external mechanisms. Internal quenching by a compact bulge, in a fast mode and especially at high z, may involve starbursts, stellar and active galactic nucleus feedback, or Q-quenching. Quenching due to hot-medium haloes above 1012M⊙ provides maintenance and a slower mode at low redshift. These predictions are confirmed in simulations and are consistent with observations at z = 0-3. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1310.1074}, -author = {Dekel, A. and Burkert, A.}, -doi = {10.1093/mnras/stt2331}, -eprint = {1310.1074}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Spiral,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics}, -number = {2}, -pages = {1870--1879}, -title = {{Wet disc contraction to galactic blue nuggets and quenching to red nuggets}}, -url = {http://arxiv.org/abs/1310.1074%0Ahttp://dx.doi.org/10.1093/mnras/stt2331}, -volume = {438}, -year = {2014} -} -@article{Treu2004, -abstract = {(Shortened) The combination of lensing and stellar dynamics breaks the mass-anisotropy degeneracy and provides stringent constraints on the mass distribution in early-type (E/S0) galaxies out to z$\sim$1. We present the combined results from the five field E/S0 lens galaxies at z=0.5-1.0 analyzed as part of the LSD Survey. We find: (i) Constant M/L models are ruled out at >99% CL for all five E/S0s. The projected dark-matter mass fractions inside the Einstein (effective) radius is f_DM=0.37-0.72 (0.15-0.65) for isotropic models. (ii) The average power-law slope of the total mass distribution is <\gamma'>=1.75+-0.10 for isotropic models with 0.20 rms scatter. The ratio between the observed central stellar velocity dispersion and that from the best-fit SIE lens model is =<\sigma/\sigma_SIE>=0.87+-0.04 with 0.08 rms. Considering that \gamma'>2 and f_SIE>1 have been reported for other systems, we conclude that there is a significant intrinsic scatter in the density slopes of E/S0s (rms \$\sim$15%). Hence, the isothermal approximation is not sufficiently accurate for applications that depend critically on the slope of the mass density profile (i.e. measuring H_0). (iii) The inner power-law slope of the dark-matter halo is constrained to be <\gamma>=1.3(+0.2/-0.4) (68% CL) for the isotropic model or an upper limit of \gamma<0.6, if the galaxies are radially anisotropic (r_i=R_e). This is consistent with numerical simulations only for an isotropic velocity ellipsoid and if baryonic collapse and star-formation do not steepen dark-matter density profiles. (iv) The average stellar M/L evolves as d\log(M_*/L_B)/dz =-0.72+-0.10, obtained via the FP. Based on lensing and dynamics we find d\log(M_*/L_B)/dz=-0.75+-0.17, indicating that the M/L ratio evolution for our sample of field E/S0s is faster than those in clusters.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0401373}, -author = {Treu, Tommaso and Koopmans, Leon V. E.}, -doi = {10.1086/422245}, -eprint = {0401373}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Cosmology: Dark Matter,Galaxies: Elliptical and Lenticular,Galaxies: Structure,cD,galaxies: evolution,galaxies: formation}, -number = {2}, -pages = {739--760}, -primaryClass = {astro-ph}, -title = {{ Massive Dark Matter Halos and Evolution of Early‐Type Galaxies to z ≈ 1 }}, -url = {http://arxiv.org/abs/astro-ph/0401373%0Ahttp://dx.doi.org/10.1086/422245}, -volume = {611}, -year = {2004} -} -@article{Cappellari2012, -abstract = {Much of our knowledge of galaxies comes from analysing the radiation emitted by their stars, which depends on the present number of each type of star in the galaxy. The present number depends on the stellar initial mass function (IMF), which describes the distribution of stellar masses when the population formed, and knowledge of it is critical to almost every aspect of galaxy evolution. More than 50 years after the first IMF determination, no consensus has emerged on whether it is universal among different types of galaxies. Previous studies indicated that the IMF and the dark matter fraction in galaxy centres cannot both be universal, but they could not convincingly discriminate between the two possibilities. Only recently were indications found that massive elliptical galaxies may not have the same IMF as the Milky Way. Here we report a study of the two-dimensional stellar kinematics for the large representative ATLAS 3D sample of nearby early-type galaxies spanning two orders of magnitude in stellar mass, using detailed dynamical models. We find a strong systematic variation in IMF in early-type galaxies as a function of their stellar mass-to-light ratios, producing differences of a factor of up to three in galactic stellar mass. This implies that a galaxy's IMF depends intimately on the galaxy's formation history. {\textcopyright} 2012 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.3308}, -author = {Cappellari, Michele and McDermid, Richard M. and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Crocker, Alison F. and Davies, Roger L. and Davis, Timothy A. and {De Zeeuw}, P. T. and Duc, Pierre Alain and Emsellem, Eric and Khochfar, Sadegh and Krajnovi{\"{a}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1038/nature10972}, -eprint = {1202.3308}, -isbn = {1476-4687 (Electronic) 0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -month = {apr}, -number = {7395}, -pages = {485--488}, -pmid = {22538610}, -title = {{Systematic variation of the stellar initial mass function in early-type galaxies}}, -url = {http://arxiv.org/abs/1202.3308%5Cnhttp://dx.doi.org/10.1038/nature10972%5Cnhttp://www.nature.com/doifinder/10.1038/nature10972}, -volume = {484}, -year = {2012} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58 arcsec in the i band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including an {\$\sim${}}10 per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally,we check the sensitivity of our shear calibration estimates to other cutsmade on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalogue are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{Morganti2013, -abstract = {NGC 4494 is one of several intermediate-luminosity elliptical galaxies inferred to have an unusually diffuse dark matter halo. We use the $\chi$2-made-to-measure particle code nmagic to construct axisymmetric models of NGC 4494 from photometric and various kinematic data. The extended kinematics include light spectra in multiple slitlets out to 3.5Re, and hundreds of planetary nebula velocities out to ≃7Re, thus allowing us to probe the dark matter content and orbital structure in the halo. We use Monte Carlo simulations to estimate confidence boundaries for the halo parameters, given our data and modelling set-up. We find that the true potential of the dark matter halo is recovered within $\Delta$G (merit function) ≲ 26 ($\Delta$$\chi$2 ≲ 59) at the 70 per cent confidence level (CL), and within $\Delta$G ≲ 32 ($\Delta$$\chi$2 ≲ 70) at the 90 per cent CL. These numbers are much larger than the usually assumed $\Delta$$\chi$2 2.3 (4.6) for the 70 per cent (90 per cent) CL for two free parameters, perhaps case dependent, but calling into question the general validity of the standard assumptions used for halo and black hole mass determinations. The best-fitting models for NGC 4494 have a dark matter fraction of about 0.6 ± 0.1 at 5Re (70 per cent CL) and are embedded in a dark matter halo with circular velocity ∼200 km s-1. The total circular velocity curve (CVC) is approximately flat at vc 220 km s-1 outside ∼0.5Re. The orbital anisotropy of the stars is moderately radial. These results are independent of the assumed inclination of the galaxy, and edge-on models are preferred. Comparing with the haloes of NGC 3379 and NGC 4697, whose velocity dispersion profiles also decrease rapidly from the centre outwards, the outer CVCs and dark matter haloes are quite similar. NGC 4494 shows a particularly high dark matter fraction inside ∼ 3Re, and a strong concentration of baryons in the centre. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.2688}, -author = {Morganti, Lucia and Gerhard, Ortwin and Coccato, Lodovico and Martinez-valpuesta, Inma and Arnaboldi, Magda}, -doi = {10.1093/mnras/stt442}, -eprint = {1303.2688}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: individual: NGC 4494,Galaxies: kinematics and dynamics,Methods: numerical,cD}, -number = {4}, -pages = {3570--3588}, -title = {{Elliptical galaxies with rapidly decreasing velocity dispersion profiles: Nmagic models and dark halo parameter estimates for NGC 4494}}, -volume = {431}, -year = {2013} -} -@article{Handley2015, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR $\eta$(z) using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of 102 SGL with the measurement of corresponding velocity dispersion $\sigma$0 and Einstein radius $\theta$E. In addition, we also use a dataset of 12 two image lensing systems containing the measure of time delay $\Delta$ t between source images. Jointly these two datasets give us the angular diameter distance DAol of the lens. Further, for luminosity distance, we use the 740 observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ($\eta$=1) within 2$\sigma$ confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R F L}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Buitrago2017a, -abstract = {Using the exquisite depth of the Hubble Ultra Deep Field (HUDF12 programme) data set, we explore the ongoing assembly of the outermost regions of the most massive galaxies (Mstellar ≥ 5× 1010 M) at z ≤ 1. The outskirts of massive objects, particularly early-type Galaxies (ETGs), are expected to suffer a dramatic transformation across cosmic time due to continuous accretion of small galaxies. HUDF imaging allows us to study this process at intermediate redshifts in six massive galaxies, exploring the individual surface brightness profiles out to ∼25 effective radii. We find that 5–20 per cent of the total stellar mass for the galaxies in our sample is contained within 10 < R < 50 kpc. These values are in close agreement with numerical simulations, and higher than those reported for local late-type galaxies (5 per cent). The fraction of stellar mass stored in the outer envelopes/haloes of massive ETGs increases with decreasing redshift, being 28.7 per cent at = 0.1, 15.1 per cent at = 0.65 and 3.5 per cent at = 2. The fraction of mass in diffuse features linked with ongoing minor merger events is >1–2 per cent, very similar to predictions based on observed close pair counts. Therefore, the results for our small albeit meaningful sample suggest that the size and mass growth of the most massive galaxies have been solely driven by minor and major merging from z = 1 to today.}, -archivePrefix = {arXiv}, -arxivId = {1602.01846}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Curtis-Lake, Emma and Montes, Mireia and Cooper, Andrew P. and Bruce, Victoria A. and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G. and Cirasuolo, Michele}, -doi = {10.1093/mnras/stw3382}, -eprint = {1602.01846}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buitrago et al. - 2017 - The cosmic assembly of stellar haloes in massive early-type Galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: haloes,Galaxies: high-redshift,Galaxies: structure}, -number = {4}, -pages = {4888--4903}, -title = {{The cosmic assembly of stellar haloes in massive early-type Galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3382}, -volume = {466}, -year = {2017} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum $j_\star$ and the stellar mass $M_\star$ in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction $f_{\rm inf}$ of baryons that infall toward the central regions of galaxies where star formation can occur. We find $f_{\rm inf}\approx 1$ for LTGs and $\approx 0.4$ for ETGs with an uncertainty of about $0.25$ dex, consistent with a biased collapse. By comparing with the locally observed $j_\star$ vs. $M_\star$ relations for LTGs and ETGs we estimate the fraction $f_j$ of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find $f_j\approx 1.11^{+0.75}_{-0.44}$, in line with the classic disc formation picture; for ETGs we infer $f_j\approx 0.64^{+0.20}_{-0.16}$, that can be traced back to a $z<1$ evolution via dry mergers. We also show that the observed scatter in the $j_{\star}$ vs. $M_{\star}$ relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at $z\sim 2$ is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, J. and Lapi, A. and Mancuso, C. and Wang, H. and Danese, L.}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shi et al. - 2017 - Angular Momentum of Early- and Late-type Galaxies Nature or Nurture(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {2}, -pages = {105}, -title = {{Angular Momentum of Early- and Late-type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -volume = {843}, -year = {2017} -} -@article{Cooper:2010aa, -abstract = {We present six simulations of galactic stellar haloes formed by the tidal disruption of accreted dwarf galaxies in a fully cosmological setting. Our model is based on the Aquarius project, a suite of high-resolution N-body simulations of individual dark matter haloes. We tag subsets of particles in these simulations with stellar populations predicted by the galform semi-analytic model. Our method self-consistently tracks the dynamical evolution and disruption of satellites from high redshift. The luminosity function (LF) and structural properties of surviving satellites, which agree well with observations, suggest that this technique is appropriate. We find that accreted stellar haloes are assembled between 1 < z < 7 from less than five significant progenitors. These progenitors are old, metal-rich satellites with stellar masses similar to the brightest Milky Way dwarf spheroidals (107-108 M⊙). In contrast to previous stellar halo simulations, we find that several of these major contributors survive as self-bound systems to the present day. Both the number of these significant progenitors and their infall times are inherently stochastic. This results in great diversity among our stellar haloes, which amplifies small differences between the formation histories of their dark halo hosts. The masses (∼ 108-109 M⊙) and density/surface-brightness profiles of the stellar haloes (from 10 to 100 kpc) are consistent with expectations from the Milky Way and M31. Each halo has a complex structure, consisting of well-mixed components, tidal streams, shells and other subcomponents. This structure is not adequately described by smooth models. The central regions (<10 kpc) of our haloes are highly prolate (c/a ∼ 0.3), although we find one example of a massive accreted thick disc. Metallicity gradients in our haloes are typically significant only where the halo is built from a small number of satellites. We contrast the ages and metallicities of halo stars with surviving satellites, finding broad agreement with recent observations. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0910.3211}, -author = {Cooper, A. P. and Cole, S. and Frenk, C. S. and White, S. D.M. and Helly, J. and Benson, A. J. and {De Lucia}, G. and Helmi, A. and Jenkins, A. and Navarro, J. F. and Springel, V. and Wang, J.}, -doi = {10.1111/j.1365-2966.2010.16740.x}, -eprint = {0910.3211}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: dwarf,Galaxies: formation,Galaxies: haloes,Galaxies: structure,Galaxy: halo,Methods: numerical}, -month = {aug}, -number = {2}, -pages = {744--766}, -title = {{Galactic stellar haloes in the CDM model}}, -volume = {406}, -year = {2010} -} -@article{Birrer2018, -abstract = {We present a blind time-delay strong lensing (TDSL) cosmographic analysis of the doubly imaged quasar SDSS 1206+4332. We combine the relative time delay between the quasar images, Hubble Space Telescope imaging, the Keck stellar velocity dispersion of the lensing galaxy, and wide-field photometric and spectroscopic data of the field to constrain two angular diameter distance relations. The combined analysis is performed by forward modelling the individual data sets through a Bayesian hierarchical framework, and it is kept blind until the very end to prevent experimenter bias. After unblinding, the inferred distances imply a Hubble constant {\$}H{\_}0 = 68.8{\^{}}{\{}+5.4{\}}{\_}{\{}-5.1{\}}{\$} kms{\$}{\^{}}{\{}-1{\}}{\$}Mpc{\$}{\^{}}{\{}-1{\}}{\$}, assuming a flat Lambda cold dark matter cosmology with uniform prior on {\$}\backslashbackslashOmega{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm m{\}}{\$} in [0.05, 0.5]. The precision of our cosmographic measurement with the doubly imaged quasar SDSS 1206+4332 is comparable with those of quadruply imaged quasars and opens the path to perform on selected doubles the same analysis as anticipated for quads. Our analysis is based on a completely independent lensing code than our previous three H0LiCOW systems and the new measurement is fully consistent with those. We provide the analysis scripts paired with the publicly available software to facilitate independent analysis. The consistency between blind measurements with independent codes provides an important sanity check on lens modelling systematics. By combining the likelihoods of the four systems under the same prior, we obtain {\$}H{\_}0 = 72.5{\^{}}{\{}+2.1{\}}{\_}{\{}-2.3{\}}{\$}kms{\$}{\^{}}{\{}-1{\}}{\$}Mpc{\$}{\^{}}{\{}-1{\}}{\$}. This measurement is independent of the distance ladder and other cosmological probes.}, -archivePrefix = {arXiv}, -arxivId = {1809.01274}, -author = {Birrer, S and Treu, T and Rusu, C E and Bonvin, V and Fassnacht, C D and Chan, J H H and Agnello, A and Shajib, A J and Chen, G C -F. and Auger, M and Courbin, F and Hilbert, S and Sluse, D and Suyu, S H and Wong, K C and Marshall, P and Lemaux, B C and Meylan, G}, -eprint = {1809.01274}, -keywords = {cosmology,galaxies,gravitational lensing,hubble constant,method}, -number = {September}, -pages = {1--27}, -title = {{H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant}}, -url = {http://arxiv.org/abs/1809.01274}, -volume = {27}, -year = {2018} -} -@article{Dullo2014, -abstract = {New surface brightness profiles from 26 early-type galaxies with suspected partially depleted cores have been extracted from the full radial extent of Hubble Space Telescope images. We have carefully quantified the radial stellar distributions of the elliptical galaxies using the core- S{\'{e}}rsic model whereas for the lenticular galaxies a core-S{\'{e}}rsic bulge plus an exponential disc model gives the best representation. We additionally caution about the use of excessive multiple S{\'{e}}rsic functions for decomposing galaxies and compare with past fits in the literature. The structural parameters obtained from our fitted models are, in general, in good agreement with our initial study using radially limited (R ≲ 10 arcsec) profiles, and are used here to update several 'central' as well as 'global' galaxy scaling relations. We find near-linear relations between the break radius Rb and the spheroid luminosity L such that Rb ∝ L1.13±0.13, and with the supermassive black hole mass MBH such that Rb ∝ M0.83±0.21BH. This is internally consistent with the notion that major, dry mergers add the stellar and black hole mass in equal proportion, i.e. MBH ∝ L. In addition, we observe a linear relation Rb ∝ R0.98±0.15e for the core-S{\'{e}}rsic elliptical galaxies - where Re is the galaxies' effective half-light radii - which is collectively consistent with the approximately linear, bright-end of the curved L-Re relation. Finally, we measure accurate stellar mass deficits Mdef that are in general 0.5-4 MBH, and we identify two galaxies (NGC 1399, NGC 5061) that, due to their high Mdef/MBH ratio, may have experienced oscillatory core-passage by a (gravitational radiation)-kicked black hole. The galaxy scaling relations and stellar mass deficits favour core-S{\'{e}}rsic galaxy formation through a few 'dry' major merger events involving supermassive black holes such that Mdef ∝ M3.70±0.76BH, for MBH≳ 2 × 108M⊙.}, -archivePrefix = {arXiv}, -arxivId = {1310.5867}, -author = {Dullo, Bililign T. and Graham, Alister W.}, -doi = {10.1093/mnras/stu1590}, -eprint = {1310.5867}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Elliptical and lenticular,Fundamental parameters-galaxies,Galaxies,Nuclei-galaxies,Photometry-galaxies,Structure,cD-galaxies}, -month = {nov}, -number = {3}, -pages = {2700--2722}, -title = {{Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Bellstedt2018, -abstract = {We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 1010 < M*/M⊙ < 1011.6 that cover a large radial range of 0.1-4.0 effective radii.We combine SLUGGS and ATLAS3D data sets to model the total-mass profiles of a sample of 21 fast-rotator galaxies, utilizing a hyperparameter method to combine the two independent data sets. The total-mass density profile slope values derived for these galaxies are consistent with those measured in the inner regions of galaxies by other studies. Furthermore, the total-mass density slopes ($\gamma$tot) appear to be universal over this broad stellar mass range, with an average value of $\gamma$tot= -2.24± 0.05, i.e. slightly steeper than isothermal. We compare our results to model galaxies from the Magneticum and EAGLE cosmological hydrodynamic simulations, in order to probe the mechanisms that are responsible for varying total-mass density profile slopes. The simulated-galaxy slopes are shallower than the observed values by $\sim$0.3-0.5, indicating that the physical processes shaping the mass distributions of galaxies in cosmological simulations are still incomplete. For galaxies with M* > 1010.7M⊙ in the Magneticum simulations, we identify a significant anticorrelation between total-mass density profile slopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas this anticorrelation is weaker for lower stellar masses, implying that the measured total-mass density slopes for low-mass galaxies are less likely to be determined by merger activity.}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A. and Romanowsky, Aaron J. and Remus, Rhea Silvia and Stevens, Adam R.H. and Brodie, Jean P. and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bellstedt et al. - 2018 - The SLUGGS survey A comparison of total-mass profiles of early-type galaxies from observations and cosmologica.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to $\sim$4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Rauch1998, -abstract = {Observations of redshifted Lyman alpha forest absorption in the spectra of quasistellar objects (QSOs) provide a highly sensitive probe of the distribution of gaseous matter in the universe. Over the past two decades optical spectroscopy with large ground-based telescopes, and more recently ultraviolet spectroscopy from space have yielded a wealth of information on what appears to be a gaseous, photoionized intergalactic medium, partly enriched by the products of stellar nucleosynthesis, residing in coherent structures over many hundreds of kiloparsecs. Recent progress with cosmological hydro-simulations based on hierarchical structure formation models has led to important insights into the physical structures giving rise to the forest. If these ideas are correct, a truely inter- and proto-galactic medium [at high redshift (z {\$\sim${}} 3), the main repository of baryons] collapses under the influence of dark matter gravity into flattened or filamentary structures, which are seen in absorption against background QSOs. With decreasing redshift, galaxies forming in the denser regions, may contribute an increasing part of the Lyman alpha absorption cross-section. Comparisons between large data samples from the new generation of telescopes and artificial Lyman alpha forest spectra from cosmological simulations promise to become a useful cosmological tool.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9806286}, -author = {Rauch, Michael}, -doi = {10.1146/annurev.astro.36.1.267}, -eprint = {9806286}, -issn = {0066-4146}, -journal = {Annual Review of Astronomy and Astrophysics}, -number = {1}, -pages = {267--316}, -primaryClass = {astro-ph}, -title = {{the Lyman Alpha Forest in the Spectra of Quasistellar Objects}}, -url = {http://arxiv.org/abs/astro-ph/9806286%7B%5C%25%7D0Ahttp://dx.doi.org/10.1146/annurev.astro.36.1.267}, -volume = {36}, -year = {2002} -} -@article{Hall2014, -abstract = {The science goals of space missions from the Hubble Space Telescope through to Gaia and Euclid require ultraprecise positional, photometric, and shape measurement information. However, in the radiation environment of the space telescopes, damage to the focal plane detectors through high-energy protons leads to the creation of traps, a loss of charge transfer efficiency, and a consequent deterioration in measurement accuracy. An understanding of the traps produced and their properties in the CCD during operation is essential to allow optimization of the devices and suitable modeling to correct the effect of the damage through the postprocessing of images. The technique of 'pumping single traps' has allowed the study of individual traps in high detail that cannot be achieved with other techniques, such as deep level transient spectroscopy, whilst also locating each trap to the subpixel level in the device. Outlining the principles used, we have demonstrated the technique for the A-center, the most influential trap in serial readout, giving results consistent with the more general theoretical values, but here showing new results indicating the spread in the emission times achieved and the variation in capture probability of individual traps with increasing signal levels. This technique can now be applied to other time and temperature regimes in the CCD to characterize individual traps in situ under standard operating conditions such that dramatic improvements can be made to optimization processes and modeling techniques. ? 2013 IEEE.}, -author = {Hall, David J and Murray, Neil J and Holland, Andrew D and Gow, Jason and Clarke, Andrew and Burt, David}, -doi = {10.1109/TNS.2013.2295941}, -isbn = {9781467350570}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {A-centre,CCD image sensors,Euclid,Si-A,defect,pocket pumping,radiation damage,trap pumping}, -number = {4}, -pages = {1826--1833}, -title = {{Determination of in situ trap properties in CCDs using a "single-trap pumping" technique}}, -volume = {61}, -year = {2014} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned {\$}r{\$} and {\$}g{\$} band images from a sample of 45508 galaxies from SDSS DR9 in the redshift range {\$}0.06\backslash,\backslashle\backslash,z\backslash,\backslashle\backslash,0.1{\$} and in the mass range {\$}10{\^{}}{\{}10.0{\}} M{\_}{\{}\backslashodot{\}} {\textless} M{\_}{\{}*{\}} {\textless} 10{\^{}}{\{}11.4{\}} M{\_}{\{}\backslashodot{\}}{\$}r. We derive surface brightness profiles to a depth of almost {\$}\backslashmu{\_}r \backslashsim 32 \backslash,\backslashmathrm{\{}mag\backslash,arcsec{\}}{\^{}}{\{}-2{\}}{\$}. We find that the ellipticity of the stellar halo is a function of galaxy stellar mass and that the haloes of high concentration ({\$}C {\textgreater} 2.6{\$}) galaxies are more elliptical than those of low concentration ({\$}C {\textless} 2.6{\$}) galaxies. The {\$}g{\$}-{\$}r{\$} colour profile of high concentration galaxies reveals that the {\$}g{\$}-{\$}r{\$} colour of the stellar population in the stellar halo is bluer than in the main galaxy, and the colour of the stellar halo is redder for higher mass galaxies. We further demonstrate that the full two-dimensional surface intensity distribution of our galaxy stacks can only be fit through multi-component S$\backslash$'{\{}e{\}}rsic models. Using the fraction of light in the outer component of the models as a proxy for the fraction of accreted stellar light, we show that this fraction is a function of stellar mass and galaxy type. For high concentration galaxies, the fraction of accreted stellar light rises from {\$}30\backslash{\%}{\$} to {\$}70\backslash{\%}{\$} for galaxies in the stellar mass range from {\$}10{\^{}}{\{}10.0{\}} M{\_}{\{}\backslashodot{\}}{\$} to {\$}10{\^{}}{\{}11.4{\}} M{\_}{\{}\backslashodot{\}}{\$}. The fraction of accreted light is much smaller in low concentration systems, increasing from {\$}2\backslash{\%}{\$} to {\$}25\backslash{\%}{\$} over the same mass range. This work provides important constraints for the theoretical understanding of the formation of stellar haloes of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1404.2123}, -author = {D'Souza, Richard and Kauffman, Guinevere and Wang, Jing and Vegetti, Simona}, -doi = {10.1093/mnras/stu1194}, -eprint = {1404.2123}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: halo,Galaxy: structure}, -number = {2}, -pages = {1433--1450}, -title = {{Parametrizing the stellar haloes of galaxies}}, -volume = {443}, -year = {2014} -} -@article{Tinker2013, -abstract = {We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2, 1.0]. For massive galaxies, M ≳ 1010.6 M , our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M ∼ 1010 M , the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1308.2974}, -author = {Tinker, Jeremy L. and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R. and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H.}, -doi = {10.1088/0004-637X/778/2/93}, -eprint = {1308.2974}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tinker et al. - 2013 - Evolution of the stellar-to-dark matter relation Separating star-forming and passive galaxies from z = 1 to 0.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: halos}, -number = {2}, -title = {{Evolution of the stellar-to-dark matter relation: Separating star-forming and passive galaxies from z = 1 to 0}}, -volume = {778}, -year = {2013} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in {\$\sim${}}10 dynamical times, or {\$\sim${}}0.5Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, {\$\sim${}}100 Msun/yr, and each clump converts into stars in {\$\sim${}}0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z{\$\sim${}}3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z{\$\sim${}}1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M{\textgreater}10{\^{}}11 M{\_}sun) galaxies at 1.7{\textless}z{\textless}3 utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our sample is almost an order of magnitude larger than previous studies at these redshifts, providing the first statistical study of massive galaxy sizes at z{\textgreater}2, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n{\textless}2) and spheroid-like (n{\textgreater}2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z{\$\sim${}}2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z{\textgreater}2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ({\$\sim${}}2x10{\^{}}10 M{\_}sun kpc{\^{}}-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J and Bouwens, Rychard J and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -isbn = {1005-0302}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61--------L64}, -title = {{Size evolution of the most massive galaxies at 1.7{\textless}z{\textless}3 from GOODS NICMOS survey imaging}}, -url = {http://arxiv.org/abs/0807.4141%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Biernaux2016, -abstract = {Context. The luminosity profiles of galaxies acting as strong gravitational lenses can be tricky to study. Indeed, strong gravitational lensing images display several lensed components, both point-like and diffuse, around the lensing galaxy. Those objects limit the study of the galaxy luminosity to its inner parts. Therefore, the usual fitting methods perform rather badly on such images. Previous studies of strong lenses luminosity profiles using software such as GALFIT or IMFITFITS and various PSF-determining methods have resulted in somewhat discrepant results. Aims. The present work aims at investigating the causes of those discrepancies, as well as at designing more robust techniques for studying the morphology of early-type lensing galaxies with the ability to subtract a lensed signal from their luminosity profiles. Methods. We design a new method to independently measure each shape parameter, namely, the position angle, ellipticity, and half-light radius of the galaxy. Our half-light radius measurement method is based on an innovative scheme for computing isophotes that is well suited to measuring the morphological properties of gravititational lensing galaxies. Its robustness regarding various specific aspects of gravitational lensing image processing is analysed and tested against GALFIT. It is then applied to a sample of systems from the CASTLES database. Results. Simulations show that, when restricted to small, inner parts of the lensing galaxy, the technique presented here is more trustworthy than GALFIT. It gives more robust results than GALFIT, which shows instabilities regarding the fitting region, the value of the S{\'{e}}rsic index, and the signal-to-noise ratio. It is therefore better suited than GALFIT for gravitational lensing galaxies. It is also able to study lensing galaxies that are not much larger than the PSF. New values for the half-light radius of the objects in our sample are presented and compared to previous works.}, -archivePrefix = {arXiv}, -arxivId = {1510.09118}, -author = {Biernaux, J. and Magain, P. and Sluse, D. and Chantry, V.}, -doi = {10.1051/0004-6361/201526910}, -eprint = {1510.09118}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: luminosity function, mass function,Gravitational lensing: strong}, -month = {jan}, -pages = {A84}, -title = {{Analysis of luminosity distributions and the shape parameters of strong gravitational lensing elliptical galaxies}}, -url = {http://www.aanda.org/10.1051/0004-6361/201526910}, -volume = {585}, -year = {2016} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287----a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted $\sim$100-200 luminous satellite galaxies in the past \$\sim$12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ($\sim$80%) coming from the \$\sim$15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of $\sim$9 Gyr in the past, while surviving satellite systems have median accretion times of $\sim$5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S. and Johnston, Kathryn V.}, -doi = {10.1086/497422}, -eprint = {0506467}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bullock, Johnston - 2005 - Tracing Galaxy Formation with Stellar Halos. I. Methods(2).pdf:pdf}, -isbn = {0272-9490 (Print)\r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Leauthaud2017, -abstract = {We present high signal-to-noise galaxy-galaxy lensing measurements of the Baryon Oscillation Spectroscopic Survey constant mass (CMASS) sample using 250 deg2 of weak-lensing data from Canada-France-Hawaii Telescope Lensing Survey and Canada-France-Hawaii Telescope Stripe 82 Survey. We compare this signal with predictions from mock catalogues trained to match observables including the stellar mass function and the projected and twodimensional clustering of CMASS. We show that the clustering of CMASS, together with standard models of the galaxy-halo connection, robustly predicts a lensing signal that is 20-40 per cent larger than observed. Detailed tests show that our results are robust to a variety of systematic effects. Lowering the value of S8 = $\sigma$8 √ $\Omega$m/0.3 compared to Planck Collaboration XIII reconciles the lensing with clustering. However, given the scale of our measurement (r {\textless} 10 h-1 Mpc), other effects may also be at play and need to be taken into consideration. We explore the impact of baryon physics, assembly bias, massive neutrinos and modifications to general relativity on $\Delta$$\Sigma$ and show that several of these effects may be non-negligible given the precision of our measurement. Disentangling cosmological effects from the details of the galaxy-halo connection, the effect of baryons, and massive neutrinos, is the next challenge facing joint lensing and clustering analyses. This is especially true in the context of large galaxy samples from Baryon Acoustic Oscillation surveys with precise measurements but complex selection functions.}, -archivePrefix = {arXiv}, -arxivId = {1611.08606}, -author = {Leauthaud, Alexie and Saito, Shun and Hilbert, Stefan and Barreira, Alexandre and More, Surhud and White, Martin and Alam, Shadab and Behroozi, Peter and Bundy, Kevin and Coupon, Jean and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Mandelbaum, Rachel and Miller, Lance and Moraes, Bruno and Pereira, Maria E S and Rodr{\'{i}}guez-Torres, Sergio A and Schmidt, Fabian and Shan, Huan Yuan and Viel, Matteo and Villaescusa-Navarro, Francisco}, -doi = {10.1093/mnras/stx258}, -eprint = {1611.08606}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {3}, -pages = {3024--3047}, -title = {{Lensing is low: Cosmology, galaxy formation or new physics?}}, -volume = {467}, -year = {2017} -} -@article{Vogelsberger2013, -abstract = {We present a multi-epoch analysis of the galaxy populations formed within the cosmological hydrodynamical simulations presented in Vogelsberger et al. These simulations explore the performance of a recently implemented feedback model which includes primordial and metal line radiative cooling with self-shielding corrections; stellar evolution with associated mass-loss and chemical enrichment; feedback by stellar winds; black hole seeding, growth and merging; and active galactic nuclei (AGN) quasar-and radio-mode heating with a phenomenological prescription for AGN electro-magnetic feedback.We illustrate the impact of the model parameter choices on the resulting simulated galaxy population properties at high and intermediate redshifts.We demonstrate that our scheme is capable of producing galaxy populations that broadly reproduce the shape of the observed galaxy stellar mass function extending from redshift z = 0 to z = 3. We also characterize the evolving galactic B-band luminosity function, stellar mass to halo mass ratio, star formation main sequence, Tully-Fisher relation and gas-phase mass-metallicity relation and confront them against recent observational estimates. This detailed comparison allows us to validate elements of our feedback model, while also identifying areas of tension (e.g., the shape and normalization of the mass-metallicity relation and normalization of the star formation main sequence) that will be addressed in future work. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1305.4931}, -author = {Torrey, Paul and Vogelsberger, Mark and Genel, Shy and Sijacki, Debora and Springel, Volker and Hernquist, Lars}, -doi = {10.1093/mnras/stt2295}, -eprint = {1305.4931}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {1985--2004}, -title = {{A model for cosmological simulations of galaxy formation physics: Multi-epoch validation}}, -url = {http://arxiv.org/abs/1305.2913}, -volume = {438}, -year = {2014} -} -@article{Huang2018, -abstract = {We use {\$\sim${}}100 deg2 of deep ({\textgreater} 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach {\$\sim${}}4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) {\textgreater} 11.6 in more massive haloes at 0.3 {\textless} z {\textless} 0.5 have shallower inner stellar mass density profiles (within {\$\sim${}}10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) {\textgreater} 14.0 are {\$\sim${}}20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{Carpenter2017, -abstract = {Stan is a probabilistic programming language for specifying statistical models. A Stan program imperatively defines a log probability function over parameters conditioned on specified data and constants. As of version 2.14.0, Stan provides full Bayesian inference for continuous-variable models through Markov chain Monte Carlo methods such as the No-U-Turn sampler, an adaptive form of Hamiltonian Monte Carlo sampling. Penalized maximum likelihood estimates are calculated using optimization methods such as the limited memory Broyden-Fletcher-Goldfarb-Shanno algorithm. Stan is also a platform for computing log densities and their gradients and Hessians, which can be used in alternative algorithms such as variational Bayes, expectation propagation, and marginal inference using approximate integration. To this end, Stan is set up so that the densities, gradients, and Hessians, along with intermediate quantities of the algorithm such as acceptance probabilities, are easily accessible. Stan can be called from the command line using the cmdstan package, through R using the rstan package, and through Python using the pystan package. All three interfaces support sampling and optimization-based inference with diagnostics and posterior analysis. rstan and pystan also provide access to log probabilities, gradients, Hessians, parameter transforms, and specialized plotting.}, -author = {Carpenter, Bob and Gelman, Andrew and Hoffman, Matthew D and Lee, Daniel and Goodrich, Ben and Betancourt, Michael and Brubaker, Marcus A and Guo, Jiqiang and Li, Peter and Riddell, Allen}, -doi = {10.18637/jss.v076.i01}, -issn = {15487660}, -journal = {Journal of Statistical Software}, -keywords = {Algorithmic differentiation,Bayesian inference,Probabilistic program,Stan}, -number = {1}, -title = {{Stan: A probabilistic programming language}}, -volume = {76}, -year = {2017} -} -@article{Skilling2006, -abstract = {Nested sampling estimates directly how the likelihood function relates to prior mass. The evidence (alternatively the marginal likelihood, marginal density of the data, or the prior predictive) is immediately obtained by summation. It is the prime result of the computation, and is accompanied by an estimate of numerical uncertainty. Samples from the posterior distribution are an optional by-product, obtainable for any temperature. The method relies on sampling within a hard constraint on likelihood value, as opposed to the softened likelihood of annealing methods. Progress depends only on the shape of the "nested"contours of likelihood, and not on the likelihood values. This invariance (over monotonic relabelling) allows the method to deal with a class of phasechange problems which effectively defeat thermal annealing. {\textcopyright} 2006 International Society for Bayesian Analysis.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {Skilling, John}, -doi = {10.1214/06-BA127}, -eprint = {arXiv:1011.1669v3}, -isbn = {9788578110796}, -issn = {19360975}, -journal = {Bayesian Analysis}, -keywords = {Algorithm,Annealing,Bayesian computation,Evidence,Marginal likelihood,Model selection,Nest,Phase change}, -number = {4}, -pages = {833--860}, -pmid = {25246403}, -title = {{Nested sampling for general Bayesian computation}}, -url = {http://projecteuclid.org/euclid.ba/1340370944}, -volume = {1}, -year = {2006} -} -@article{Etherington2023a, -abstract = {The distribution of mass in galaxy-scale strong gravitational lenses is often modelled as an elliptical power law plus `external shear', which notionally accounts for neighbouring galaxies and cosmic shear. We show that it does not. Except in a handful of rare systems, the best-fit values of external shear do not correlate with independent measurements of shear: from weak lensing in 45 Hubble Space Telescope images, or in 50 mock images of lenses with complex distributions of mass. Instead, the best-fit shear is aligned with the major or minor axis of 88% of lens galaxies; and the amplitude of the external shear increases if that galaxy is disky. We conclude that `external shear' attached to a power law model is not physically meaningful, but a fudge to compensate for lack of model complexity. Since it biases other model parameters that are interpreted as physically meaningful in several science analyses (e.g. measuring galaxy evolution, dark matter physics or cosmological parameters), we recommend that future studies of galaxy-scale strong lensing should employ more flexible mass models.}, -archivePrefix = {arXiv}, -arxivId = {2301.05244}, -author = {Etherington, Amy and Nightingale, James W. and Massey, Richard and Tam, Sut-Ieng and Cao, XiaoYue and Niemiec, Anna and He, Qiuhan and Robertson, Andrew and Li, Ran and Amvrosiadis, Aristeidis and Cole, Shaun and Diego, Jose M. and Frenk, Carlos S. and Frye, Brenda L. and Harvey, David and Jauzac, Mathilde and Koekemoer, Anton M. and Lagattuta, David J. and Limousin, Marceau and Mahler, Guillaume and Sirks, Ellen and Steinhardt, Charles L.}, -eprint = {2301.05244}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Etherington2023Shear.pdf:pdf}, -journal = {arXiv:2301.05244}, -keywords = {galaxies,gravitational lensing,strong,structure}, -number = {January}, -title = {{Strong gravitational lensing's `external shear' is not shear}}, -url = {http://arxiv.org/abs/2301.05244}, -year = {2023} -} -@article{Geometryel, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z ∼ 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u - g color profiles for these galaxies and show that most z ∼ 2galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z ∼ 2galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: ($\Delta$(u - g rest)/$\Delta$(log r))median = -0.47, -0.33, and -0.46 for z ∼ 2, z ∼ 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z ∼ 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u - g colors, and lower S{\'{e}}rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch. {\textcopyright}2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J and {Van Dokkum}, Pieter G and Labb{\'{e}}, Ivo and Illingworth, Garth D and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Brooks2015a, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Alexander2020, -abstract = {The identity of dark matter remains one of the most pressing questions in physics today. While many promising dark matter candidates have been put forth over the last half-century, to date the true identity of dark matter remains elusive. While it is possible that one of the many proposed candidates may turn out to be dark matter, it is at least equally likely that the correct physical description has yet to be proposed. To address this challenge, novel applications of machine learning can help physicists gain insight into the dark sector from a theory agnostic perspective. In this work we demonstrate the use of unsupervised machine learning techniques to infer the presence of substructure in dark matter halos using galaxy-galaxy strong lensing simulations in a proof-of-principle application.}, -archivePrefix = {arXiv}, -arxivId = {2008.12731}, -author = {Alexander, Stephon and Gleyzer, Sergei and Parul, Hanna and Reddy, Pranath and Toomey, Michael W. and Usai, Emanuele and Klar, Ryker Von}, -eprint = {2008.12731}, -file = {:C\:/Users/Jammy/Documents/Papers/PyAutoLens/Alexander2020GSoCDecoding.pdf:pdf}, -issn = {23318422}, -journal = {arXiv}, -number = {1998}, -title = {{Decoding Dark Matter Substructure without Supervision}}, -year = {2020} -} -@article{Magnelli2012, -abstract = {We study a sample of 61submillimetre galaxies (SMGs) selected from ground-based surveys, with known spectroscopic redshifts and observed with the Herschel Space Observatory as part of the PACS Evolutionary Probe (PEP) and the Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time key programmes. Our study makes use of the broad far-infrared and submillimetre wavelength coverage (100-600 $\mu$m) only made possible by the combination of observations from the PACS and SPIRE instruments aboard the Herschel Space Observatory. Using a power-law temperature distribution model to derive infrared luminosities and dust temperatures, we measure a dust emissivity spectral index for SMGs of $\beta$ = 2.0 ± 0.2. Our results unambiguously unveil the diversity of the SMG population. Some SMGs exhibit extreme infrared luminosities of ∼10 13L ⊙ and relatively warm dust components, while others are fainter (a few times 10 12 L ⊙) and are biased towards cold dust temperatures. Although at z ∼ 2 classical SMGs (>5 mJy at 850 $\mu$m) have large infrared luminosities (∼10 13 L ⊙), objects only selected on their submm flux densities (without any redshift informations) probe a large range in dust temperatures and infrared luminosities. The extreme infrared luminosities of some SMGs (L IR ≈ 10 12.7 L ⊙, 26/61 systems) imply star formation rates (SFRs) of >500 M ⊙ yr -1 (assuming a Chabrier IMF and no dominant AGN contribution to the FIR luminosity). Such high SFRs are difficult to reconcile with a secular mode of star formation, and may instead correspond to a merger-driven stage in the evolution of these galaxies. Another observational argument in favour of this scenario is the presence of dust temperatures warmer than that of SMGs of lower luminosities (∼40 K as opposed to ∼25 K), consistent with observations of local ultra-luminous infrared galaxies triggered by major mergers and with results from hydrodynamic simulations of major mergers combined with radiative transfer calculations. Moreover, we find that luminous SMGs are systematically offset from normal star-forming galaxies in the stellar mass-SFR plane, suggesting that they are undergoing starburst events with short duty cycles, compatible with the major merger scenario. On the other hand, a significant fraction of the low infrared luminosity SMGs have cold dust temperatures, are located close to the main sequence of star formation, and therefore might be evolving through a secular mode of star formation. However, the properties of this latter population, especially their dust temperature, should be treated with caution because at these luminosities SMGs are not a representative sample of the entire star-forming galaxy population. {\textcopyright} 2012 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1202.0761}, -author = {Magnelli, B. and Lutz, D. and Santini, P. and Saintonge, A. and Berta, S. and Albrecht, M. and Altieri, B. and Andreani, P. and Aussel, H. and Bertoldi, F. and B{\'{e}}thermin, M. and Bongiovanni, A. and Capak, P. and Chapman, S. and Cepa, J. and Cimatti, A. and Cooray, A. and Daddi, E. and Danielson, A. L.R. and Dannerbauer, H. and Dunlop, J. S. and Elbaz, D. and Farrah, D. and {F{\"{o}}rster Schreiber}, N. M. and Genzel, R. and Hwang, H. S. and Ibar, E. and Ivison, R. J. and {Le Floc'H}, E. and Magdis, G. and Maiolino, R. and Nordon, R. and Oliver, S. J. and {P{\'{e}}rez Garc{\'{i}}a}, A. and Poglitsch, A. and Popesso, P. and Pozzi, F. and Riguccini, L. and Rodighiero, G. and Rosario, D. and Roseboom, I. and Salvato, M. and Sanchez-Portal, M. and Scott, D. and Smail, I. and Sturm, E. and Swinbank, A. M. and Tacconi, L. J. and Valtchanov, I. and Wang, L. and Wuyts, S.}, -doi = {10.1051/0004-6361/201118312}, -eprint = {1202.0761}, -isbn = {9780099578529}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {galaxies: evolution,galaxies: starburst,infrared: galaxies,submillimeter: galaxies}, -pages = {A155}, -pmid = {18701455}, -title = {{A Herschel view of the far-infrared properties of submillimetre galaxies}}, -url = {http://arxiv.org/abs/1202.0761%0Ahttp://dx.doi.org/10.1051/0004-6361/201118312}, -volume = {539}, -year = {2012} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}$\backslash${\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashsigma{\$} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and {P{\'{e}}rez Gonz{\'{a}}lez}, Pablo G and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {112}, -title = {{ CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z ∼ 2 }}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -volume = {846}, -year = {2017} -} -@article{Xie2015, -abstract = {Recent work has suggested that the amplitude of the size mass relation of massive early type galaxies evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive early type galaxies. We find this model is able to reproduce the amplitude of present day amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark halos at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than {\$}10{\^{}}{\{}11.4{\}}M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$}. At lower masses, low mass ratio mergers play a more important role. In situ star formation contribute more to the size growth than it does to stellar mass growth. We also find that, for ETGs identified at {\$}z=2{\$}, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Barger1998, -abstract = {Optical surveys of the global star-formation rate in high-redshift galaxies show a strong peak in activity at a redshift of z ≃ 1.5, which implies that most of the star formation1 has already been seen. High- redshift galaxies may, however, emit most of their energy at submillimetre wavelengths, if they contain substantial amounts of dust that absorbs the starlight and reradiates it as far-infrared light. Here we report a deep survey of a blank region of sky, performed at submillimetre wavelengths (450 and 850 $\mu$m). We detect luminous sources in the 850-$\mu$m band which, if they have similar spectra to low-redshift ultraluminous infrared galaxies and are primarily powered by star formation, must each be converting more than 100 solar masses of gas per year into stars: this is larger than the maximum star-formation rates inferred for most optically selected galaxis2. The total amount of star formation at high redshifts is essentially fixed by the level of background light, but where the peak activity occurs at submillimetre wavelengths is not yet well established. However, the background light inferred from the sources that we have detected is already comparable to that from the optically selected sources. Establishing the main epoch of star formation will therefore require a combination of optical and submillimetre studies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9806317}, -author = {Barger, A. J. and Cowie, L. L. and Sanders, D. B. and Fulton, E. and Taniguchi, Y. and Sato, Y. and Kawara, K. and Okuda, H.}, -doi = {10.1038/28338}, -eprint = {9806317}, -issn = {00280836}, -journal = {Nature}, -number = {6690}, -pages = {248--251}, -primaryClass = {astro-ph}, -title = {{Submillimetre-wavelength detection of dusty star-forming galaxies at high redshift}}, -url = {http://adsabs.harvard.edu/abs/1998Natur.394..248B}, -volume = {394}, -year = {1998} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum $j_\star$ and the stellar mass $M_\star$ in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction $f_{\rm inf}$ of baryons that infall toward the central regions of galaxies where star formation can occur. We find $f_{\rm inf}\approx 1$ for LTGs and $\approx 0.4$ for ETGs with an uncertainty of about $0.25$ dex, consistent with a biased collapse. By comparing with the locally observed $j_\star$ vs. $M_\star$ relations for LTGs and ETGs we estimate the fraction $f_j$ of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find $f_j\approx 1.11^{+0.75}_{-0.44}$, in line with the classic disc formation picture; for ETGs we infer $f_j\approx 0.64^{+0.20}_{-0.16}$, that can be traced back to a $z<1$ evolution via dry mergers. We also show that the observed scatter in the $j_{\star}$ vs. $M_{\star}$ relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at $z\sim 2$ is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, J. and Lapi, A. and Mancuso, C. and Wang, H. and Danese, L.}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shi et al. - 2017 - Angular Momentum of Early- and Late-type Galaxies Nature or Nurture(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {2}, -pages = {105}, -title = {{Angular Momentum of Early- and Late-type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -volume = {843}, -year = {2017} -} -@article{Einstein1916, -abstract = {Not Available}, -author = {Lorentz, H. A. and Einstein, A. and Minkowski, H. and Einstein, A.}, -doi = {10.1007/978-3-663-19510-8_7}, -isbn = {1521-3889}, -issn = {15213889}, -journal = {Das Relativit{\"{a}}tsprinzip}, -number = {7}, -pages = {81--124}, -pmid = {168842}, -title = {{Die Grundlage der allgemeinen Relativit{\"{a}}tstheorie}}, -volume = {354}, -year = {1923} -} -@article{Bartelmann1999, -abstract = {We review theory and applications of weak gravitational lensing. After summarising Friedmann-Lema{\^{i}}tre cosmological models, we present the formalism of gravitational lensing and light propagation in arbitrary space-times. We discuss how weak-lensing effects can be measured. The formalism is then applied to reconstructions of galaxy-cluster mass distributions, gravitational lensing by large-scale matter distributions, QSO-galaxy correlations induced by weak lensing, lensing of galaxies by galaxies, and weak lensing of the cosmic microwave background. {\textcopyright}2001 Elsevier Science B.V.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9912508}, -author = {Bartelmann, Matthias and Schneider, Peter}, -doi = {10.1016/S0370-1573(00)00082-X}, -eprint = {9912508}, -issn = {03701573}, -journal = {Physics Report}, -number = {4-5}, -pages = {291--472}, -primaryClass = {astro-ph}, -title = {{Weak gravitational lensing}}, -url = {http://arxiv.org/abs/astro-ph/9912508%7B%5C%25%7D0Ahttp://dx.doi.org/10.1016/S0370-1573(00)00082-X}, -volume = {340}, -year = {2001} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, $M_{BH}$, that had been imaged at $3.6\sim\mu m$ with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between $M_{ BH}$ and the host spheroid (and galaxy) luminosity, $L_{sph}$ (and $L_{gal}$), and also stellar mass, $M_{*,sph}$. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have $M_{BH} < 10^7\simM_\odot$, and allows us to better investigate the poorly studied low-mass end of the $M_{BH} - M_{*,sph}$ correlation. The bulges of early-type galaxies follow $M_{BH} \propto M_{*,sph}^{1.04 \pm 0.10}$ and define a tight red sequence with intrinsic scatter $\epsilon = 0.43 \pm 0.06\simdex$ and a median $M_{BH}/M_{*,sph}$ ratio of $0.68 \pm 0.04\%$, i.e.$\sim$a $\pm 2\sigma$ range of 0.1-5%. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with $M_{BH} \propto M_{*,sph}^{2-3}$, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index $n<2$, argued by some to be pseudo-bulges, are not offset to lower $M_{BH}$ from the correlation defined by the current bulge sample with $n>2$; and iii) $L_{sph}$ and $L_{gal}$ correlate equally well with $M_{BH}$, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with $L_{ sph}$ is better than that with $L_{gal}$.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A. D. and Graham, Alister W. and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Savorgnan et al. - 2016 - Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M ,Sph Diagr(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Zehavi2017, -abstract = {We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -- halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto- and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.}, -archivePrefix = {arXiv}, -arxivId = {1706.07871}, -author = {Zehavi, Idit and Contreras, Sergio and Padilla, Nelson and Smith, Nicholas J and Baugh, Carlton M and Norberg, Peder}, -doi = {10.3847/1538-4357/aaa54a}, -eprint = {1706.07871}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {clustering,cosmology,evolution,galaxies,halos,large-scale structure of universe,statistics,theory}, -number = {1}, -pages = {84}, -title = {{The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos}}, -url = {http://arxiv.org/abs/1706.07871%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaa54a}, -volume = {853}, -year = {2018} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: `blue-sequence' galaxies that are rapidly forming young stars, and `red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than {\$}3\backslashtimes10{\^{}}{\{}10{\}} M{\_}\backslashodot{\$} follow the red-sequence while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's center. We develop a simple analytic model for this interaction. In galaxies less massive than {\$}3\backslashtimes10{\^{}}{\{}10{\}} M{\_}\backslashodot{\$}, young stars and supernovae drive a high entropy outflow that is more buoyant that any diffuse corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by a hot corona. We argue that above a halo mass of {\$}\backslashsim 10{\^{}}{\{}12{\}} M{\_}\backslashodot{\$}, the supernova-driven outflow is no longer buoyant and star formation is unable to prevent the build up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers. We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations, and demonstrate that, so long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice. The transition mass disappears entirely, however, if star formation driven outflows are absent.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Ding2016, -abstract = {The empirical correlation between the mass of a supermassive black hole (MBH) and its host galaxy properties is widely considered to be an evidence of their co-evolution. A powerful way to test the co-evolution scenario and learn about the feedback processes linking galaxies and nuclear activity is to measure these correlations as a function of redshift. Unfortunately, currently MBH can only be estimated in active galaxies at cosmological distances. At these distances, bright active galactic nuclei (AGNs) can outshine the host galaxy, making it extremely difficult to measure the host's luminosity. Strongly lensed AGNs provide in principle a great opportunity to improve the sensitivity and accuracy of the host galaxy luminosity measurements as the host galaxy is magnified and more easily separated from the point source, provided the lens model is sufficiently accurate. In order to measure the MBH-L correlation with strong lensing, it is necessary to ensure that the lens modelling is accurate, and that the host galaxy luminosity can be recovered to at least a precision and accuracy better than that of the typical MBH measurement. We carry out extensive and realistic simulations of deep Hubble Space Telescope observations of lensed AGNs obtained by our collaboration. We show that the host galaxy luminosity can be recovered with better accuracy and precision than the typical uncertainty in MBH($\sim$0.5 dex) for hosts as faint as 2-4 mag dimmer than the AGN itself. Our simulations will be used to estimate bias and uncertainties in the actual measurements to be presented in a future paper.}, -archivePrefix = {arXiv}, -arxivId = {1610.08504}, -author = {Ding, Xuheng and Liao, Kai and Treu, Tommaso and Suyu, Sherry H. and Chen, Geoff C.F. and Auger, Matthew W. and Marshall, Philip J. and Agnello, Adriano and Courbin, Frederic and Nierenberg, Anna M. and Rusu, Cristian E. and Sluse, Dominique and Sonnenfeld, Alessandro and Wong, Kenneth C.}, -doi = {10.1093/mnras/stw3078}, -eprint = {1610.08504}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ding et al. - 2017 - H0LiCOW. VI. Testing the fidelity of lensed quasar host galaxy reconstruction.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: evolution}, -number = {4}, -pages = {4634--4649}, -title = {{H0LiCOW. VI. Testing the fidelity of lensed quasar host galaxy reconstruction}}, -url = {http://arxiv.org/abs/1610.08504}, -volume = {465}, -year = {2017} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo {\textgreater} 1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from ˜30° to 10° for M ˜ 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@misc{DElia1998, -abstract = {Despite its proximity to other well studied islands, Cebu has received little attention from herpetologists, most likely because of early deforestation and the perception very little natural habitat remains for amphibians and reptiles. In this study, we present a preliminary assessment of island's herpetofauna, focusing our field work on Cebu's last remaining forest fragments and synthesizing all available historical museum distribution data. We surveyed amphibians and reptile populations using standardized methods to allow for comparisons between sites and assess sufficiency of sampling effort. Fieldwork resulted in a total of 27 species recorded from five study sites, complementing the 58 species previously known from the island. Together, our data and historical museum records increase the known number of Cebu's resident species to 13 amphibians (frogs) and 63 reptiles (lizards, snakes, turtle, crocodile). We recorded the continued persistence Cebu's rare and endemic lizard (Brachymeles cebuensis) and secretive snakes such as Malayotyphlops hypogius, and Ramphotyhlops cumingii, which persist despite Cebu's long history of widespread and continuous habitat degradation. Most species encountered, including common and widespread taxa, appeared to persist at low population abundances. To facilitate the immediate recovery of the remaining forest fragments, and resident herpetofauna, conservation effort must be sustained. However, prior to any conservation interventions, ecological baselines must be established to inform the process of recovery.}, -archivePrefix = {arXiv}, -arxivId = {1511.07122}, -author = {Supsup, Christian E. and Puna, Nevong M. and Asis, Augusto A. and Redoblado, Bernard R. and Panaguinit, Maria Fatima G. and Guinto, Faith M. and Rico, Edmund B. and Diesmos, Arvin C. and Brown, Rafe M. and Mallari, Neil Aldrin D.}, -booktitle = {Asian Herpetological Research}, -doi = {10.16373/j.cnki.ahr.150049}, -eprint = {1511.07122}, -isbn = {0894-0282}, -issn = {20950357}, -keywords = {Cebu,Deforestation,Frogs,Lizards,Philippines,Snakes}, -number = {3}, -pages = {151--179}, -pmid = {22352717}, -title = {{Amphibians and reptiles of Cebu, Philippines: The poorly understood herpetofauna of an Island with very little remaining natural habitat}}, -volume = {7}, -year = {2016} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance LCDM cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for `radio' feedback from those AGN that lie at the centre of a quasistatic X-ray emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models which might explain the accretion rate scalings required for our phenomenological `radio mode' model to be successful.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J and Springel, Volker and White, Simon D M and {De Lucia}, G and Frenk, C S and Gao, L and Jenkins, A and Kauffmann, G and Navarro, J F and Yoshida, N}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Laporte2013, -abstract = {We study the formation and evolution of brightest cluster galaxies starting from a z = 2 population of quiescent ellipticals and following them to z = 0. To this end, we use a suite of nine high-resolution dark matter only simulations of galaxy clusters in a $\lambda$ cold dark matter ($\lambda$CDM)universe.We develop a scheme inwhich simulation particles are weighted to generate realistic and dynamically stable stellar density profiles at z = 2. Our initial conditions assign a stellar mass to every identified dark halo as expected from abundance matching; assuming that there exists a one-to-one relation between the visible properties of galaxies and their host haloes. We setthe sizes of the luminous components according to the observed relations for z $\sim$ 2 massive quiescent galaxies. We study the evolution of the mass-sizerelation, the fate of satellite galaxies and the mass aggregation of the cluster central. From z = 2, these galaxies grow on average in size by a factor of 5 to 10 and in galaxy mass by 2 to 3. The stellar mass of our simulated BCGs grow by a factor of $\sim$2.1 in the range 0.3 < z < 1.0, consistent with observations, and by a factor of $\sim$1.4 in the range 0.0 < z<0.3. Furthermore, the non-central galaxies evolve on to the present-day mass-size relation by z = 0. Assuming passively evolving stellar populations, we present surface brightness profiles for our cluster centrals which resemble those observed for the cDs in similar mass clusters both at z = 0 and at z = 1. This demonstrates that the $\lambda$CDM cosmology does indeed predict minor and major mergers to occur in galaxy clusters with the frequency and mass ratio distribution required to explain the observed growth in size of passive galaxies since z = 2. Our experiment shows that brightest cluster galaxies could, inprinciple, form through dissipationless mergers of quiescent massive z = 2 galaxies, without substantial additional star formation. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1301.5319}, -author = {Laporte, Chervin F.P. and White, Simon D.M. and Naab, Thorsten and Gao, Liang}, -doi = {10.1093/mnras/stt912}, -eprint = {1301.5319}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Laporte et al. - 2013 - The growth in size and mass of cluster galaxies since z = 2(2).pdf:pdf}, -isbn = {9781450301992}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Clusters: General,Galaxies,Galaxies: Elliptical and lenticular: cD,Galaxies: Evolution,Galaxies: Formation}, -number = {2}, -pages = {901--909}, -title = {{The growth in size and mass of cluster galaxies since z = 2}}, -volume = {435}, -year = {2013} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance $\Lambda$ cold dark matter cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for 'radio' feedback from those active galactic nuclei that lie at the centre of a quasi-static X-ray-emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models that might explain the accretion rate scalings required for our phenomenological 'radio mode' model to be successful. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J and Springel, Volker and White, Simon D M and {De Lucia}, G and Frenk, C S and Gao, L and Jenkins, A and Kauffmann, G and Navarro, J F and Yoshida, N}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Salvatier2016, -abstract = {Probabilistic programming allows for automatic Bayesian inference on user-defined probabilistic models. Recent advances in Markov chain Monte Carlo (MCMC) sampling allow inference on increasingly complex models. This class of MCMC, known as Hamiltonian Monte Carlo, requires gradient information which is often not readily available. PyMC3 is a new open source probabilistic programming framework written in Python that uses Theano to compute gradients via automatic differentiation as well as compile probabilistic programs on-the-fly to C for increased speed. Contrary to other probabilistic programming languages, PyMC3 allows model specification directly in Python code. The lack of a domain specific language allows for great flexibility and direct interaction with the model. This paper is a tutorial-style introduction to this software package.}, -archivePrefix = {arXiv}, -arxivId = {1507.08050}, -author = {Salvatier, John and Wiecki, Thomas V and Fonnesbeck, Christopher}, -doi = {10.7717/peerj-cs.55}, -eprint = {1507.08050}, -issn = {23765992}, -journal = {PeerJ Computer Science}, -keywords = {Bayesian statistic,Markov chain Monte Carlo,Probabilistic Programming,Python,Statistical modeling}, -number = {4}, -pages = {1--24}, -title = {{Probabilistic programming in Python using PyMC3}}, -volume = {2016}, -year = {2016} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M{\_}*/M{\_}sun) {\textgreater} 11.5 (M{\_}K {\textless} -25.3 mag) and distance D {\textless} 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38$\backslash$pm6{\%} down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80$\backslash$pm10{\%} and 28$\backslash$pm6{\%}, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R{\_}e), and the gas morphologies are diverse, with 17/28 = 61$\backslash$pm9{\%} being centrally concentrated, 8/28 = 29$\backslash$pm9{\%} exhibiting clear rotation out to several kpc, and 3/28 = 11$\backslash$pm6{\%} being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly {\$\sim${}}10{\^{}}5M{\_}sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A and Blakeslee, John P and Goulding, Andy D and McConnell, Nicholas J and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{Gomer2018, -abstract = {The positions of multiple images in galaxy lenses are related to the galaxy mass distribution. Smooth elliptical mass profiles were previously shown to be inadequate in reproducing the quad population. In this paper, we explore the deviations from such smooth elliptical mass distributions. Unlike most other work, we use a model-free approach based on the relative polar image angles of quads, and their position in 3D space with respect to the fundamental surface of quads (FSQ). The FSQ is defined by quads produced by elliptical lenses. We have generated thousands of quads from synthetic populations of lenses with substructure consistent with Lambda cold dark matter ($\Lambda$CDM) simulations, and found that such perturbations are not sufficient to match the observed distribution of quads relative to the FSQ. The result is unchanged even when subhalo masses are increased by a factor of 10, and the most optimistic lensing selection bias is applied. We then produce quads from galaxies created using two components, representing baryons and dark matter. The transition from the mass being dominated by baryons in inner radii to being dominated by dark matter in outer radii can carry with it asymmetries, which would affect relative image angles. We run preliminary experiments using lenses with two elliptical mass components with non-identical axial ratios and position angles, perturbations from ellipticity in the form of non-zero Fourier coefficients a4 and a6, and artificially offset ellipse centres as a proxy for asymmetry at image radii. We show that combination of these effects is a promising way of accounting for quad population properties. We conclude that the quad population provides a unique and sensitive tool for constraining detailed mass distribution in the centres of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1712.07665}, -author = {Gomer, Matthew R. and Williams, Liliya L.R.}, -doi = {10.1093/mnras/stx3294}, -eprint = {1712.07665}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gomer, Williams - 2018 - The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1987--2002}, -title = {{The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses}}, -volume = {475}, -year = {2018} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Schneider2014a, -abstract = {The main obstacle that gravitational lensing has in determining accurate masses of deflectors, or in determining precise estimates for the Hubble constant, is the degeneracy of lensing observables with respect to the mass-sheet transformation (MST). The MST is a global modification of the mass distribution which leaves all image positions, shapes, and flux ratios invariant, but which changes the time delay. Here we show that another global transformation of lensing mass distributions exists which leaves image positions and flux ratios almost invariant, and of which the MST is a special case. As is the case for the MST, this new transformation only applies if one considers only those source components that are at the same distance from us. Whereas for axi-symmetric lenses this source position transformation exactly reproduces all strong lensing observables, it does so only approximately for more general lens situations. We provide crude estimates for the accuracy with which the transformed mass distribution can reproduce the same image positions as the original lens model, and present an illustrative example of its performance. This new invariance transformation is most likely the reason why the same strong lensing information can be accounted for with rather different mass models. {\textcopyright} 2014 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1306.4675}, -author = {Schneider, Peter and Sluse, Dominique}, -doi = {10.1051/0004-6361/201322106}, -eprint = {1306.4675}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Schneider2013SPT.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Cosmological parameters,Gravitational lensing: strong}, -title = {{Source-position transformation: An approximate invariance in strong gravitational lensing}}, -volume = {564}, -year = {2014} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) 'CMASS' sample at z $\sim$ 0.5. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogues which include selection effects, reproduce the overall SMF, the projected two-point correlation function wp, the CMASS dn/dz, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of 'age matching' and show that these effects are markedly different compared to the ones explored by Hearin et al. at lower stellar masses. We construct two models, one in which galaxy colour is stochastic ('AbM' model) as well as a model which contains assembly bias effects ('AgM' model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colours are not a stochastic process in high-mass haloes. Our results suggest that the colours of galaxies in high-mass haloes are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P. and Bundy, Kevin and Zentner, Andrew R. and Behroozi, Peter S. and Reid, Beth A. and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L. and White, Martin and Schneider, Donald P.}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Saito et al. - 2016 - Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass.pdf:pdf}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Furlong:2017aa, -abstract = {We present the evolution of galaxy sizes, from redshift 2 to 0, for actively star forming and passive galaxies in the cosmological hydrodynamical 1003 cMpc3 simulation of the EAGLE project. We find that the sizes increase with stellar mass, but that the relation weakens with increasing redshift. Separating galaxies by their star formation activity, we find that passive galaxies are typically smaller than active galaxies at a fixed stellar mass. These trends are consistent with those found in observations and the level of agreement between the predicted and observed size-mass relations is of the order of 0.1 dex for z < 1 and 0.2-0.3 dex from redshift 1 to 2. We use the simulation to compare the evolution of individual galaxies with that of the population as a whole. While the evolution of the size-stellar mass relation for active galaxies provides a good proxy for the evolution of individual galaxies, the evolution of individual passive galaxies is not well represented by the observed size-mass relation due to the evolving number density of passive galaxies. Observations of z $\sim$ 2 galaxies have revealed an abundance of massive red compact galaxies, which depletes below z $\sim$ 1. We find that a similar population forms naturally in the simulation. Comparing these galaxies with their z = 0 descendants, we find that all compact galaxies grow in size due to the high-redshift stars migrating outwards. Approximately 60 per cent of the compact galaxies increase in size further due to renewed star formation and/or mergers.}, -archivePrefix = {arXiv}, -arxivId = {1510.05645}, -author = {Furlong, M. and Bower, R. G. and Crain, R. A. and Schaye, J. and Theuns, T. and Trayford, J. W. and Qu, Y. and Schaller, M. and Berthet, M. and Helly, J. C.}, -doi = {10.1093/mnras/stw2740}, -eprint = {1510.05645}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Furlong et al. - 2017 - Size evolution of normal and compact galaxies in the EAGLE simulation(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: star formation,Galaxies: structure}, -month = {feb}, -number = {1}, -pages = {722--738}, -title = {{Size evolution of normal and compact galaxies in the EAGLE simulation}}, -volume = {465}, -year = {2017} -} -@article{Greene2017, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless}M{\_}200b {\textless}10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater}10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20{\$}\backslash{\$}{\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, Jenny E and Leauthaud, Alexie and Emsellem, Eric and Ge, J and Arag'on-Salamanca, A and Greco, J P and Lin, Y -T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -pages = {1--23}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -year = {2017} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani}, and Nelson Caldwell}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani - 2002 - EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXI(2).pdf:pdf}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Tajalli2025, -abstract = {We present an extended analysis of the gravitational lens systems SDSS J0946+1006 and JVAS B1938+666. We focus on the properties of two low-mass dark matter haloes previously detected in these systems and compare them with predictions from different dark matter models. In agreement with previous studies, we find that the object H detected in J0946+1006 is a dark-matter-dominated subhalo. Object A, in B1938+666, is a foreground halo at $z = 0.13\pm0.07$, contradicting previous analyses which suggested this object to be located either within or at higher redshift than the lens. Given the new redshift for this object, we update the 3$\sigma$ upper limit on its luminosity to $L_V < 6.3 \times 10^5 {(z/0.13)}^2 L_{V,\odot}$. By selecting central galaxies from the TNG50 hydrodynamical simulation, we find that analogues with projected mass density profiles around the robust radius of $\sim$ 91 pc and luminosities consistent with detection A can be found, although they lie near the edge of the halo distribution in the relevant mass and redshift ranges. We conclude, therefore, that this object is an atypical but possible event in $\Lambda$CDM. The projected mass density profile of both detections over the well-constrained range of radii may be consistent with expectations from SIDM gravothermal fluid model if the effective self-interaction cross-section $\sigma_{c,0}/m_{\rm{dm}}$ is of order $300 \ \rm{cm}^2 g^{-1}$ or larger.}, -archivePrefix = {arXiv}, -arxivId = {2505.07944}, -author = {Tajalli, Maryam and Vegetti, Simona and O'Riordan, Conor M. and White, Simon D. M. and Fassnacht, Christopher D. and Powell, Devon M. and McKean, J. P. and Despali, Giulia}, -eprint = {2505.07944}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Tajali2025DM.pdf:pdf}, -keywords = {cosmology,dark matter,galaxies,gravitational lensing,haloes,strong,structure}, -number = {August}, -pages = {1--18}, -title = {{SHARP -- IX. The dense, low-mass perturbers in B1938+666 and J0946+1006: implications for cold and self-interacting dark matter}}, -url = {http://arxiv.org/abs/2505.07944}, -volume = {18}, -year = {2025} -} -@article{Shajib2021, -abstract = {We investigate the internal structure of elliptical galaxies at z ∼ 0.2 from a joint lensing-dynamics analysis. We model Hubble Space Telescope images of a sample of 23 galaxy-galaxy lenses selected from the Sloan Lens ACS (SLACS) survey. Whereas the original SLACS analysis estimated the logarithmic slopes by combining the kinematics with the imaging data, we estimate the logarithmic slopes only from the imaging data. We find that the distribution of the lensing-only logarithmic slopes has a median 2.08c ± 0.03 and intrinsic scatter 0.13 ± 0.02, consistent with the original SLACS analysis. We combine the lensing constraints with the stellar kinematics and weak lensing measurements, and constrain the amount of adiabatic contraction in the dark matter (DM) haloes. We find that the DM haloes are well described by a standard Navarro-Frenk-White halo with no contraction on average for both of a constant stellar mass-to-light ratio (M/L) model and a stellar M/L gradient model. For the M/L gradient model, we find that most galaxies are consistent with no M/L gradient. Comparison of our inferred stellar masses with those obtained from the stellar population synthesis method supports a heavy initial mass function (IMF) such as the Salpeter IMF. We discuss our results in the context of previous observations and simulations, and argue that our result is consistent with a scenario in which active galactic nucleus feedback counteracts the baryonic-cooling-driven contraction in the DM haloes.}, -archivePrefix = {arXiv}, -arxivId = {2008.11724}, -author = {Shajib, Anowar J. and Treu, Tommaso and Birrer, Simon and Sonnenfeld, Alessandro}, -doi = {10.1093/mnras/stab536}, -eprint = {2008.11724}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Shajib2021MassSlopeNFW.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: elliptical,Gravitational lensing: strong,Lenticular,cD}, -number = {2}, -pages = {2380--2405}, -publisher = {Oxford University Press}, -title = {{Dark matter haloes of massive elliptical galaxies at z ∼ 0.2 are well described by the Navarro-Frenk-White profile}}, -volume = {503}, -year = {2021} -} -@article{Kruk2017, -abstract = {We use multi-wavelength SDSS images and Galaxy Zoo morphologies to identify a sample of {\$}\backslashsim{\$}{\$}270{\$} late-type galaxies with an off-centre bar. We measure offsets in the range 0.2-2.5 kpc between the photometric centres of the stellar disc and stellar bar. The measured offsets correlate with global asymmetries of the galaxies, with those with largest offsets showing higher lopsidedness. These findings are in good agreement with predictions from simulations of dwarf-dwarf tidal interactions producing off-centre bars. We find that the majority of galaxies with off-centre bars are of Magellanic type, with a median mass of {\$}10{\^{}}{\{}9.6{\}} M{\_}{\{}\backslashodot{\}}{\$}, and 91{\%} of them having {\$}M{\_}{\{}\backslashstar{\}}{\textless}3\backslashtimes10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}, the characteristic mass at which galaxies start having higher central concentrations attributed to the presence of bulges. We conduct a search for companions to test the hypothesis of tidal interactions, but find that a similar fraction of galaxies with offset bars have companions within 100 kpc as galaxies with centred bars. Although this may be due to the incompleteness of the SDSS spectroscopic survey at the faint end, alternative scenarios that give rise to offset bars such as interactions with dark companions or the effect of lopsided halo potentials should be considered. Future observations are needed to confirm possible low mass companion candidates and to determine the shape of the dark matter halo, in order to find the explanation for the off-centre bars in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1705.00007}, -author = {Kruk, Sandor J and Lintott, Chris J and Simmons, Brooke D and Bamford, Steven P and Cardamone, Carolin N and Fortson, Lucy and Hart, Ross E and H{\"{a}}u{\ss}ler, Boris and Masters, Karen L and Nichol, Robert C and Schawinski, Kevin and Smethurst, Rebecca J}, -doi = {10.1093/mnras/stx1026}, -eprint = {1705.00007}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: dwarf,Galaxies: evolution,Galaxies: interactions,Galaxies: irregular,Galaxies: structure}, -number = {3}, -pages = {3363--3373}, -title = {{Galaxy Zoo: Finding offset discs and bars in SDSS galaxies}}, -url = {http://arxiv.org/abs/1705.00007%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1026}, -volume = {469}, -year = {2017} -} -@article{Peng2010, -abstract = {We present a two-dimensional (2D) fitting algorithm (GALFIT, ver. 3) with new capabilities to study the structural components of galaxies and other astronomical objects in digital images. Our technique improves on previous 2D fitting algorithms by allowing for irregular, curved, logarithmic and power-law spirals, ring, and truncated shapes in otherwise traditional parametric functions like the S{\'{e}}rsic, Moffat, King, Ferrer, etc., profiles. One can mix and match these new shape features freely, with or without constraints, and apply them to an arbitrary number of model components of numerous profile types, so as to produce realistic-looking galaxy model images. Yet, despite the potential for extreme complexity, the meaning of the key parameters like the S{\'{e}}rsic index, effective radius, or luminosity remains intuitive and essentially unchanged. The new features have an interesting potential for use to quantify the degree of asymmetry of galaxies, to quantify low surface brightness tidal features beneath and beyond luminous galaxies, to allow more realistic decompositions of galaxy subcomponents in the presence of strong rings and spiral arms, and to enable ways to gauge the uncertainties when decomposing galaxy subcomponents. We illustrate these new features by way of several case studies that display various levels of complexity. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0912.0731}, -author = {Peng, Chien Y. and Ho, Luis C. and Impey, Chris D. and Rix, Hans Walter}, -doi = {10.1088/0004-6256/139/6/2097}, -eprint = {0912.0731}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Peng et al. - 2010 - Detailed decomposition of galaxy images. II. beyond axisymmetric models.pdf:pdf}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Galaxies: bulges,Galaxies: fundamental parameters,Galaxies: structure,Techniques: image processing,Techniques: photometric}, -number = {6}, -pages = {2097--2129}, -title = {{Detailed decomposition of galaxy images. II. beyond axisymmetric models}}, -volume = {139}, -year = {2010} -} -@article{Bellstedt2018, -abstract = {We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 10}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A and Romanowsky, Aaron J and Remus, Rhea Silvia and Stevens, Adam R H and Brodie, Jean P and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to {\$\sim${}}4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, {\$}\backslashbackslashsigma(R){\$}, for 85 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute {\$}K{\$}-band magnitude {\$}M{\_}K {\textless}-25.3{\$} mag, or stellar mass {\$}M{\_}* {\textgreater}4 \backslashbackslashtimes 10{\^{}}{\{}11{\}} M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}}, within 108 Mpc. Our wide-field 107" {\$}\backslashbackslashtimes{\{}\backslash{\$}{\}} 107" IFS data cover radii as large as 40 kpc, for which we quantify separately the inner ({\$}{\textless}5{\$} kpc) and outer logarithmic slopes {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm inner{\}}{\$} and {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm outer{\}}{\$} of {\$}\backslashbackslashsigma(R){\$}. While {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm inner{\}}{\$} is mostly negative, of the 61 galaxies with sufficient radial coverage to determine {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm outer{\}}{\$} we find 33{\%} to have rising outer dispersion profiles ({\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm outer{\}} {\textgreater}0.03{\$}), 13{\%} to be flat ({\$}-0.03 {\textless}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm outer{\}} {\textless}0.03{\$}), and 54{\%} to be falling. The fraction of galaxies with rising outer profiles increases with {\$}M{\_}*{\$} and in denser galaxy environment, with the 11 most massive galaxies in our sample all having flat or rising dispersion profiles. The strongest environmental correlation is with halo mass, but weaker correlations with large-scale density and local density also exist. The average {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm outer{\}}{\$} is similar for brightest group galaxies, satellites, and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis {\$}h{\_}4{\$}. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z > 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G.}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2006 - Breaking the hierarchy of galaxy formation(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -publisher = {MNRAS}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Rojas2022, -abstract = {We present our search for strong lens, galaxy-scale systems in the first data release of the Dark Energy Survey (DES), based on a color-selected parent sample of 18 745 029 luminous red galaxies (LRGs). We used a convolutional neural network (CNN) to grade this LRG sample with values between 0 (non-lens) and 1 (lens). Our training set of mock lenses is data-driven, that is, it uses lensed sources taken from HST-COSMOS images and lensing galaxies from DES images of our LRG sample. A total of 76 582 cutouts were obtained with a score above 0.9, which were then visually inspected and classified into two catalogs. The first one contains 405 lens candidates, of which 90 present clear lensing features and counterparts, while the other 315 require more evidence, such as higher resolution imaging or spectra, to be conclusive. A total of 186 candidates are newly identified by our search, of which 16 are among the 90 most promising (best) candidates. The second catalog includes 539 ring galaxy candidates. This catalog will be a useful false positive sample for training future CNNs. For the 90 best lens candidates we carry out color-based deblending of the lens and source light without fitting any analytical profile to the data. This method is shown to be very efficient in the deblending, even for very compact objects and for objects with a complex morphology. Finally, from the 90 best lens candidates, we selected 52 systems with one single deflector to test an automated modeling pipeline that has the capacity to successfully model 79% of the sample within an acceptable computing runtime.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:2109.00014v1}, -author = {Rojas, K. and Savary, E. and Cl{\'{e}}ment, B. and Maus, M. and Courbin, F. and Lemon, C. and Chan, J. H.H. and Vernardos, G. and Joseph, R. and Ca{\~{n}}ameras, R. and Galan, A.}, -doi = {10.1051/0004-6361/202142119}, -eprint = {arXiv:2109.00014v1}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Rojas2022DESLensMOdelFinding.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Catalogs,Gravitational lensing: strong,Surveys,Techniques: image processing}, -pages = {1--37}, -title = {{Search of strong lens systems in the Dark Energy Survey using convolutional neural networks}}, -volume = {668}, -year = {2022} -} -@article{Oguri2014, -abstract = {We derive the average mass profile of elliptical galaxies from the ensemble of 161 strong gravitational lens systems selected from several surveys, assuming that the mass profile scales with the stellar mass and effective radius of each lensing galaxy. The total mass profile is well fitted by a power law$\rho$(r)$\alpha$r$\gamma$ with best-fitting slope $\gamma$ =-2.11±0.05. The decomposition of the total mass profile into stellar and dark matter distributions is difficult due to a fundamental degeneracy between the stellar initial mass function (IMF) and the dark matter fraction fDM. We demonstrate that this IMF-fDM degeneracy can be broken by adding direct stellar mass fraction measurements by quasar microlensing observations. Our best-fitting model prefers the Salpeter IMF over the Chabrier IMF and a smaller central dark matter fraction than that predicted by adiabatic contraction models. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1309.5408}, -author = {Oguri, Masamune and Rusu, Cristian E. and Falco, Emilio E.}, -doi = {10.1093/mnras/stu106}, -eprint = {1309.5408}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {CD-galaxies,Elliptical and lenticular,Formation-galaxies,Gravitational lensing,Haloes-dark matter,Strong-galaxies}, -number = {3}, -pages = {2494--2504}, -title = {{The stellar and dark matter distributions in elliptical galaxies from the ensemble of strong gravitational lenses}}, -volume = {439}, -year = {2014} -} -@article{Cholis2014, -abstract = {Several classes of astrophysical sources contribute to the approximately isotropic gamma-ray background measured by the Fermi Gamma-Ray Space Telescope. In this paper, we use Fermi's catalog of gamma-ray sources (along with corresponding source catalogs at infrared and radio wavelengths) to build and constrain a model for the contributions to the extragalactic gamma-ray background from astrophysical sources, including radio galaxies, star-forming galaxies, and blazars. We then combine our model with Fermi's measurement of the gamma-ray background to derive constraints on the dark matter annihilation cross section, including contributions from both extragalactic and galactic halos and subhalos. The resulting constraints are competitive with the strongest current constraints from the Galactic Center and dwarf spheroidal galaxies. As Fermi continues to measure the gamma-ray emission from a greater number of astrophysical sources, it will become possible to more tightly constrain the astrophysical contributions to the extragalactic gamma-ray background. We project that with 10 years of data, Fermi's measurement of this background combined with the improved constraints on the astrophysical source contributions will yield a sensitivity to dark matter annihilations that exceeds the strongest current constraints by a factor of ∼ 5-10.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1312.0608v1}, -author = {Cholis, Ilias and Hooper, Dan and McDermott, Samuel D.}, -doi = {10.1088/1475-7516/2014/02/014}, -eprint = {arXiv:1312.0608v1}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark matter theory,gamma ray theory}, -number = {2}, -pages = {014--014}, -title = {{Dissecting the gamma-ray background in search of dark matter}}, -url = {http://stacks.iop.org/1475-7516/2014/i=02/a=014?key=crossref.524e7c5d7dd5417a10056684646b065c}, -volume = {2014}, -year = {2014} -} -@article{Li2008, -abstract = {We analyze properties of subhalos/substructures resolved in a dark matter simulation of a Milky Way-like halo in a $\Lambda$CDM cosmology. We explore possible links between subhalos and the Galactic satellites and find: 1) The infall patterns of subhalos are slightly elongated along the major axis of the galaxy halo and are clumpy on smaller scales. 2) The Great disk defined by MW satellites (Kroupa et al. 2005) is easily reproduced in our simulations without recurring to sophisticated galaxy formation recipes and is purely due to their highly centrally concentrated distribution around the Galaxy.}, -archivePrefix = {arXiv}, -arxivId = {0807.2780}, -author = {Li, Yang Shyang and Helmi, Amina}, -doi = {10.1007/978-1-4020-5573-7_53}, -eprint = {0807.2780}, -isbn = {0000000000000}, -issn = {15706605}, -journal = {Astrophysics and Space Science Proceedings}, -keywords = {Dark matter,Galaxies: Dwarf,Galaxies: Kinematics and dynamics,Galaxy: Formation,Methods: Numerical}, -number = {202409}, -pages = {311--314}, -title = {{Infall of substructures onto a milky way-like dark halo}}, -volume = {385}, -year = {2007} -} -@article{Klypin1999, -abstract = {Using published data, we have compiled the circular velocity (Vc) distribution function (VDF) of galaxy satellites in the Local Group. We find that within the volumes of radius of 570 kpc (400/h kpc for h=0.7) centered on the Milky Way and Andromeda, the average VDF is roughly approximated as n(>Vc)$\sim$ 45(Vc/10 km/s)^{-1} h^3 Mpc^{-3} for Vc in the range $\sim$10-70 km/s. The observed VDF is compared with results of high-resolution cosmological simulations. We find that the VDF in models is very different from the observed one: n(>Vc)$\sim$1200(Vc/10 km/s)^{-2.75}h^3 Mpc^{-3}. Cosmological models thus predict that a halo of the size of our Galaxy should have about 50 dark matter satellites with circular velocity >20 km/s and mass >3x10^8/h Msun within a 570 kpc radius. This number is significantly higher than the approximate dozen satellites actually observed around our Galaxy. The observed and predicted VDFs cross at $\sim$50 km/s, indicating that the predicted abundance of satellites with Vc> 50 km/s is in reasonably good agreement with observations. We conclude, therefore, that unless a large fraction of the Local Group satellites has been missed in observations, there is a dramatic discrepancy between observations and hierarchical models, regardless of the model parameters. We discuss several possible explanations for this discrepancy including identification of some satellites with the High Velocity Clouds observed in the Local Group, and the existence of dark satellites that failed to accrete gas and form stars due either to the expulsion of gas in the supernovae-driven winds or to gas heating by the intergalactic ionizing background. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9901240}, -author = {Klypin, Anatoly and Kravtsov, Andrey V. and Valenzuela, Octavio and Prada, Francisco}, -doi = {10.1086/307643}, -eprint = {9901240}, -isbn = {0021-9258 (Print)\r0021-9258 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: THEORY,Cosmology: Theory,GALAXIES: CLUSTERS: GENERAL,GALAXIES: INTERACTIONS,GALAXIES: LOCAL GROUP,GALAXY: FORMATION,Galaxies: Clusters: General,Galaxies: Interactions,Galaxies: Local Group,Galaxy: Formation,METHODS: NUMERICAL,Methods: Numerical}, -month = {sep}, -number = {1}, -pages = {82--92}, -pmid = {11553635}, -primaryClass = {astro-ph}, -title = {{Where Are the Missing Galactic Satellites?}}, -url = {http://arxiv.org/abs/astro-ph/9901240%0Ahttp://dx.doi.org/10.1086/307643}, -volume = {522}, -year = {1999} -} -@article{Pontzen2015a, -abstract = {Galaxies and the dark matter haloes that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealized calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter core-creation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are 'maximally stable', i.e. that do not evolve at first order when external potentials (which arise from baryons, large-scale tidal fields or infalling substructure) are applied. We show that a spherically symmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for near-isotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealized spherically symmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter haloes (formed in collisionless cosmological simulations) nearly attain our maximally stable limit, but their evolution freezes out before reaching it.}, -archivePrefix = {arXiv}, -arxivId = {1502.07356}, -author = {Pontzen, Andrew and Read, Justin I and Teyssier, Romain and Governato, Fabio and Gualandris, Alessia and Roth, Nina and Devriendt, Julien}, -doi = {10.1093/mnras/stv1032}, -eprint = {1502.07356}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {1366--1379}, -title = {{Milking the spherical cow - on aspherical dynamics in spherical coordinates}}, -volume = {451}, -year = {2015} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1138?key=crossref.6ebb2a01dc7b45f1fa5c66089a37542b}, -volume = {709}, -year = {2010} -} -@article{Gomer2018, -abstract = {The positions of multiple images in galaxy lenses are related to the galaxy mass distribution. Smooth elliptical mass profiles were previously shown to be inadequate in reproducing the quad population. In this paper, we explore the deviations from such smooth elliptical mass distributions. Unlike most other work, we use a model-free approach based on the relative polar image angles of quads, and their position in 3D space with respect to the fundamental surface of quads (FSQ). The FSQ is defined by quads produced by elliptical lenses. We have generated thousands of quads from synthetic populations of lenses with substructure consistent with Lambda cold dark matter ($\Lambda$CDM) simulations, and found that such perturbations are not sufficient to match the observed distribution of quads relative to the FSQ. The result is unchanged even when subhalo masses are increased by a factor of 10, and the most optimistic lensing selection bias is applied. We then produce quads from galaxies created using two components, representing baryons and dark matter. The transition from the mass being dominated by baryons in inner radii to being dominated by dark matter in outer radii can carry with it asymmetries, which would affect relative image angles. We run preliminary experiments using lenses with two elliptical mass components with non-identical axial ratios and position angles, perturbations from ellipticity in the form of non-zero Fourier coefficients a4 and a6, and artificially offset ellipse centres as a proxy for asymmetry at image radii. We show that combination of these effects is a promising way of accounting for quad population properties. We conclude that the quad population provides a unique and sensitive tool for constraining detailed mass distribution in the centres of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1712.07665}, -author = {Gomer, Matthew R. and Williams, Liliya L.R.}, -doi = {10.1093/mnras/stx3294}, -eprint = {1712.07665}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gomer, Williams - 2018 - The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1987--2002}, -title = {{The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses}}, -volume = {475}, -year = {2018} -} -@article{RomanoDiaz2010, -abstract = {We compare the substructure evolution in pure dark matter (DM) halos with those in the presence of baryons, hereafter PDM and BDM models, respectively. The prime halos have been analyzed in the previous work. Models have been evolved from identical initial conditions which have been constructed by means of the constrained realization method. The BDM model includes star formation and feedback from stellar evolution onto the gas. A comprehensive catalog of subhalo populations has been compiled and individual and statistical properties of subhalos analyzed, including their orbital differences. We find that subhalo population mass functions in PDM and BDM are consistent with a single power law, M $\alpha$sbh, for each of the models in the mass range of ∼ 2 × 108 M ⊙-2 × 1011 M ⊙. However, we detect a nonnegligible shift between these functions, the time-averaged $\alpha$ ∼ -0.86 for the PDM and -0.98 for the BDM models. Overall, $\alpha$ appears to be a nearly constant in time, with variations of ± 15%. Second, we find that the radial mass distribution of subhalo populations can be approximated by a power law, with a steepening that occurs at the radius of a maximal circular velocity, R vmax, in the prime halos. Here we find that $\gamma$sbh ∼ -1.5 for the PDM and -1 for the BDM models, when averaged over time inside R vmax. The slope is steeper outside this region and approaches -3. We detect little spatial bias (less than 10%) between the subhalo populations and the DM distribution of the main halos. Also, the subhalo population exhibits much less triaxiality in the presence of baryons, in tandem with the shape of the prime halo. Finally, we find that, counter-intuitively, the BDM population is depleted at a faster rate than the PDM one within the central 30kpc of the prime halo. The reason for this is that although the baryons provide a substantial glue to the subhalos, the main halo exhibits the same trend. This assures a more efficient tidal disruption of the BDM subhalo population. However, this effect can be reversed for a more efficient feedback from stellar evolution and the central supermassive black holes, which will expel baryons from the center and decrease the central concentration of the prime halo. We compare our results with via Lactea and Aquarius simulations and other published results. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1002.4200}, -author = {Romano-D{\'{i}}az, Emilio and Shlosman, Isaac and Heller, Clayton and Hoffman, Yehuda}, -doi = {10.1088/0004-637X/716/2/1095}, -eprint = {1002.4200}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: interactions,Galaxies: kinematics and dynamics}, -month = {jun}, -number = {2}, -pages = {1095--1104}, -title = {{Dissecting galaxy formation. II. Comparing substructure in pure dark matter and baryonic models}}, -url = {http://stacks.iop.org/0004-637X/716/i=2/a=1095?key=crossref.1b77362a2a339033443db2676c609fe7}, -volume = {716}, -year = {2010} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centres of typical {\$\sim${}} L* and lower mass spheroids exhibit power-law 'cusps' with $\Sigma$ $\alpha$ R-$\eta$, where 0.5 ≲ $\eta$ ≲ 1 for radii {\$\sim${}} 1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for, or strongly modify, the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m = 1 lopsided/eccentric disc instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*({\textless} R) « MBH. When the stellar surface density profile is comparatively shallow with $\eta$ {\textless} 1/2, the modes cannot efficiently propagate to R = 0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than $\eta$ = 1, the inward propagation of eccentricity is strongly damped, suppressing inflow and bringing $\eta$ down again. Together these results produce an equilibrium slope of 1/2 ≲ $\eta$ ≲ 1 in the potential of the central black hole. These physical arguments are supported by non-linear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies. {\textcopyright}2010 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Goobar2016, -abstract = {We report the discovery of a multiply-imaged gravitationally lensed Type Ia supernova, iPTF16geu (SN 2016geu), at redshift $z=0.409$. This phenomenon could be identified because the light from the stellar explosion was magnified more than fifty times by the curvature of space around matter in an intervening galaxy. We used high spatial resolution observations to resolve four images of the lensed supernova, approximately 0.3" from the center of the foreground galaxy. The observations probe a physical scale of $\backslashsim{\$}1 kiloparsec, smaller than what is typical in other studies of extragalactic gravitational lensing. The large magnification and symmetric image configuration implies close alignment between the line-of-sight to the supernova and the lens. The relative magnifications of the four images provide evidence for sub-structures in the lensing galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1611.00014}, -author = {Goobar, A and Amanullah, R and Kulkarni, S R and Nugent, P E and Johansson, J and Steidel, C and Law, D and M{\"{o}}rtsell, E and Quimby, R and Blagorodnova, N and Brandeker, A and Cao, Y and Cooray, A and Ferretti, R and Fremling, C and Hangard, L and Kasliwal, M and Kupfer, T and Lunnan, R and Masci, F and Miller, A A and Nayyeri, H and Neill, J D and Ofek, E O and Papadogiannakis, S and Petrushevska, T and Ravi, V and Sollerman, J and Sullivan, M and Taddia, F and Walters, R and Wilson, D and Yan, L and Yaron, O}, -doi = {10.1126/science.aal2729}, -eprint = {1611.00014}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Goobar et al. - 2017 - IPTF16geu A multiply imaged, gravitationally lensed type ia supernova.pdf:pdf}, -isbn = {1095-9203 (Electronic) 0036-8075 (Linking)}, -issn = {10959203}, -journal = {Science}, -number = {6335}, -pages = {291--295}, -pmid = {28428419}, -title = {{IPTF16geu: A multiply imaged, gravitationally lensed type ia supernova}}, -url = {http://arxiv.org/abs/1611.00014}, -volume = {356}, -year = {2017} -} -@article{Pontzen2017, -abstract = {We show how the interplay between active galactic nuclei (AGNs) and merger history determines whether a galaxy quenches star formation (SF) at high redshift. We first simulate, in a full cosmological context, a galaxy of total dynamical mass Mvir = 1012M⊙ at z = 2. Then we systematically alter the accretion history of the galaxy by minimally changing the linear overdensity in the initial conditions. This 'genetic modification' approach allows the generation of three sets of $\Lambda$ CDM initial conditions leading to maximum merger ratios of 1:10, 1:5 and 2:3, respectively. The changes leave the final halo mass, large-scale structure and local environment unchanged, providing a controlled numerical experiment. Interaction between the AGN physics and mergers in the three cases leads, respectively, to a star-forming, temporarily quenched and permanently quenched galaxy. However, the differences do not primarily lie in the black hole accretion rates, but in the kinetic effects of the merger: the galaxy is resilient against AGN feedback unless its gaseous disc is first disrupted. Typical accretion rates are comparable in the three cases, falling below 0.1M⊙ yr-1, equivalent to around 2 per cent of the Eddington rate or 10-3 times the pre-quenching star formation rate, in agreement with observations. This low level of black hole accretion can be sustained even when there is insufficient dense cold gas for SF. Conversely, supernova feedback is too distributed to generate outflows in high-mass systems, and cannot maintain quenching over periods longer than the halo gas cooling time.}, -archivePrefix = {arXiv}, -arxivId = {1607.02507}, -author = {Pontzen, Andrew and Tremmel, Michael and Roth, Nina and Peiris, Hiranya V. and Saintonge, Am{\'{e}}lie and Volonteri, Marta and Quinn, Tom and Governato, Fabio}, -doi = {10.1093/mnras/stw2627}, -eprint = {1607.02507}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pontzen et al. - 2017 - How to quench a galaxy.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: star formation,Galaxies: stellar content}, -number = {1}, -pages = {547--558}, -title = {{How to quench a galaxy}}, -volume = {465}, -year = {2017} -} -@article{Skottfelt2017, -abstract = {The VIS instrument on board the Euclid mission is a weak-lensing experiment that depends on very precise shape measurements of distant galaxies obtained by a large CCD array. Due to the harsh radiative environment outside the Earth's atmosphere, it is anticipated that the CCDs over the mission lifetime will be degraded to an extent that these measurements will only be possible through the correction of radiation damage effects. We have therefore created a Monte Carlo model that simulates the physical processes taking place when transferring signal through a radiation-damaged CCD. The software is based on Shockley-Read-Hall theory, and is made to mimic the physical properties in the CCD as closely as possible. The code runs on a single electrode level and takes three dimensional trap position, potential structure of the pixel, and multi-level clocking into account. A key element of the model is that it also takes device specific simulations of electron density as a direct input, thereby avoiding to make any analytical assumptions about the size and density of the charge cloud. This paper illustrates how test data and simulated data can be compared in order to further our understanding of the positions and properties of the individual radiation-induced traps.}, -archivePrefix = {arXiv}, -arxivId = {1710.10958}, -author = {Skottfelt, Jesper and Hall, David J. and Gow, Jason P. D. and Murray, Neil J. and Holland, Andrew D. and Prod'homme, Thibaut}, -doi = {10.1117/1.jatis.3.2.028001}, -eprint = {1710.10958}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Skottfelt et al. - 2017 - Comparing simulations and test data of a radiation damaged charge-coupled device for the Euclid mission.pdf:pdf}, -issn = {2329-4124}, -journal = {J. Astron. Telesc. Instrum. Syst.}, -keywords = {ac,charge-coupled devices,image reconstruction,jesper,jesper skottfelt,open,radiation,simulations,skottfelt,uk}, -number = {2}, -pages = {028001}, -title = {{Comparing simulations and test data of a radiation damaged charge-coupled device for the Euclid mission}}, -url = {http://arxiv.org/abs/1710.10958%0Ahttp://dx.doi.org/10.1117/1.JATIS.3.2.028001}, -volume = {3}, -year = {2017} -} -@article{Hoekstra2004, -abstract = { We present the results of a study of the average mass profile around galaxies using weak gravitational lensing. We use 45.5 deg 2 of R C band imaging data from the Red-Sequence Cluster Survey (RCS) and define a sample of {\$\sim${}} 1.2 × 10 5 lenses with 19.5 {\textless} R C {\textless} 21, and a sample of {\$\sim${}} 1.5 × 10 6 background galaxies with 21.5 {\textless} R {\textless} 24. We constrain the power law scaling relations between the B -band luminosity and the mass and size of the halo, and find that the results are in excellent agreement with observed luminosity–line-width relations. Under the assumption that the luminosity does not evolve with redshift, the best fit NFW model yields a mass M 200 = (8.8±0.7) × 10 11 h –1 M ⊙ and a scale radius r s = I6.7+ 3.7 –3.0 h –1 kpc for a galaxy with a fiducial luminosity of L b = 10 10 h –2 L B⊙ . the latter result is in excellent agreement with predictions from numerical simulations for a halo of this mass. We also observe a signficant anisotropy of the lensing signal around the lenses, implying that the halos are flattened and aligned with the light distribution. We find an average (projected) halo ellipticity of 〈 e halo 〉 = 0.20 +0.04 –0.05 , in fair agreement with results from numerical simulations of CDM. Alternative theories of gravity (without dark matter) predict an isotropic lensing signal, which is excluded with 99.5{\%} confidence. Hence, our results provide strong support for the existence of dark matter. }, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, Howard K C and Gladders, Michael D}, -doi = {10.1086/382726}, -eprint = {0306515}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of galaxy dark matter halos from weak lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2003} -} -@article{Stark2013, -abstract = {Bright gravitationally lensed galaxies provide our most detailed view of galaxies at high redshift. The very brightest (r < 21) systems enable high spatial and spectral resolution measurements, offering unique constraints on the outflow energetics, metallicity gradients and stellar populations in high-redshift galaxies. Yet as a result of the small number of ultrabright z ≃ 2 lensed systems with confirmed redshifts, most detailed spectroscopic studies have been limited in their scope. With the goal of increasing the number of bright lensed galaxies available for detailed follow-up, we have undertaken a spectroscopic campaign targeting wide separation (≳3 arcsec) galaxy-galaxy lens candidates within the Sloan Digital Sky Survey (SDSS). Building on the earlier efforts of our Cambridge and Sloan Survey Of Wide Arcs in Thesky survey, we target a large sample of candidate galaxy-galaxy lens systems in SDSS using a well-established search algorithm which identifies blue arc-like structures situated around luminous red galaxies. In this paper, we present a new redshift catalogue containing 29 lensed sources in SDSS confirmed through spectroscopic follow-up of candidate galaxy-galaxy lens systems. Included in this new sample are two of the brightest galaxies (r=19.6 and 19.7) known at z ≃ 2, a low metallicity (12 + log (O/H) ≃ 8.0) extreme nebular line emitting galaxy at z = 1.43, and numerous systems for which detailed follow-up will be possible. The source redshifts span 0.9 1010 M⊙) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z ≳ 2, cSFGs present SFR = 100-200 M yr-1, yet their specific star formation rates (sSFR ∼ 10-9 yr -1) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (∼30%) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 108 yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z ∼ 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z ≳ 2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z ≲ 2) path in which larger SFGs form extended QGs without passing through a compact state. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1206.5000}, -author = {Barro, Guillermo and Faber, S. M. and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G. and Koo, David C. and Williams, Christina C. and Kocevski, Dale D. and Trump, Jonathan R. and Mozena, Mark and McGrath, Elizabeth and {Van Der Wel}, Arjen and Wuyts, Stijn and Bell, Eric F. and Croton, Darren J. and Daniel, Ceverino and Dekel, Avishai and Ashby, M. L.N. and Cheung, Edmond and Ferguson, Henry C. and Fontana, Adriano and Fang, Jerome and Giavalisco, Mauro and Grogin, Norman A. and Guo, Yicheng and Hathi, Nimish P. and Hopkins, Philip F. and Huang, Kuang Han and Koekemoer, Anton M. and Kartaltepe, Jeyhan S. and Lee, Kyoung Soo and Newman, Jeffrey A. and Porter, Lauren A. and Primack, Joel R. and Ryan, Russell E. and Rosario, David and Somerville, Rachel S. and Salvato, Mara and Hsu, Li Ting}, -doi = {10.1088/0004-637X/765/2/104}, -eprint = {1206.5000}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Barro et al. - 2013 - Candels The progenitors of compact quiescent galaxies at Z ∼ 2.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: high-redshift,galaxies: photometry,galaxies: starburst}, -number = {2}, -pmid = {7117407}, -title = {{Candels: The progenitors of compact quiescent galaxies at Z ∼ 2}}, -volume = {765}, -year = {2013} -} -@article{Schrabback2010, -abstract = {We present a comprehensive analysis of weak gravitational lensing by large-scale structure in the Hubble Space Telescope Cosmic Evolution Survey (COSMOS), in which we combine space-based galaxy shape measurements with ground-based photometric redshifts to study the redshift dependence of the lensing signal and constrain cosmological parameters. After applying our weak lensing-optimized data reduction, principal-component interpolation for the spatially, and temporally varying ACS point-spread function, and improved modelling of charge-transfer inefficiency, we measured a lensing signal that is consistent with pure gravitational modes and no significant shape systematics. We carefully estimated the statistical uncertainty from simulated COSMOS-like fields obtained from ray-tracing through the Millennium Simulation, including the full non-Gaussian sampling variance. We tested our lensing pipeline on simulated space-based data, recalibrated non-linear power spectrum corrections using the ray-tracing analysis, employed photometric redshift information to reduce potential contamination by intrinsic galaxy alignments, and marginalized over systematic uncertainties. We find that the weak lensing signal scales with redshift as expected from general relativity for a concordance $\Lambda$CDM cosmology, including the full cross-correlations between different redshift bins. Assuming a flat $\Lambda$CDM cosmology, we measure $\sigma$8($\Omega$ m/0.3)0.51 = 0.75±0.08 from lensing, in perfect agreement with WMAP-5, yielding joint constraints $\Omega$m = 0.266+0.025-0.023, $\sigma$8 = 0.802 +0.028-0.029 (all 68.3% conf.). Dropping the assumption of flatness and using priors from the HST Key Project and Big-Bang nucleosynthesis only, we find a negative deceleration parameter q0 at 94.3% confidence from the tomographic lensing analysis, providing independent evidence of the accelerated expansion of the Universe. For a flat wCDM cosmology and prior w $\epsilon$ [-2,0], we obtain w <-0.41 (90% conf.). Our dark energy constraints are still relatively weak solely due to the limited area of COSMOS. However, they provide an important demonstration of the usefulness of tomographic weak lensing measurements from space. {\textcopyright} ESO 2010.}, -archivePrefix = {arXiv}, -arxivId = {0911.0053}, -author = {Schrabback, T. and Hartlap, J. and Joachimi, B. and Kilbinger, M. and Simon, P. and Benabed, K. and Brada{\v{c}}, M. and Eifler, T. and Erben, T. and Fassnacht, C. D. and High, F. William and Hilbert, S. and Hildebrandt, H. and Hoekstra, H. and Kuijken, K. and Marshall, P. J. and Mellier, Y. and Morganson, E. and Schneider, P. and Semboloni, E. and {Van Waerbeke}, L. and Velander, M.}, -doi = {10.1051/0004-6361/200913577}, -eprint = {0911.0053}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Schrabback et al. - 2010 - Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {cosmological parameters,dark matter,gravitational lensing: weak,large-scale structure of Universe}, -number = {19}, -title = {{Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS}}, -volume = {516}, -year = {2010} -} -@article{Shi2015, -abstract = {We study how halo intrinsic dynamical properties are linked to their formation processes for halos in two mass ranges, 1012-1012.5 h-1M⊙ and ≥1013 h-1M⊙, and how both are correlated with the large-scale tidal field within which the halos reside at present. We identify infall halos that are about to merge with their hosts. We find that the tangential infall velocity increases significantly with the strength of the tidal field, but no strong correlation is found for the radial component. These results can be used to explain the environmental dependence of internal velocity anisotropy and spin of halos. The position vectors and velocities of infall halos are aligned with the principal axes of the tidal field, and the alignment depends on the strength of the tidal field. Opposite accretion patterns are found in weak and strong tidal fields, showing that in a weak field the accretion flow is dominated by radial motion within the local structure, while a large tangential component is present in a strong field. These findings can be used to understand the strong alignments we find between the principal axes of the internal velocity ellipsoids of halos and the tidal field, and their dependence on the strength of the tidal field. We further find that only in weak tidal fields does the spin-tidal field alignment follow the prediction of the tidal torque theory. We discuss how our results may be used to understand the spins of disk galaxies and velocity structures of elliptical galaxies and their correlations with large-scale structure.}, -archivePrefix = {arXiv}, -arxivId = {1501.07764}, -author = {Shi, Jingjing and Wang, Huiyuan and Mo, H J}, -doi = {10.1088/0004-637X/807/1/37}, -eprint = {1501.07764}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: halos,large-scale structure of universe,methods: statistical}, -number = {1}, -title = {{Flow Patterns Around Dark Matter Halos: the Link Between Halo Dynamical Properties and Large-Scale Tidal Field}}, -volume = {807}, -year = {2015} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ($\sim$100 deg2) and deep (>28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of $\sim$7000 massive galaxies at z $\sim$ 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E. and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2018 - Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 z 0.5 using Hyper Suprime-Cam(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 < z < 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Tinker2016, -abstract = {We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen etal (2012) clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of Mgal for galaxies with logMgal>=11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma_logM. Using this approach, we find sigma_logM=0.18^{+0.01}_{-0.02}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L. and Brownstein, Joel R. and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D. and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D.}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tinker et al. - 2017 - The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {121}, -title = {{The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -volume = {839}, -year = {2017} -} -@article{Governato2015, -abstract = {We use high-resolution Hydro+N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass {\$\sim${}}106-7 M⊙, total mass 1010 M⊙) in $\Lambda$-dominated cold dark matter (CDM) and 2 keV warm dark matter (WDM) cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the dark matter (DM) model, but proportionally to the SF efficiency, gas outflows lower the central mass density through 'dynamical heating', such that all realizations have circular velocities {\textless} 20 km s-1 at 500 pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial colour- magnitude diagrams and star formation histories (SFHs) in order to directly compare to available observations. The simulated galaxies formed most of their stars in many {\$\sim${}}10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including 'baryon physics' in simulations when (1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and (2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F and Weisz, D and Pontzen, A and Loebman, S and Reed, D and Brooks, A M and Behroozi, P and Christensen, C and Madau, P and Mayer, L and Shen, S and Walker, M and Quinn, T and Keller, B W and Wadsley, J}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Hopkins2009, -abstract = {Transformation of discs into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that the bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in haloes according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the overproduction of spheroids: low- and intermediate-mass galaxies are predicted to be bulge-dominated (B/T ∼ 0.5 at <10 10 M ⊙, with almost no 'bulgeless' systems), even if they have avoided major mergers. Including the different physical behaviour of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T ∼ 0.1 at <10 10 M ⊙, with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behaviour of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4111}, -author = {Hopkins, Philip F. and Somerville, Rachel S. and Cox, Thomas J. and Hernquist, Lars and Jogee, Shardha and Kere{\v{s}}, Dusan and Ma, Chung Pei and Robertson, Brant and Stewart, Kyle}, -doi = {10.1111/j.1365-2966.2009.14983.x}, -eprint = {0901.4111}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins et al. - 2009 - The effects of gas on morphological transformation in mergers Implications for bulge and disc demographics(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Galaxies: spiral}, -number = {2}, -pages = {802--814}, -title = {{The effects of gas on morphological transformation in mergers: Implications for bulge and disc demographics}}, -volume = {397}, -year = {2009} -} -@article{Schombert2015a, -abstract = {Using isophotal radius correlations for a sample of Two Micron All Sky Survey ellipticals, we have constructed a series of template surface brightness profiles to describe the profile shapes of ellipticals as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that ellipticals are weakly nonhomologous with respect to structure. Through comparison to the templates, it is discovered that ellipticals are divided into two families: those well matched to the templates, and a second class of ellipticals with distinctly shallower profile slopes. We refer to this second type of ellipticals as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D ellipticals cover the same range of luminosity, size, and kinematics as normal ellipticals, but maintain a signature of recent equal-mass dry mergers. We propose that normal ellipticals grow after an initial dissipation formation era by accretion of low-mass companions as outlined in hierarchical formation scenarios, while D ellipticals are the result of later equal-mass mergers producing shallow luminosity profiles.}, -archivePrefix = {arXiv}, -arxivId = {1509.08381}, -author = {Schombert, James M}, -doi = {10.1088/0004-6256/150/5/162}, -eprint = {1509.08381}, -isbn = {doi:10.1088/0004-6256/150/5/162}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: structure}, -number = {5}, -pages = {162}, -publisher = {IOP Publishing}, -title = {{The structure of galaxies. III. Two structural families of ellipticals}}, -url = {http://dx.doi.org/10.1088/0004-6256/150/5/162}, -volume = {150}, -year = {2015} -} -@article{Sonnenfeld2020, -abstract = {Context. Strong lenses are extremely useful probes of the distribution of matter on galaxy and cluster scales at cosmological distances, however, they are rare and difficult to find. The number of currently known lenses is on the order of 1000. Aims. The aim of this study is to use crowdsourcing to carry out a lens search targeting massive galaxies selected from over 442 square degrees of photometric data from the Hyper Suprime-Cam (HSC) survey. Methods. Based on the S16A internal data release of the HSC survey, we chose a sample of ∼300 000 galaxies with photometric redshifts in the range of 0.2 < zphot < 1.2 and photometrically inferred stellar masses of log M∗ > 11.2. We crowdsourced lens finding on this sample of galaxies on the Zooniverse platform as part of the Space Warps project. The sample was complemented by a large set of simulated lenses and visually selected non-lenses for training purposes. Nearly 6000 citizen volunteers participated in the experiment. In parallel, we used YATTALENS, an automated lens-finding algorithm, to look for lenses in the same sample of galaxies. Results. Based on a statistical analysis of classification data from the volunteers, we selected a sample of the most promising ∼1500 candidates, which we then visually inspected: half of them turned out to be possible (grade C) lenses or better. By including lenses found by YATTALENS or serendipitously noticed in the discussion section of the Space Warps website, we were able to find 14 definite lenses (grade A), 129 probable lenses (grade B), and 581 possible lenses. YATTALENS found half the number of lenses that were discovered via crowdsourcing. Conclusions. Crowdsourcing is able to produce samples of lens candidates with high completeness, when multiple images are clearly detected, and with higher purity compared to the currently available automated algorithms. A hybrid approach, in which the visual inspection of samples of lens candidates pre-selected by discovery algorithms or coupled to machine learning is crowdsourced, will be a viable option for lens finding in the 2020s, with forthcoming wide-area surveys such as LSST, Euclid, and WFIRST.}, -archivePrefix = {arXiv}, -arxivId = {2004.00634}, -author = {Sonnenfeld, Alessandro and Verma, Aprajita and More, Anupreeta and Baeten, Elisabeth and Macmillan, Christine and Wong, Kenneth C. and Chan, James H.H. and Jaelani, Anton T. and Lee, Chien Hsiu and Oguri, Masamune and Rusu, Cristian E. and Veldthuis, Marten and Trouille, Laura and Marshall, Philip J. and Hutchings, Roger and Allen, Campbell and {O' Donnell}, James and Cornen, Claude and Davis, Christopher P. and McMaster, Adam and Lintott, Chris and Miller, Grant}, -doi = {10.1051/0004-6361/202038067}, -eprint = {2004.00634}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnenfeld2020HSCLENSMODELINGFIND.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Galaxies: elliptical and lenticular,Gravitational lensing: strong,cD}, -pages = {1--19}, -title = {{Survey of Gravitationally-lensed Objects in HSC Imaging (SuGOHI): VI. Crowdsourced lens finding with Space Warps}}, -volume = {642}, -year = {2020} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/19158792}, -volume = {457}, -year = {2009} -} -@article{Wang2018c, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}} \backslashbackslashleqslant M{\_}{\{}\backslashbackslashast{\{}\backslash{\}}{\}} \backslashbackslashleqslant 10{\^{}}{\{}11.9{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashbackslashlangle\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}\backslashbackslashrangle = 2.003 \backslashbackslashpm 0.008{\$} and a standard deviation of {\$}\backslashbackslashsigma{\{}\backslash{\_}{\}}{\{}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}mw{\{}\backslash{\}}{\}}{\}}{\^{}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}-f{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}DM{\{}\backslash{\}}{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {1}, -year = {2018} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the LambdaCDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no statistically significant detection of a stellar halo, as in the case of M101, NGC3351 and NGC1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction f{\_}SH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming and assemble their dark matter halos on average earlier than galaxies with similar stellar masses. Accreted satellites are also lower in stellar mass and have earlier infall times than centrals with high f{\_}SH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretion-dominated r{\$\sim${}}45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers only at higher redshifts and evolved relatively unperturbed in the last {\$\sim${}}10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M and Sales, Laura V and Creasey, Peter and Cooper, Michael C and Bullock, James S and {Michael Rich}, R and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 < $\sigma$∗ < 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E. and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J. and Blakeslee, John P. and Thomas, Jens and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2015 - the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{VandeSande2016, -abstract = {Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h3 ({\$\sim${}}skewness) and h4 ({\$\sim${}}kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using 2D integral field data from the SAMI Galaxy Survey. A proxy for the spin parameter ({\$}\backslashlambda{\_}{\{}R{\_}e{\}}{\$}) and ellipticity ({\$}\backslashepsilon{\_}e{\$}) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h3 versus {\$}V/\backslashsigma{\$} anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h3 and {\$}V/\backslashsigma{\$}. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h3 versus {\$}V/\backslashsigma{\$} signatures. We identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar {\$}\backslashlambda{\_}{\{}R{\_}e{\}}-\backslashepsilon{\_}e{\$} values can show distinctly different h3-{\$}V/\backslashsigma{\$} signatures. Class 5 objects are previously unidentified fast rotators that show a weak h3 versus {\$}V/\backslashsigma{\$} anti-correlation. These objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h3 versus {\$}V/\backslashsigma{\$} as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.}, -archivePrefix = {arXiv}, -arxivId = {1611.07039}, -author = {van de Sande, Jesse and Bland-Hawthorn, Joss and Fogarty, Lisa M R and Cortese, Luca and D'Eugenio, Francesco and Croom, Scott M and Scott, Nicholas and Allen, James T and Brough, Sarah and Bryant, Julia J and Cecil, Gerald and Colless, Matthew and Couch, Warrick J and Davies, Roger and Elahi, Pascal J and Foster, Caroline and Goldstein, Greg and Goodwin, Michael and Groves, Brent and Ho, I-Ting and Jeong, Hyunjin and Jones, D Heath and Konstantopoulos, Iraklis S and Lawrence, Jon S and Leslie, Sarah K and Lopez-Sanchez, Angel R and McDermid, Richard M and McElroy, Rebecca and Medling, Anne M and Oh, Sree and Owers, Matt S and Richards, Samuel N and Schaefer, Adam L and Sharp, Rob and Sweet, Sarah M and Taranu, Dan and Tonini, Chiara and Walcher, C Jakob and Yi, Sukyoung K}, -doi = {10.3847/1538-4357/835/1/104}, -eprint = {1611.07039}, -issn = {1538-4357}, -keywords = {cosmology,dynamics,evolution,formation,galaxies,kinematics and,observations,stellar content,structure}, -title = {{The SAMI Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics}}, -url = {http://arxiv.org/abs/1611.07039%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/835/1/104}, -year = {2016} -} -@article{Navarro1991, -abstract = {We simulate the dynamical evolution of both collisionless "dark" particles and a dissipative gaseous ("baryonic") component in a flat universe in order to investigate the formation process of the luminous components of galaxies at the center of galactic dark halos. We assume that the initial density fluctuations are Gaussian with a power spectrum of the form P(k) ∝ K-1. Our models assume that the gas amounts to 10% of the mass of the universe, and that both the gas and the dark matter are identically distributed in phase space at high redshifts. The gas is allowed to dissipate energy according to a cooling function corresponding to an H-He mixture with primordial abundances. We neglect the effects of star formation and supernova explosions. Our results confirm previous suggestions that the merging history of the surrounding halo is a key factor in the determination of the morphological type of a galaxy. The baryonic component is found to lose more angular momentum than could be predicted by dissipationless simulations. We observe the formation of dense, slowly rotating baryonic cores at the center of galactic dark halos. This provides an attractive explanation for the origin of the slow rotation and large densities observed in spheroids and elliptical galaxies. On the other hand, the loss of angular momentum by the gaseous component is so important that prominent, rotationally supported disks like those of bright spirals did not appear to be able to form in our simulations. We conclude that these structures may only form in a scenario including mechanisms preventing the baryonic component from sinking in the deep cores of nonlinear clumps at high redshift and losing a large fraction of their angular momentum during subsequent mergers. We speculate that star formation and supernova explosions could provide such a mechanism, and that these processes are essential for the formation of spiral galaxies.}, -author = {Navarro, Julio F. and Benz, Willy}, -doi = {10.1086/170590}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Astronomical Models,Collisionless Plasmas,Computational Astrophysics,Cooling Flows (Astrophysics),Dark Matter,Elliptical Galaxies,Galactic Evolution,Galactic Rotation,Galactic Structure,Gas Dynamics,Halos}, -month = {oct}, -pages = {320}, -title = {{Dynamics of cooling gas in galactic dark halos}}, -url = {http://adsabs.harvard.edu/doi/10.1086/170590}, -volume = {380}, -year = {1991} -} -@article{Schombert2013, -abstract = {Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions; the r{\^{}}1/4 law and the Sersic r{\^{}}1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r{\^{}}1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpcs) and the outer regions (beyond the half-light radius) which do not have r{\^{}}1/4 shapes. It is found that the Sersic r{\^{}}1/n model produce good fits to the core regions of ellipticals (r {\textless}r{\_}half), but is an inadequate function for the entire profile of an elliptical from core to halo due to competing effects on the Sersic n index and the fact that the interior shape of an elliptical is only weakly correlated with its halo shape. In addition, there are a wide range of Sersic parameters that will equally describe the shape of the outer profile, degrading the Sersic models usefulness as a describer of the entire profile. Empirically determined parameters, such as half-light radius and total luminosity, have less scatter than fitting function variables. The scaling relations for ellipticals are often non-linear, but for ellipticals brighter than M{\_}J {\textless}-23 the following structural relations are found: L propto r{\^{}}0.8 {\$}\backslash{\$}pm 0.1, L propto Sigma{\^{}}-0.5 {\$}\backslash{\$}pm 0.1 and Sigma propto r{\^{}}-1.5 {\$}\backslash{\$}pm 0.1.}, -archivePrefix = {arXiv}, -arxivId = {1303.4710}, -author = {Schombert, J M}, -doi = {10.1017/pas.2013.010}, -eprint = {1303.4710}, -issn = {13233580}, -journal = {Publications of the Astronomical Society of Australia}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: star formation,galaxies: structure}, -number = {1}, -title = {{The structure of galaxies: II. Fitting functions and scaling relations for ellipticals}}, -url = {http://arxiv.org/abs/1303.4710%7B%5C%25%7D0Ahttp://dx.doi.org/10.1017/pas.2013.010}, -volume = {30}, -year = {2013} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M>10^11 M_sun) galaxies at 1.72, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n<2) and spheroid-like (n>2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z$\sim$2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z>2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ($\sim$2x10^10 M_sun kpc^-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J. and Bouwens, Rychard J. and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buitrago et al. - 2008 - Size Evolution of the Most Massive Galaxies at 1.7 z 3 from GOODS NICMOS Survey Imaging.pdf:pdf}, -isbn = {1005-0302}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61--L64}, -title = {{ Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging }}, -url = {http://arxiv.org/abs/0807.4141%0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Bellstedt2018, -abstract = {We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 1010 {\textless} M*/M⊙ {\textless} 1011.6 that cover a large radial range of 0.1-4.0 effective radii.We combine SLUGGS and ATLAS3D data sets to model the total-mass profiles of a sample of 21 fast-rotator galaxies, utilizing a hyperparameter method to combine the two independent data sets. The total-mass density profile slope values derived for these galaxies are consistent with those measured in the inner regions of galaxies by other studies. Furthermore, the total-mass density slopes ($\gamma$tot) appear to be universal over this broad stellar mass range, with an average value of $\gamma$tot= -2.24± 0.05, i.e. slightly steeper than isothermal. We compare our results to model galaxies from the Magneticum and EAGLE cosmological hydrodynamic simulations, in order to probe the mechanisms that are responsible for varying total-mass density profile slopes. The simulated-galaxy slopes are shallower than the observed values by {\$\sim${}}0.3-0.5, indicating that the physical processes shaping the mass distributions of galaxies in cosmological simulations are still incomplete. For galaxies with M* {\textgreater} 1010.7M⊙ in the Magneticum simulations, we identify a significant anticorrelation between total-mass density profile slopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas this anticorrelation is weaker for lower stellar masses, implying that the measured total-mass density slopes for low-mass galaxies are less likely to be determined by merger activity.}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A and Romanowsky, Aaron J and Remus, Rhea Silvia and Stevens, Adam R H and Brodie, Jean P and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to {\$\sim${}}4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}$\backslash${\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashsigma{\$} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and {P{\'{e}}rez Gonz{\'{a}}lez}, Pablo G and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {112}, -title = {{ CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z ∼ 2 }}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -volume = {846}, -year = {2017} -} -@article{Mendez-Abreu2016, -abstract = {We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area data release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log (M∗/MȮ) {\textgreater} 11), the galaxy population is dominated by galaxies modelled with a single S{\'{e}}rsic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T {\textgreater} 0.2. At intermediate masses (9.5 {\textless} log (M∗/MȮ) {\textless} 11), galaxies described with bulge+disc but B/T {\textless} 0.2 are preponderant, whereas, at the low mass end (log (M∗/MȮ) {\textless} 9.5), the prevailing population is constituted by galaxies modelled with either purediscs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57{\%} of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5 {\textless} log (M∗/MȮ) {\textless} 11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62{\%}, 28{\%}, and 10{\%} for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.}, -archivePrefix = {arXiv}, -arxivId = {1610.05324}, -author = {M{\'{e}}ndez-Abreu, J and Ruiz-Lara, T and S{\'{a}}nchez-Menguiano, L and {De Lorenzo-C{\'{a}}ceres}, A and Costantin, L and Catal{\'{a}}n-Torrecilla, C and Florido, E and Aguerri, J A L and Bland-Hawthorn, J and Corsini, E M and Dettmar, R J and Galbany, L and Garc{\'{i}}a-Benito, R and Marino, R A and M{\'{a}}rquez, I and Ortega-Minakata, R A and Papaderos, P and S{\'{a}}nchez, S F and S{\'{a}}nchez-Blazquez, P and Spekkens, K and {Van De Ven}, G and Wild, V and Ziegler, B}, -doi = {10.1051/0004-6361/201629525}, -eprint = {1610.05324}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -title = {{Two-dimensional multi-component photometric decomposition of CALIFA galaxies}}, -url = {http://arxiv.org/abs/1610.05324%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201629525}, -volume = {598}, -year = {2017} -} -@article{Fe, -author = {By, Llustrated}, -keywords = {pee r}, -number = {1987}, -pages = {3--6}, -title = {{P 2 P 2 P 2}}, -volume = {93}, -year = {2009} -} -@article{Lanusse2017a, -abstract = {Galaxy-scale strong gravitational lensing can not only provide a valuable probe of the dark matter distribution of massive galaxies, but also provide valuable cosmological constraints, either by studying the population of strong lenses or by measuring time delays in lensed quasars. Due to the rarity of galaxy-scale strongly lensed systems, fast and reliable automated lens finding methods will be essential in the era of large surveys such as Large Synoptic Survey Telescope, Euclid and Wide-Field Infrared Survey Telescope. To tackle this challenge, we introduce CMU DeepLens, a new fully automated galaxy-galaxy lens finding method based on deep learning. This supervised machine learning approach does not require any tuning after the training step which only requires realistic image simulations of strongly lensed systems. We train and validate our model on a set of 20 000 LSST-like mock observations including a range of lensed systems of various sizes and signal-to-noise ratios (S/N).We find on our simulated data set that for a rejection rate of non-lenses of 99 per cent, a completeness of 90 per cent can be achieved for lenses with Einstein radii larger than 1.4 arcsec and S/N larger than 20 on individual g-band LSST exposures. Finally, we emphasize the importance of realistically complex simulations for training such machine learning methods by demonstrating that the performance of models of significantly different complexities cannot be distinguished on simpler simulations.}, -archivePrefix = {arXiv}, -arxivId = {1703.02642}, -author = {Lanusse, Fran{\c{c}}ois and Ma, Quanbin and Li, Nan and Collett, Thomas E and Li, Chun Liang and Ravanbakhsh, Siamak and Mandelbaum, Rachel and P{\'{o}}czos, Barnab{\'{a}}s}, -doi = {10.1093/mnras/stx1665}, -eprint = {1703.02642}, -isbn = {0021-9258 (Print)$\backslash$r0021-9258 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: statistical,gravitational lensing: strong}, -number = {3}, -pages = {3895--3906}, -pmid = {10913147}, -title = {{CMU DeepLens: Deep learning for automatic image-based galaxy-galaxy strong lens finding}}, -url = {http://arxiv.org/abs/1703.02642}, -volume = {473}, -year = {2018} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M{\_}*/M{\_}sun) {\textgreater} 11.5 (M{\_}K {\textless} -25.3 mag) and distance D {\textless} 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38$\backslash$pm6{\%} down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80$\backslash$pm10{\%} and 28$\backslash$pm6{\%}, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R{\_}e), and the gas morphologies are diverse, with 17/28 = 61$\backslash$pm9{\%} being centrally concentrated, 8/28 = 29$\backslash$pm9{\%} exhibiting clear rotation out to several kpc, and 3/28 = 11$\backslash$pm6{\%} being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly {\$\sim${}}10{\^{}}5M{\_}sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A and Blakeslee, John P and Goulding, Andy D and McConnell, Nicholas J and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58 arcsec in the i band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including an {\$\sim${}}10 per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally,we check the sensitivity of our shear calibration estimates to other cutsmade on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalogue are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{Bower:2016aa, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of $\sim$1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G. and Schaye, Joop and Frenk, Carlos S. and Theuns, Tom and Schaller, Matthieu and Crain, Robert A. and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an en(4).pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an en(5).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -month = {jul}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{2001es, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Nightingale2021, -author = {Nightingale, James. and Hayes, Richard and Kelly, Ashley and Amvrosiadis, Aristeidis and Etherington, Amy and He, Qiuhan and Li, Nan and Cao, XiaoYue and Frawley, Jonathan and Cole, Shaun and Enia, Andrea and Frenk, Carlos and Harvey, David and Li, Ran and Massey, Richard and Negrello, Mattia and Robertson, Andrew}, -doi = {10.21105/joss.02825}, -file = {:C\:/Users/Jammy/Documents/Papers/Software/PyAutoLens.pdf:pdf}, -issn = {2475-9066}, -journal = {J. Open Source Softw.}, -number = {58}, -pages = {2825}, -title = {{PyAutoLens: Open-Source Strong Gravitational Lensing}}, -volume = {6}, -year = {2021} -} -@article{Swinbank2013, -abstract = {We present a study of the radio properties of 870 $\mu$m-selected submillimetre galaxies (SMGs), observed at high resolution with Atacama Large Millimeter Array (ALMA) in the Extended Chandra Deep Field South. From our initial sample of 76 ALMA SMGs, we detect 52 SMGs at >3$\sigma$ significance in Karl G. Jansky Very Large Array 1400 MHz imaging, of which 35 are also detected at >3$\sigma$ in new 610 MHz Giant Metre-Wave Radio Telescope imaging. Within this sample of radio-detected SMGs, we measure a median radio spectral index $\alpha$6101400 = -0.79 ± 0.06, (with inter-quartile range $\alpha$ = [-1.16, -0.56]) and investigate the far-infrared/radio correlation via the parameter qIR, the logarithmic ratio of the rest-frame 8-1000 $\mu$m flux and monochromatic radio flux. Our median qIR = 2.56 ± 0.05 (inter-quartile range qIR = [2.42, 2.78]) is higher than that typically seen in single-dish 870 $\mu$m-selected sources (qIR $\sim$ 2.4), which may reflect the fact that our ALMA-based study is not biased to radio-bright counterparts, as previous samples were. Finally, we search for evidence that qIR and $\alpha$ evolve with age in a codependent manner, as predicted by starburst models: the data populate the predicted region of parameter space, with the stellar mass tending to increase along tracks of qIR versus a in the direction expected, providing the first observational evidence in support of these models.}, -archivePrefix = {arXiv}, -arxivId = {1404.7128}, -author = {Thomson, A. P. and Ivison, R. J. and Simpson, J. M. and Swinbank, A. M. and Smail, Ian and Arumugam, V. and Alexander, D. M. and Beelen, A. and Brandt, W. N. and Chandra, I. and Dannerbauer, H. and Greve, T. R. and Hodge, J. A. and Ibar, E. and Karim, A. and Murphy, E. J. and Schinnerer, E. and Sirothia, S. and Walter, F. and Wardlow, J. L. and van der Werf, P.}, -doi = {10.1093/mnras/stu839}, -eprint = {1404.7128}, -isbn = {00358711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: starburst}, -number = {1}, -pages = {577--588}, -pmid = {26630356}, -title = {{An ALMA survey of submillimetre galaxies in the Extended Chandra Deep Field South: Radio properties and the far-infrared/radio correlation}}, -volume = {442}, -year = {2014} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ($z = 1.489$), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5$+$2223 ($z = 0.542$), published by Grillo et al. (2016), and explore different $\Lambda$CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of $H_{0}$ and $\Omega_{\rm m}$ with relative (1$\sigma$) statistical errors of, respectively, 6% (7%) and 31% (26%) in flat (general) cosmological models, assuming a conservative 3% uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of $H_{0}$, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C. and Rosati, P. and Suyu, S. H. and Balestra, I. and Caminha, G. B. and Halkola, A. and Kelly, P. L. and Lombardi, M. and Mercurio, A. and Rodney, S. A. and Treu, T.}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Grillo et al. - 2018 - Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -number = {2}, -pages = {94}, -title = {{Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”}}, -url = {http://arxiv.org/abs/1802.01584}, -volume = {860}, -year = {2018} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/de Vaucouleurs - 2005 - Author Index.pdf:pdf}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287--a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{Mcconnell2013, -abstract = {New kinematic data and modeling efforts in the past few years have substantially expanded and revised dynamical measurements of black hole masses (M •) at the centers of nearby galaxies. Here we compile an updated sample of 72 black holes and their host galaxies, and present revised scaling relations between M • and stellar velocity dispersion ($\sigma$), V-band luminosity (L), and bulge stellar mass (M bulge), for different galaxy subsamples. Our best-fitting power-law relations for the full galaxy sample are log10(M •) = 8.32 + 5.64log10($\sigma$/200 km s-1), log10(M •) = 9.23 + 1.11log10(L/1011 L ⊙), and log10(M •) = 8.46 + 1.05log10(M bulge/1011 M ⊙). A log-quadratic fit to the M •-$\sigma$ relation with an additional term of $\beta$2 [log10($\sigma$/200 km s -1)]2 gives $\beta$2 = 1.68 ± 1.82 and does not decrease the intrinsic scatter in M •. Including 92 additional upper limits on M • does not change the slope of the M •-$\sigma$ relation. When the early- and late-type galaxies are fit separately, we obtain similar slopes of 5.20 and 5.06 for the M •-$\sigma$ relation but significantly different intercepts - M • in early-type galaxies are about two times higher than in late types at a given sigma. Within early-type galaxies, our fits to M •($\sigma$) give M • that is about two times higher in galaxies with central core profiles than those with central power-law profiles. Our M •-L and M •-M bulge relations for early-type galaxies are similar to those from earlier compilations, and core and power-law galaxies yield similar L- and M bulge-based predictions for M •. When the conventional quadrature method is used to determine the intrinsic scatter in M •, our data set shows weak evidence for increased scatter at M bulge < 1011 M ⊙ or LV < 1010.3 L⊙, while the scatter stays constant for 1011 < M bulge < 1012.3 M ⊙ and 1010.3 < LV < 10 11.5 L⊙. A Bayesian analysis indicates that a larger sample of M • measurements would be needed to detect any statistically significant trend in the scatter with galaxy properties. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1211.2816}, -author = {McConnell, Nicholas J. and Ma, Chung Pei}, -doi = {10.1088/0004-637X/764/2/184}, -eprint = {1211.2816}, -isbn = {0004-637X}, -issn = {15384357}, -journal = {ApJ}, -keywords = {galaxies: nuclei,galaxies: statistics}, -month = {feb}, -number = {2}, -pages = {184}, -title = {{Revisiting the scaling relations of black hole masses and host galaxy properties}}, -url = {http://stacks.iop.org/0004-637X/764/i=2/a=184?key=crossref.d80a3579de9be22fa41e43d743902a27}, -volume = {764}, -year = {2013} -} -@article{Schombert2015a, -abstract = {Using isophotal radius correlations for a sample of Two Micron All Sky Survey ellipticals, we have constructed a series of template surface brightness profiles to describe the profile shapes of ellipticals as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that ellipticals are weakly nonhomologous with respect to structure. Through comparison to the templates, it is discovered that ellipticals are divided into two families: those well matched to the templates, and a second class of ellipticals with distinctly shallower profile slopes. We refer to this second type of ellipticals as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D ellipticals cover the same range of luminosity, size, and kinematics as normal ellipticals, but maintain a signature of recent equal-mass dry mergers. We propose that normal ellipticals grow after an initial dissipation formation era by accretion of low-mass companions as outlined in hierarchical formation scenarios, while D ellipticals are the result of later equal-mass mergers producing shallow luminosity profiles.}, -archivePrefix = {arXiv}, -arxivId = {1509.08381}, -author = {Schombert, James M.}, -doi = {10.1088/0004-6256/150/5/162}, -eprint = {1509.08381}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Schombert - 2015 - The structure of galaxies. III. Two structural families of ellipticals.pdf:pdf}, -isbn = {doi:10.1088/0004-6256/150/5/162}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: photometry,galaxies: structure}, -number = {5}, -pages = {162}, -publisher = {IOP Publishing}, -title = {{The structure of galaxies. III. Two structural families of ellipticals}}, -url = {http://dx.doi.org/10.1088/0004-6256/150/5/162}, -volume = {150}, -year = {2015} -} -@article{Ellis2010, -abstract = {I review the development of gravitational lensing as a powerful tool of the observational cosmologist. After the historic eclipse expedition organized by Arthur Eddington and Frank Dyson, the subject lay observationally dormant for 60 years. However, subsequent progress has been astonishingly rapid, especially in the past decade, so that gravitational lensing now holds the key to unravelling the two most profound mysteries of our Universe - the nature and distribution of dark matter, and the origin of the puzzling cosmic acceleration first identified in the late 1990s. In this non-specialist review, I focus on the unusual history and achievements of gravitational lensing and its future observational prospects. {\textcopyright} 2010 The Royal Society.}, -author = {Ellis, Richard S.}, -doi = {10.1098/rsta.2009.0209}, -issn = {1364503X}, -journal = {Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences}, -keywords = {Galaxy evolution,Gravitational lensing,Large-scale structure,Observational cosmology}, -month = {feb}, -number = {1914}, -pages = {967--987}, -pmid = {20123743}, -title = {{Gravitational lensing: A unique probe of dark matter and dark energy}}, -url = {http://rsta.royalsocietypublishing.org/cgi/doi/10.1098/rsta.2009.0209}, -volume = {368}, -year = {2010} -} -@article{Moore2018, -archivePrefix = {arXiv}, -arxivId = {arXiv:1401.7988v1}, -author = {Moore, M and Wang, Lianqi and Ellerbroek, Brent}, -eprint = {arXiv:1401.7988v1}, -pages = {1--19}, -title = {{Prospects for measuring supermassive black hole masses with future extremely large telescopes}}, -year = {2018} -} -@article{Spingola2018, -abstract = {We present milliarcsecond (mas) angular resolution observations of the gravitationally lensed radio source MG J0751+2716 (at z= 3.2) obtained with global very long baseline interferometry (VLBI) at 1.65 GHz. The background object is highly resolved in the tangential and radial directions, showing evidence of both compact and extended structure across several gravitational arcs that are 200-600 mas in size. By identifying compact sub-components in the multiple images, we constrain the mass distribution of the foreground z = 0.35 gravitational lens using analytic models for the main deflector [power-law elliptical mass model; $\rho$(r)∞ r-$\gamma$, where $\gamma$ = 2 corresponds to isothermal] and for the members of the galaxy group. Moreover, our mass models with and without the group find an inner mass-density slope steeper than isothermal for the main lensing galaxy, with $\gamma$1 = 2.08 ± 0.02 and $\gamma$2 = 2.16 ± 0.02 at the 4.2$\sigma$ level and 6.8$\sigma$ level, respectively, at the Einstein radius (b1 = 0.4025 ± 0.0008 and b2 = 0.307 ± 0.002 arcsec, respectively). We find randomly distributed image position residuals of about 3 mas, which are much larger that the measurement errors (40 $\mu$as on average). This suggests that at the mas level, the assumption of a smooth mass distribution fails, requiring additional structure in the model. However, given the environment of the lensing galaxy, it is not clear whether this extra mass is in the form of sub-haloes within the lens or along the line of sight, or from a more complex halo for the galaxy group.}, -archivePrefix = {arXiv}, -arxivId = {1807.05566}, -author = {Spingola, C. and McKean, J. P. and Auger, M. W. and Fassnacht, C. D. and Koopmans, L. V.E. and Lagattuta, D. J. and Vegetti, S.}, -doi = {10.1093/mnras/sty1326}, -eprint = {1807.05566}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Spingola et al. - 2018 - SHARP - V. Modelling gravitationally lensed radio arcs imaged with global VLBI observations.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: active,Gravitational lensing: strong,Radio continuum: galaxies,Techniques: interferometric}, -number = {4}, -pages = {4816--4829}, -title = {{SHARP - V. Modelling gravitationally lensed radio arcs imaged with global VLBI observations}}, -url = {http://arxiv.org/abs/1807.05566%0Ahttp://dx.doi.org/10.1093/mnras/sty1326}, -volume = {478}, -year = {2018} -} -@article{Cohen2018, -abstract = {We present HST/ACS imaging of twenty-three very low surface brightness ({\$}\backslashmu{\_}{\{}e,V{\}}{\$}=25-27.5) galaxies detected in the fields of four nearby galaxy groups. These objects were selected from deep optical imaging obtained with the Dragonfly Telephoto Array. Seven are new discoveries, while most of the others had been identified previously in visual surveys of deep photographic plates and more recent surveys. Few have previously been studied in detail. From the ACS images, we measure distances to the galaxies using both the tip of the red giant branch method and the surface brightness fluctuations method. We demonstrate that the two methods are consistent with each other in the regime where both can be applied. The distances to 15 out of 20 galaxies with stable measurements are consistent with that of the targeted group within errors. This suggests that assuming group membership based solely on projected proximity is {\$\sim${}}75{\%} successful in this regime. The galaxies are nearly round, with a median axis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The objects have a range of sizes, from {\$}R{\_}e{\$}=0.4 kpc to {\$}R{\_}e{\$}=1.8 kpc, with a median of 1.0 kpc. They range in luminosity from {\$}M{\_}V{\$}=-11.4 to {\$}M{\_}V{\$}=-15.6, with a median of -12.4. Galaxies with {\$}R{\_}e{\$}{\$\sim${}}1 kpc and {\$}M{\_}V{\$}{\$\sim${}}-12 are fairly rare in the Local Group but we find many of them in this relatively small sample. Four of the objects fall in the class of ultra diffuse galaxies (UDGs), with {\$}R{\_}e{\$}{\textgreater}1.5 kpc and {\$}\backslashmu{\_}{\{}0,V{\}}{\$}{\textgreater}24 mag/arcsec{\^{}}2, including the recently identified dark matter deficient galaxy NGC1052-DF2.}, -archivePrefix = {arXiv}, -arxivId = {1807.06016}, -author = {Cohen, Yotam and van Dokkum, Pieter and Danieli, Shany and Romanowsky, Aaron J and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Mowla, Lamiya and Kruijssen, J M Diederik and Conroy, Charlie and Wasserman, Asher}, -doi = {10.3847/1538-4357/aae7c8}, -eprint = {1807.06016}, -issn = {1538-4357}, -journal = {eprint arXiv:1807.06016}, -keywords = {Astrophysics,Astrophysics of Galaxies}, -title = {{The Dragonfly Nearby Galaxies Survey. V. HST/ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC1052, NGC1084, M96, and NGC4258}}, -url = {http://arxiv.org/abs/1807.06016%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aae7c8}, -year = {2018} -} -@article{Ferrero2017, -abstract = {The Tully-Fisher relation (TFR) links the stellar mass of a disk galaxy, {\$}M{\_}{\{}\backslashrm str{\}}{\$}, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling ({\$}M\backslashpropto V{\^{}}3{\$}) of dark matter halos, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to be non-monotonic and rapidy evolving. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of {\$}\backslashLambda{\$}CDM cosmological simulations. Matching both relations requires disk sizes to satisfy constraints given by the concentration of halos and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to {\$}z=1{\$}. {\$}\backslashLambda{\$}CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1607.03100}, -author = {Ferrero, Ismael and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw2691}, -eprint = {1607.03100}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {4}, -pages = {4736--4746}, -title = {{Size matters: Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE}}, -volume = {464}, -year = {2017} -} -@article{Ding2018a, -abstract = {Strong gravitational lenses with measured time delay are a powerful tool to measure cosmological parameters, especially the Hubble constant ({\$}H{\_}0{\$}). Recent studies show by combining just three multiply-imaged AGN systems, one can determine {\$}H{\_}0{\$} to 3.8{\%} precision. Furthermore, the number of time-delay lens is growing rapidly, enabling the determination of {\$}H{\_}0{\$} to 1{\%} precision in the near future. However, it is important to ensure that systematic errors and biases remain subdominant. For this purpose, challenges with simulated datasets are a key component. Following the experience of the past challenge on time delay, where it was shown that time delays can be measured precisely and accurately at the sub-percent level, we now present the "Time Delay Lens Modeling Challenge" (TDLMC). The goal of TDLMC is to assess the present capabilities of lens modeling codes and assumptions and test the level of accuracy of inferred cosmological parameters given realistic mock datasets. We invite scientists to model a set of simulated HST observations of 50 mock lens systems. The systems are organized in rungs, with the complexity and realism increasing going up the ladder. The goal of the challenge is to infer {\$}H{\_}0{\$} for each rung, given the HST images, the time delay, and a stellar velocity dispersion of the deflector, for a fixed background cosmology. The TDLMC challenge will start with the mock data release on 2018 January 8th. The deadline for blind submission is different for each rung. The deadline for Rung0-1 is 2018 September 8; the deadline for Rung2 is 2019 January 8 and the one for Rung3 is 2019 May 8. This first paper gives an overview of the challenge including the data design, and a set of metrics to quantify the modeling performance and challenge details. After the deadline, the results of the challenge will be presented in a companion paper with all challenge participants as co-authors.}, -archivePrefix = {arXiv}, -arxivId = {1801.01506}, -author = {Ding, Xuheng and Treu, Tommaso and Shajib, Anowar J and Xu, Dandan and Chen, Geoff C -F. and More, Anupreeta and Despali, Giulia and Frigo, Matteo and Fassnacht, Christopher D and Gilman, Daniel and Hilbert, Stefan and Marshall, Philip J and Sluse, Dominique and Vegetti, Simona}, -eprint = {1801.01506}, -title = {{Time Delay Lens Modeling Challenge: I. Experimental Design}}, -url = {http://arxiv.org/abs/1801.01506}, -year = {2018} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1016/s0020-7063(13)00118-0}, -isbn = {3018804090}, -issn = {00207063}, -journal = {The International Journal of Accounting}, -number = {4}, -pages = {559--561}, -title = {{Author Index}}, -url = {https://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {48}, -year = {2013} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter (CDM) galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes possess a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a $\Lambda$CDM universe. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R and Eke, Vincent R and Frenk, Carlos S and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{Mendez-Abreu2010, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Graham2001a, -abstract = {From a diameter-limited sample of 86 `face-on' spiral galaxies, the bulge-to-disk size and luminosity ratios, and other quantitative measurements for the prominence of the bulge are derived. The bulge and disk parameters have been estimated using a seeing convolved Sersic r^(1/n) bulge and a seeing convolved exponential disk. In general, early-type spiral galaxy bulges have Sersic values of n>1, and late-type spiral galaxy bulges have values of n<1. In the B-band, only 8 galaxies have a bulge shape parameter n consistent with the exponential value of 1, and only 5 galaxies do in the K-band. Application of the r^(1/n) bulge models results in a larger mean r_e/h ratio for the early-type spiral galaxies than the late-type spiral galaxies. Although, this result is shown not to be statistically significant. The mean B/D luminosity ratio is, however, significantly larger (> 3-sigma) for the early-type spirals than the late-type spirals. This apparent contradiction with the r_e/h values can be explained with an iceberg-like scenario, in which the bulges in late-type spiral galaxies are relatively submerged in their disk. This can be achieved by varying the relative bulge/disk stellar density while maintaining the same effective bulge-to-disk size ratio. The absolute bulge magnitude - log(n) diagram is used as a diagnostic tool for comparative studies with dwarf elliptical and ordinary elliptical galaxies. At least in the B-band, these objects occupy distinctly different regions of this parameter space. While the dwarf ellipticals appear to be the faint extension to the brighter elliptical galaxies, the bulges of spiral galaxies are not.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0011256}, -author = {Graham, Alister W.}, -doi = {10.1086/318767}, -eprint = {0011256}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Graham - 2001 - An Investigation into the Prominence of Spiral Galaxy Bulges(2).pdf:pdf}, -issn = {00046256}, -journal = {AJ}, -keywords = {Galaxies: Dwarf,Galaxies: Formation,Galaxies: Fundamental Parameters,Galaxies: Photometry,Galaxies: Spiral,Galaxies: Structure}, -number = {2}, -pages = {820--840}, -primaryClass = {astro-ph}, -title = {{An Investigation into the Prominence of Spiral Galaxy Bulges}}, -url = {http://arxiv.org/abs/astro-ph/0011256%0Ahttp://dx.doi.org/10.1086/318767}, -volume = {121}, -year = {2001} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}1011 to {\textgreater} 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Buitrago2017a, -abstract = {Using the exquisite depth of the Hubble Ultra Deep Field (HUDF12 programme) data set, we explore the ongoing assembly of the outermost regions of the most massive galaxies (Mstellar ≥ 5× 1010 M) at z ≤ 1. The outskirts of massive objects, particularly early-type Galaxies (ETGs), are expected to suffer a dramatic transformation across cosmic time due to continuous accretion of small galaxies. HUDF imaging allows us to study this process at intermediate redshifts in six massive galaxies, exploring the individual surface brightness profiles out to ∼25 effective radii. We find that 5–20 per cent of the total stellar mass for the galaxies in our sample is contained within 10 {\textless} R {\textless} 50 kpc. These values are in close agreement with numerical simulations, and higher than those reported for local late-type galaxies (5 per cent). The fraction of stellar mass stored in the outer envelopes/haloes of massive ETGs increases with decreasing redshift, being 28.7 per cent at {\textless}z {\textgreater}= 0.1, 15.1 per cent at {\textless}z {\textgreater}= 0.65 and 3.5 per cent at {\textless}z {\textgreater}= 2. The fraction of mass in diffuse features linked with ongoing minor merger events is {\textgreater}1–2 per cent, very similar to predictions based on observed close pair counts. Therefore, the results for our small albeit meaningful sample suggest that the size and mass growth of the most massive galaxies have been solely driven by minor and major merging from z = 1 to today.}, -archivePrefix = {arXiv}, -arxivId = {1602.01846}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Curtis-Lake, Emma and Montes, Mireia and Cooper, Andrew P and Bruce, Victoria A and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Cirasuolo, Michele}, -doi = {10.1093/mnras/stw3382}, -eprint = {1602.01846}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: haloes,Galaxies: high-redshift,Galaxies: structure,cD}, -number = {4}, -pages = {4888--4903}, -title = {{The cosmic assembly of stellar haloes in massive early-type Galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3382}, -volume = {466}, -year = {2017} -} -@article{Pieri2011, -abstract = {We study the prospects for detecting the annihilation products of dark matter (DM) in the framework of the two highest-resolution numerical simulations currently available, i.e., Via Lactea II and Aquarius. We propose a strategy to determine the shape and size of the region around the Galactic center that maximizes the probability of observing a DM signal, and we show that, although the predicted flux can differ by a factor of 10 for a given DM candidate in the two simulation setups, the search strategy remains actually unchanged, since it relies on the angular profile of the annihilation flux, not on its normalization. We present mock $\gamma$-ray maps that keep into account the diffuse emissions produced by unresolved halos in the Galaxy, and we show that, in an optimistic DM scenario, a few individual clumps can be resolved above the background with the Fermi-LAT. Finally, we calculate the energy-dependent boost factors for positrons and antiprotons and show that they are always of O(1), and, therefore, they cannot lead to the large enhancements of the antimatter fluxes required to explain the recent PAMELA, ATIC, Fermi, and HESS data. Still, we show that the annihilation of 100 GeV weakly interacting massive particles into charged lepton pairs may contribute significantly to the positron budget. {\textcopyright} 2011 The American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {0908.0195}, -author = {Pieri, Lidia and Lavalle, Julien and Bertone, Gianfranco and Branchini, Enzo}, -doi = {10.1103/PhysRevD.83.023518}, -eprint = {0908.0195}, -issn = {15507998}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -number = {2}, -title = {{Implications of high-resolution simulations on indirect dark matter searches}}, -volume = {83}, -year = {2011} -} -@article{Kitching2019, -abstract = {In this paper we derive a full expression for the propagation of multiplicative and additive shape measurement biases into the cosmic shear power spectrum. In doing so we identify several new terms that are associated with selection effects, as well as cross-correlation terms between the multiplicative and additive biases and the shear field. The computation of the resulting bias in the shear power spectrum scales as the fifth power of the maximum multipole considered. Consequently the calculation is unfeasible for large l-modes, and the only tractable way to assess the full impact of shape measurement biases on cosmic shear power spectrum is through forward modelling of the effects. To linear order in bias parameters the shear power spectrum is only affected by the mean of the multiplicative bias field over a survey and the cross correlation between the additive bias field and the shear field. If the mean multiplicative bias is zero then second order convolutive terms are expected to be orders of magnitude smaller.}, -archivePrefix = {arXiv}, -arxivId = {1904.07173}, -author = {Kitching, Thomas D. and Paykari, Paniez and Hoekstra, Henk and Cropper, Mark}, -doi = {10.21105/astro.1904.07173}, -eprint = {1904.07173}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kitching et al. - 2019 - Propagating Residual Biases in Cosmic Shear Power Spectra.pdf:pdf}, -journal = {The Open Journal of Astrophysics}, -number = {1}, -pages = {14}, -title = {{Propagating Residual Biases in Cosmic Shear Power Spectra}}, -volume = {3}, -year = {2019} -} -@article{Witt1997, -abstract = {We study a general elliptical potential of the form $\psi$ (x2 + y2/q2) (0 < q ≤ 1) plus a shear (with an arbitrary direction) as models for the observed quadruple lenses. It is shown that a minimum additional shear is needed even to simply reproduce the observed galaxy and image positions. We also obtain the dependence of the axial ratio, q, on the orientation of the major axis of potential. A relation also exists between the shear, the position angle and the axial ratio of the lensing galaxy. The relation reveals a degeneracy in modelling quadruple lenses when only the image positions are used. More specifically, only the ratio of the ellipticity, ∈ ≡ (1 - q2)/ (1 + q2), to the magnitude of shear, $\gamma$, can be determined. All these results are valid regardless of the radial profile of the elliptical potential. Our formalism applies when the galaxy position is observed, which is the case for seven of the eight known quadruple lenses. Application to these seven cases reveals two quadruple lenses, CLASS 1608 + 656 and HST 12531-2914, requiring highly significant shear with magnitude ≈0.2. For HST 12531-2914, there is likely a misalignment between the major axis of light and the major axis of potential (mass). Monte Carlo simulations show that our results, although derived for elliptical potentials, apply equally well to elliptical density distributions. We conclude that detailed modelling of quadruple lenses can yield valuable quantitative information about the shape of lensing galaxies and their dark matter haloes. {\textcopyright} 1997 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9702021}, -author = {Witt, Hans J. and Mao, Shude}, -doi = {10.1093/mnras/291.1.211}, -eprint = {9702021}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Witt1997Shear.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: Structure,Gravitational lensing,Quasars: Individual: CLASS 1608 + 656,Quasars: Individual: HST 12531-2914}, -number = {1}, -pages = {211--218}, -primaryClass = {astro-ph}, -title = {{Probing the structure of lensing galaxies with quadruple lenses: The effect of 'external' shear}}, -volume = {291}, -year = {1997} -} -@article{Trujillo2007a, -abstract = {Using the combined capabilities of the large near-infrared Palomar/DEEP-2 survey, and the superb resolution of the Advanced Camera for Surveys HST camera, we explore the size evolution of 831 very massive galaxies (M Black star ≥ 1011h-270 M ⊙) since z ∼ 2. We split our sample according to their light concentration using the S{\'{e}}rsic index n. At a given stellar mass, both low (n < 2.5) and high (n > 2.5) concentrated objects were much smaller in the past than their local massive counterparts. This evolution is particularly strong for the highly concentrated (spheroid like) objects. At z ∼ 1.5, massive spheroid-like objects were a factor of 4 (±0.4) smaller (i.e. almost two orders of magnitudes denser) than those we see today. These small sized, high-mass galaxies do not exist in the nearby Universe, suggesting that this population merged with other galaxies over several billion years to form the largest galaxies we see today. {\textcopyright} 2007 The Authors.}, -archivePrefix = {arXiv}, -arxivId = {0709.0621}, -author = {Trujillo, Ignacio and Conselice, C. J. and Bundy, Kevin and Cooper, M. C. and Eisenhardt, P. and Ellis, Richard S.}, -doi = {10.1111/j.1365-2966.2007.12388.x}, -eprint = {0709.0621}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Trujillo et al. - 2007 - Strong size evolution of the most massive galaxies since z ∼ 2.pdf:pdf}, -isbn = {0046-8177 (Print)\r0046-8177 (Linking)}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: high-redshift,Galaxies: structure,cD}, -number = {1}, -pages = {109--120}, -pmid = {3679185}, -title = {{Strong size evolution of the most massive galaxies since z ∼ 2}}, -volume = {382}, -year = {2007} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 < z < 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* > 1011M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J125, i814, v606 HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V. A. and Dunlop, J. S. and McLure, R. J. and Cirasuolo, M. and Buitrago, F. and Bowler, R. A.A. and Targett, T. A. and Bell, E. F. and McIntosh, D. H. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Hartley, W. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and McGrath, E. J.}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 < z < 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.1736}, -volume = {444}, -year = {2014} -} -@article{Springel2006a, -abstract = {Galaxies are not uniformly distributed in space. On large scales, the Universe displays coherent structure, with galaxies residing in groups and clusters on scales of ∼ 1–3 h− 1 Mpc, which lie at the intersections of long filaments of galaxies that are {\textless} 10 h− 1 Mpc�in length. Vast regions of relatively empty space, known as voids, contain very few galaxies and span the volume in between these structures. This observed large-scale structure depends both on cosmological parameters and on the formation and evolution of galaxies. Using the two-point correlation function, one can trace the dependence of large-scale structure on galaxy properties, such as luminosity, color, stellar mass, and track its evolution with redshift. Comparison of the observed galaxy clustering signatures with dark matter simulations allows one to model and understand the clustering of galaxies and their formation and evolution within their parent dark matter halos. Clustering measurements can determine the parent dark matter halo mass of a given galaxy population, connect observed galaxy populations at different epochs, and constrain cosmological parameters and galaxy evolution models. This chapter describes the methods used to measure the two-point correlation function in both redshift and real space, presents the current results of how the clustering amplitude depends on various galaxy properties, and discusses quantitative measurements of the structures of voids and filaments. The interpretation of these results with current theoretical models is also presented.}, -archivePrefix = {arXiv}, -arxivId = {1202.6633}, -author = {Coil, Alison L}, -doi = {10.1007/978-94-007-5609-0_8}, -eprint = {1202.6633}, -isbn = {9789400756090}, -issn = {0038-6308}, -journal = {Planets, Stars and Stellar Systems: Volume 6: Extragalactic Astronomy and Cosmology}, -number = {7088}, -pages = {387--421}, -pmid = {16641985}, -title = {{The large-scale structure of the universe}}, -url = {http://arxiv.org/abs/astro-ph/0604561%7B%5C%25%7D0Ahttp://dx.doi.org/10.1038/nature04805}, -volume = {440}, -year = {2013} -} -@article{Christensen2014, -abstract = {We present a detailed comparison between the photometric properties of the bulges of two simulated galaxies and those of a uniform sample of observed galaxies. This analysis shows that the simulated galaxies have bulges with realistic surface brightnesses for their sizes and magnitude. These two field disc galaxies have rotational velocities ̃100 km s-1 and were integrated to a redshift of zero in a fully cosmological $\delta$ cold dark matter context as part of high-resolution smoothed particle hydrodynamic simulations. We performed bulge- disc decompositions of the galaxies using artificial observations, in order to conduct a fair comparison to observations. We also dynamically decomposed the galaxies and compared the star formation histories of the bulges to those of the entire galaxies. These star formation histories showed that the bulges were primarily formed before z = 1 and during periods of rapid star formation. Both galaxies have large amounts of early star formation, which is likely related to the relatively high bulge-to-disc ratios also measured for them. Unlike almost all previous cosmological simulations, the realistically concentrated bulges of these galaxies do not lead to unphysically high rotational velocities, causing them to naturally lie along the observed Tully-Fisher relation. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1402.2702}, -author = {Christensen, C. R. and Brooks, A. M. and Fisher, D. B. and Governato, F. and McCleary, J. and Quinn, T. R. and Shen, S. and Wadsley, J.}, -doi = {10.1093/mnrasl/slu020}, -eprint = {1402.2702}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Christensen et al. - 2014 - Simulating disc galaxy bulges that are consistent with observed scaling relations.pdf:pdf}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Bulges,Formation,Galaxies,Methods,Numerical,Spiral,Structure}, -number = {1}, -pages = {1--6}, -title = {{Simulating disc galaxy bulges that are consistent with observed scaling relations}}, -volume = {440}, -year = {2014} -} -@article{Dutton2012, -abstract = {Recentwork has suggested that the stellar initial mass function (IMF) is not universal, but rather is correlated with galaxy stellar mass, stellar velocity dispersion or morphological type. In this paper, we investigate variations of the IMF within individual galaxies. For this purpose, we use strong lensing and gas kinematics to measure independently the normalization of the IMF of the bulge and disc components of a sample of five massive spiral galaxies with substantial bulge components taken from the Sloan WFC Edge-on Late-type Lens Survey (SWELLS). We find that the stellar masses of the bulges are tightly constrained by the lensing and kinematic data. A comparison with masses based on stellar population synthesis models fitted to optical and near-infrared photometry favours a Salpeter-like normalization of the IMF. Conversely, the disc masses are less well constrained due to degeneracies with the dark matter halo, but are consistent with Milky Way-type IMFs in agreement with previous studies. The discs are submaximal at 2.2 disc scale lengths, but due to the contribution of the bulges, the galaxies are baryon dominated at 2.2 disc scale lengths. Globally, our inferred IMF normalization is consistent with that found for early-type galaxies of comparable stellar mass (>1011M⊙). Our results suggest a non-universal IMF within the different components of spiral galaxies, adding to the well-known differences in stellar populations between discs and bulges. {\textcopyright} 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1206.4310}, -author = {Dutton, Aaron A. and Treu, Tommaso and Brewer, Brendon J. and Marshall, Philip J. and Auger, M. W. and Barnab{\'{e}}, Matteo and Koo, David C. and Bolton, Adam S. and Koopmans, Leon V.E.}, -doi = {10.1093/mnras/sts262}, -eprint = {1206.4310}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: bulges,Galaxies: kinematics and dynamics,Galaxies: spiral,Stars: luminosity function, mass function}, -month = {feb}, -number = {4}, -pages = {3183--3195}, -title = {{The SWELLS survey - V. A salpeter stellar initial mass function in the bulges of massive spiral galaxies}}, -volume = {428}, -year = {2013} -} -@article{Cautun2015a, -abstract = {We investigate the angular and kinematic distributions of satellite galaxies around a large sample of bright isolated primaries in the spectroscopic and photometric catalogues of the Sloan Digital Sky Survey (SDSS). We detect significant anisotropy in the spatial distribution of satellites. To test whether this anisotropy could be related to the rotating disks of satellites recently found by Ibata et al. in a sample of SDSS galaxies, we repeat and extend their analysis. Ibata et al. found an excess of satellites on opposite sides of their primaries having anticorrelated radial velocities. We find that this excess is sensitive to small changes in the sample selection criteria which can greatly reduce its significance. In addition, we find no evidence for correspondingly correlated velocities for satellites observed on the same side of their primaries, which would be expected for rotating disks of satellites. We conclude that the detection of coherent rotation in the satellite population in current observational samples is not robust. We compare our data to the {\$}\backslashLambda{\$}CDM Millennium simulations populated with galaxies according to the semi-analytic model of Guo et al. We find excellent agreement with the spatial distribution of satellites in the SDSS data and the lack of a strong signal from coherent rotation.}, -archivePrefix = {arXiv}, -arxivId = {1410.7778}, -author = {Cautun, Marius and Wang, Wenting and Frenk, Carlos S and Sawala, Till}, -doi = {10.1093/mnras/stv490}, -eprint = {1410.7778}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {3}, -pages = {2576--2587}, -title = {{A new spin on discs of satellite galaxies}}, -volume = {449}, -year = {2015} -} -@article{Cirasuolo2003, -abstract = {We present a new approach to tackling the issue of radio loudness in quasars. We constrain a (simple) prescription for the intrinsic distribution of radio-to-optical ratios by comparing properties of Monte Carlo simulated samples with those of observed optically selected quasars. We find strong evidence for a dependence of the radio luminosity on the optical one, even though with a large scatter. The dependence of the fraction of radio-loud quasars on apparent and absolute optical magnitudes results in a selection effect related to the radio and optical limits of current surveys. The intrinsic distribution of the radio-to-optical ratios shows a peak at R 1.4* ∼ 0.3, with only ≲5 per cent of objects being included in a high-R1.4* tail, which identifies the radio-loud regime. No lack or deficit of sources - but only a steep transition region - is present between the radio-loud and radio-quiet populations at any R 1.4*. Briefly, we discuss possible origins for this behaviour (e.g. an absence of jets in radio-quiet sources, a large range of radiative radio efficiency, different lifetimes for the accretion and jet ejection phenomena, etc.).}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306415}, -author = {Cirasuolo, M. and Celotti, A. and Magliocchetti, M. and Danese, L.}, -doi = {10.1046/j.1365-2966.2003.07105.x}, -eprint = {0306415}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Galaxies: active,Radio continuum: general}, -month = {dec}, -number = {2}, -pages = {447--455}, -primaryClass = {astro-ph}, -title = {{Is there a dichotomy in the radio loudness distribution of quasars?}}, -volume = {346}, -year = {2003} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Wang2014a, -abstract = {Charged Coupled Devices (CCDs) have been successfully used in several low energy X-ray astronomical satellites over the past two decades. Their high energy resolution and high spatial resolution make them a perfect tool for low energy astronomy, such as observing the formation of galaxy clusters and the environment around black holes. The Low Energy X-ray Telescope (LE) group is developing a Swept Charge Device (SCD) for the Hard X-ray Modulation Telescope (HXMT) satellite. A SCD is a special low energy X-ray CCD, which can be read out a thousand times faster than traditional CCDs, simultaneously keeping excellent energy resolution. A test method for measuring the charge transfer efficiency (CTE) of a prototype SCD has been set up. Studies of the charge transfer inefficiency (CTI) with a proton-irradiated SCD have been performed at a range of operating temperatures. The SCD is irradiated by 3 × 10 8cm-2 10 MeV protons. {\textcopyright} 2014 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1308.1698}, -author = {Wang, Yu Sa and Yang, Yan Ji and Chen, Yong and Liu, Xiao Yan and Cui, Wei Wei and Xu, Yu Peng and Li, Cheng Kui and Li, Mao Shun and Han, Da Wei and Chen, Tian Xiang and Huo, Jia and Wang, Juan and Li, Wei and Hu, Wei and Zhang, Yi and Lu, Bo and Yin, Guo He and Zhu, Yue and Zhang, Zi Liang}, -doi = {10.1088/1674-1137/38/6/066001}, -eprint = {1308.1698}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2014 - Measurements of charge transfer efficiency in a proton-irradiated swept charge device.pdf:pdf}, -issn = {16741137}, -journal = {Chinese Physics C}, -keywords = {CCD,CTE,CTI,HXMT,LE,SCD,proton-irradiated}, -number = {6}, -pages = {066001}, -title = {{Measurements of charge transfer efficiency in a proton-irradiated swept charge device}}, -url = {http://stacks.iop.org/1674-1137/38/i=6/a=066001?key=crossref.02a5cb134fd3859a1cfa309d04df9b61}, -volume = {38}, -year = {2014} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyse sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in 255 deg2 of the Kilo Degree Survey (KiDS), one of the currentgeneration optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii ≳1.4 arcsec, about twice the r-band seeing in KiDS. In a sample of 21 789 colour-magnitude selected luminous red galaxies (LRGs), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find {\$\sim${}}100 massive LRGgalaxy lenses at z ≲ 0.4 in KiDS when completed. In the most optimistic scenario, this number can grow considerably (to maximally {\$\sim${}}2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C E and Tortora, C and Chatterjee, S and Vernardos, G and Koopmans, L V E and Kleijn, G Verdoes and Napolitano, N R and Covone, G and Schneider, P and Grado, A and McFarland, J}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys,cD}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P{\_}KS $\backslash$simeq 1.5 $\backslash$times 10{\^{}}{\{}-4{\}}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability $\backslash$simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R and Kravtsov, Andrey V and Gnedin, Oleg Y and Klypin, Anatoly A}, -doi = {10.1086/431355}, -eprint = {0502496}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Cohen2018, -abstract = {We present HST/ACS imaging of twenty-three very low surface brightness ($\mu_{e,V}$=25-27.5) galaxies detected in the fields of four nearby galaxy groups. These objects were selected from deep optical imaging obtained with the Dragonfly Telephoto Array. Seven are new discoveries, while most of the others had been identified previously in visual surveys of deep photographic plates and more recent surveys. Few have previously been studied in detail. From the ACS images, we measure distances to the galaxies using both the tip of the red giant branch method and the surface brightness fluctuations method. We demonstrate that the two methods are consistent with each other in the regime where both can be applied. The distances to 15 out of 20 galaxies with stable measurements are consistent with that of the targeted group within errors. This suggests that assuming group membership based solely on projected proximity is $\sim$75% successful in this regime. The galaxies are nearly round, with a median axis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The objects have a range of sizes, from $R_e$=0.4 kpc to $R_e$=1.8 kpc, with a median of 1.0 kpc. They range in luminosity from $M_V$=-11.4 to $M_V$=-15.6, with a median of -12.4. Galaxies with $R_e$$\sim$1 kpc and $M_V$$\sim$-12 are fairly rare in the Local Group but we find many of them in this relatively small sample. Four of the objects fall in the class of ultra diffuse galaxies (UDGs), with $R_e$>1.5 kpc and $\mu_{0,V}$>24 mag/arcsec^2, including the recently identified dark matter deficient galaxy NGC1052-DF2.}, -archivePrefix = {arXiv}, -arxivId = {1807.06016}, -author = {Cohen, Yotam and van Dokkum, Pieter and Danieli, Shany and Romanowsky, Aaron J. and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Mowla, Lamiya and Kruijssen, J. M. Diederik and Conroy, Charlie and Wasserman, Asher}, -doi = {10.3847/1538-4357/aae7c8}, -eprint = {1807.06016}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cohen et al. - 2018 - The Dragonfly Nearby Galaxies Survey. V. HST ACS Observations of 23 Low Surface Brightness Objects in the Field(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {Astrophysics,Astrophysics of Galaxies}, -number = {2}, -pages = {96}, -title = {{ The Dragonfly Nearby Galaxies Survey. V. HST /ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC 1052, NGC 1084, M96, and NGC 4258 }}, -url = {http://arxiv.org/abs/1807.06016%0Ahttp://dx.doi.org/10.3847/1538-4357/aae7c8}, -volume = {868}, -year = {2018} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Bullock2005a, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print)$\backslash$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Eales2014, -abstract = {Surveys with submillimetre telescopes are revealing large numbers of gravitationally lensed high-redshift sources. I describe how, in practice, these lensed systems could be simultaneously used to estimate the values of cosmological parameters, test models for the evolution of the distribution of dark-matter haloes and investigate the properties of the source population. Even the existing sample of lenses found with the Herschel Space Observatory is enough to formally rule out the standard models of the evolving population of dark-matter haloes, with the likely explanation a combination of baryon physics and the perturbation by infalling baryons of the density distribution of dark matter at the centres of the haloes. Independently of the evolution of the haloes, observations of a sample of 100 lensed systems would be enough to estimate $\Omega$$\Lambda$ with a precision of 5 per cent and observations of 1000 lenses would be enough to estimate $\omega$, the parameter in the equation of state of dark energy, with a precision similar to that obtained from the Planck observations of the cosmic microwave background. While the fraction of submillimetre sources that are lensed depends weakly on the specific halo mass function that is used in the model, it depends very strongly on the evolution of the submillimetre luminosity function of the source population. Therefore measurements of the lensing fraction could be used to investigate galaxy evolution in a way that is independent of the properties of the intervening haloes.}, -archivePrefix = {arXiv}, -arxivId = {1312.1242}, -author = {Eales, S. A.}, -doi = {10.1093/mnras/stu2214}, -eprint = {1312.1242}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmological parameters,Cosmology: observations,Dark matter,Galaxies: high-redshift,Submillimetre: galaxies}, -number = {3}, -pages = {3224--3234}, -title = {{Practical cosmology with lenses}}, -url = {http://mnras.oxfordjournals.org/cgi/doi/10.1093/mnras/stu2214}, -volume = {446}, -year = {2015} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as 'notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude ({\textless}50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 {\textless} G {\textless} 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G M and Prod'homme, T and Murray, N J and Crowley, C and Hopkinson, G and Brown, A G A and Kohley, R and Holland, A}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Bartelmann1999, -abstract = {We review theory and applications of weak gravitational lensing. After summarising Friedmann-Lema{\^{i}}tre cosmological models, we present the formalism of gravitational lensing and light propagation in arbitrary space-times. We discuss how weak-lensing effects can be measured. The formalism is then applied to reconstructions of galaxy-cluster mass distributions, gravitational lensing by large-scale matter distributions, QSO-galaxy correlations induced by weak lensing, lensing of galaxies by galaxies, and weak lensing of the cosmic microwave background. {\textcopyright}2001 Elsevier Science B.V.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9912508}, -author = {Bartelmann, Matthias and Schneider, Peter}, -doi = {10.1016/S0370-1573(00)00082-X}, -eprint = {9912508}, -issn = {03701573}, -journal = {Physics Report}, -number = {4-5}, -pages = {291--472}, -primaryClass = {astro-ph}, -title = {{Weak gravitational lensing}}, -url = {http://arxiv.org/abs/astro-ph/9912508%7B%5C%25%7D0Ahttp://dx.doi.org/10.1016/S0370-1573(00)00082-X}, -volume = {340}, -year = {2001} -} -@article{Oriordan2021, -abstract = {When modelling strong gravitational lenses, i.e. where there are multiple images of the same source, the most widely used parametrization for the mass profile in the lens galaxy is the singular power-law model $\rho$(r)⋊ r-$\gamma$. This model may be insufficiently flexible for very accurate work, for example, measuring the Hubble constant based on time delays between multiple images. Here, we derive the lensing properties - deflection angle, shear, and magnification - of a more adaptable model where the projected mass surface density is parametrized as a continuous two-dimensional broken power law (2DBPL). This elliptical 2DBPL model is characterized by power-law slopes t1 and t2 either side of the break radius $\theta$B. The key to the 2DBPL model is the derivation of the lensing properties of the truncated power-law (TPL) model, where the surface density is a power law out to the truncation radius $\theta$T and zero beyond. This TPL model is also useful by itself. We create mock observations of lensing by a TPL profile where the images form outside the truncation radius, so there is no mass in the annulus covered by the images. We then show that the slope of the profile interior to the images may be accurately recovered for lenses of moderate ellipticity. This demonstrates that the widely held notion that lensing measures the slope of the mass profile in the annulus of the images, and is insensitive to the mass distribution at radii interior to the images, is incorrect.}, -archivePrefix = {arXiv}, -arxivId = {2007.11588}, -author = {O'Riordan, C. M. and Warren, S. J. and Mortlock, D. J.}, -doi = {10.1093/mnras/staa3747}, -eprint = {2007.11588}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/ORiodan2020BPL3.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {galaxies: General,gravitational lensing: Strong}, -number = {3}, -pages = {3687--3694}, -title = {{Galaxy mass profiles from strong lensing - III. The two-dimensional broken power-law model}}, -volume = {501}, -year = {2021} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C. and Mo, H. J. and Mao, Shude and Kang, Xi and Weinmann, Simone M. and Guo, Yicheng and Jing, Y. P.}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yang et al. - 2006 - The alignment between the distribution of satellites and the orientation of their central galaxy(3).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Halverson2016, -abstract = {We describe a detailed radial velocity error budget for the NASA-NSF Extreme Precision Doppler Spectrometer instrument concept NEID (NN-explore Exoplanet Investigations with Doppler spectroscopy). Such an instrument performance budget is a necessity for both identifying the variety of noise sources currently limiting Doppler measurements, and estimating the achievable performance of next generation exoplanet hunting Doppler spectrometers. For these instruments, no single source of instrumental error is expected to set the overall measurement floor. Rather, the overall instrumental measurement precision is set by the contribution of many individual error sources. We use a combination of numerical simulations, educated estimates based on published materials, extrapolations of physical models, results from laboratory measurements of spectroscopic subsystems, and informed upper limits for a variety of error sources to identify likely sources of systematic error and construct our global instrument performance error budget. While natively focused on the performance of the NEID instrument, this modular performance budget is immediately adaptable to a number of current and future instruments. Such an approach is an important step in charting a path towards improving Doppler measurement precisions to the levels necessary for discovering Earth-like planets.}, -archivePrefix = {arXiv}, -arxivId = {1607.05634}, -author = {Halverson, Samuel and Terrien, Ryan and Mahadevan, Suvrath and Roy, Arpita and Bender, Chad and Stef{\'{a}}nsson, Gudmundur K and Monson, Andrew and Levi, Eric and Hearty, Fred and Blake, Cullen and McElwain, Michael and Schwab, Christian and Ramsey, Lawrence and Wright, Jason and Wang, Sharon and Gong, Qian and Roberston, Paul}, -doi = {10.1117/12.2232761}, -eprint = {1607.05634}, -isbn = {9781510601956}, -issn = {0277-786X}, -journal = {Ground-based and Airborne Instrumentation for Astronomy VI}, -keywords = {exoplanets,high resolution spectroscopy,radial velocity instrumentation,systems engineering}, -pages = {99086P}, -title = {{A comprehensive radial velocity error budget for next generation Doppler spectrometers}}, -url = {http://arxiv.org/abs/1607.05634%7B%5C%25%7D0Ahttp://dx.doi.org/10.1117/12.2232761}, -volume = {9908}, -year = {2016} -} -@article{Ma2014, -abstract = {Massive early-type galaxies represent the modern day remnants of the earliest major star formation episodes in the history of the universe. These galaxies are central to our understanding of the evolution of cosmic structure, stellar populations, and supermassive black holes, but the details of their complex formation histories remain uncertain. To address this situation, we have initiated the MASSIVE Survey, a volume-limited, multi-wavelength, integral-field spectroscopic (IFS) and photometric survey of the structure and dynamics of the {\$\sim${}}100 most massive early-type galaxies within a distance of 108 Mpc. This survey probes a stellar mass range M* {\textgreater}{\$\sim${}} 1011.5 M ⊙ and diverse galaxy environments that have not been systematically studied to date. Our wide-field IFS data cover about two effective radii of individual galaxies, and for a subset of them, we are acquiring additional IFS observations on sub-arcsecond scales with adaptive optics. We are also acquiring deep K-band imaging to trace the extended halos of the galaxies and measure accurate total magnitudes. Dynamical orbit modeling of the combined data will allow us to simultaneously determine the stellar, black hole, and dark matter halo masses. The primary goals of the project are to constrain the black hole scaling relations at high masses, investigate systematically the stellar initial mass function and dark matter distribution in massive galaxies, and probe the late-time assembly of ellipticals through stellar population and kinematical gradients. In this paper, we describe the MASSIVE sample selection, discuss the distinct demographics and structural and environmental properties of the selected galaxies, and provide an overview of our basic observational program, science goals and early survey results.}, -archivePrefix = {arXiv}, -arxivId = {1407.1054}, -author = {Ma, Chung Pei and Greene, Jenny E and McConnell, Nicholas and Janish, Ryan and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/795/2/158}, -eprint = {1407.1054}, -isbn = {0000000000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content,galaxies: structure}, -number = {2}, -pages = {158}, -pmid = {28562576}, -title = {{The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...795..158M}, -volume = {795}, -year = {2014} -} -@article{Barro2013, -abstract = {We combine high-resolution Hubble Space Telescope/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (M* > 1010 M⊙) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z ≳ 2, cSFGs present SFR = 100-200 M yr-1, yet their specific star formation rates (sSFR ∼ 10-9 yr -1) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (∼30%) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 108 yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z ∼ 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z ≳ 2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z ≲ 2) path in which larger SFGs form extended QGs without passing through a compact state. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1206.5000}, -author = {Barro, Guillermo and Faber, S. M. and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G. and Koo, David C. and Williams, Christina C. and Kocevski, Dale D. and Trump, Jonathan R. and Mozena, Mark and McGrath, Elizabeth and {Van Der Wel}, Arjen and Wuyts, Stijn and Bell, Eric F. and Croton, Darren J. and Daniel, Ceverino and Dekel, Avishai and Ashby, M. L.N. and Cheung, Edmond and Ferguson, Henry C. and Fontana, Adriano and Fang, Jerome and Giavalisco, Mauro and Grogin, Norman A. and Guo, Yicheng and Hathi, Nimish P. and Hopkins, Philip F. and Huang, Kuang Han and Koekemoer, Anton M. and Kartaltepe, Jeyhan S. and Lee, Kyoung Soo and Newman, Jeffrey A. and Porter, Lauren A. and Primack, Joel R. and Ryan, Russell E. and Rosario, David and Somerville, Rachel S. and Salvato, Mara and Hsu, Li Ting}, -doi = {10.1088/0004-637X/765/2/104}, -eprint = {1206.5000}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Barro et al. - 2013 - Candels The progenitors of compact quiescent galaxies at Z ∼ 2.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {galaxies: high-redshift,galaxies: photometry,galaxies: starburst}, -number = {2}, -pmid = {7117407}, -title = {{Candels: The progenitors of compact quiescent galaxies at Z ∼ 2}}, -volume = {765}, -year = {2013} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the 'Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a (100 cMpc)3 and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts 0 and 1, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar 'downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Greene2017b, -abstract = {The "kinematic" morphology-density relation for early-type galaxies posits that those galaxies with low angular momentum are preferentially found in the highest-density regions of the universe. We use a large sample of galaxy groups with halo masses 10{\^{}}12.5 {\textless} M{\_}halo {\textless} 10{\^{}}14.5 M{\_}sun/h observed with the Mapping Nearby Galaxies at APO (MaNGA) survey to examine whether there is a correlation between local environment and rotational support that is independent of stellar mass. We find no compelling evidence for a relationship between the angular momentum content of early-type galaxies and either local overdensity or radial position within the group at fixed stellar mass.}, -archivePrefix = {arXiv}, -arxivId = {1708.07843}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Goddard, D and Ge, J and Andrews, B H and Brinkman, J and Brownstein, J R and Greco, J P and Law, D and Lin, Y -T. and Masters, K L and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Yan, R and Drory, N}, -doi = {10.3847/2041-8213/aa8ace}, -eprint = {1708.07843}, -issn = {2041-8213}, -pages = {1--6}, -title = {{Probing the kinematic morphology-density relation of early-type galaxies with MaNGA}}, -url = {http://arxiv.org/abs/1708.07843%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa8ace}, -year = {2017} -} -@article{Mandelbaum2017, -abstract = {Weak gravitational lensing, the deflection of light by mass, is one of the best tools to constrain the growth of cosmic structure with time and reveal the nature of dark energy. I discuss the sources of systematic uncertainty in weak lensing measurements and their theoretical interpretation, including our current understanding and other options for future improvement. These include long-standing concerns such as the estimation of coherent shears from galaxy images or redshift distributions of galaxies selected on the basis of photometric redshifts, along with systematic uncertainties that have received less attention to date because they are subdominant contributors to the error budget in current surveys. I also discuss methods for automated systematics detection using survey data of the 2020s. The goal of this review is to describe the current state of the field and what must be done so that if weak lensing measurements lead toward surprising conclusions about key questions such as the nature of dark energy, those conclusions will be credible.}, -archivePrefix = {arXiv}, -arxivId = {1710.03235}, -author = {Mandelbaum, Rachel}, -doi = {10.1146/annurev-astro-081817-051928}, -eprint = {1710.03235}, -issn = {0066-4146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {cosmological parameters,cosmology,data analysis,gravitational lensing,image processing,methods,statistical,techniques}, -number = {1}, -pages = {393--433}, -title = {{Weak Lensing for Precision Cosmology}}, -url = {http://arxiv.org/abs/1710.03235%7B%5C%25%7D0Ahttp://dx.doi.org/10.1146/annurev-astro-081817-051928}, -volume = {56}, -year = {2018} -} -@article{Eisenstein2001, -abstract = {We describe the target selection and resulting properties of a spectroscopic sample of luminous, red galaxies (LRG) from the imaging data of the Sloan Digital Sky Survey (SDSS). These galaxies are selected on the basis of color and magnitude to yield a sample of luminous, intrinsically red galaxies that extends fainter and further than the main flux-limited portion of the SDSS galaxy spectroscopic sample. The sample is designed to impose a passively-evolving luminosity and rest-frame color cut to a redshift of 0.38. Additional, yet more luminous, red galaxies are included to a redshift of 0.5. Approximately 12 of these galaxies per square degree are targeted for spectroscopy, so the sample will number over 100,000 with the full survey. SDSS commissioning data indicate that the algorithm efficiently selects luminous (M_g=-21.4), red galaxies, that the spectroscopic success rate is very high, and that the resulting set of galaxies is approximately volume-limited out to z=0.38. When the SDSS is complete, the LRG spectroscopic sample will fill over 1h^-3 Gpc^3 with an approximately homogeneous population of galaxies and will therefore be well suited to studies of large-scale structure and clusters out to z=0.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108153}, -author = {Eisenstein, Daniel J. and Annis, James and Gunn, James E. and Szalay, Alexander S. and Connolly, Andrew J. and Nichol, R. C. and Bahcall, Neta A. and Bernardi, Mariangela and Burles, Scott and Castander, Francisco J. and Fukugita, Masataka and Hogg, David W. and Ivezi{\'{c}}, {\v{Z}}eljko and Knapp, G. R. and Lupton, Robert H. and Narayanan, Vijay and Postman, Marc and Reichart, Daniel E. and Richmond, Michael and Schneider, Donald P. and Schlegel, David J. and Strauss, Michael A. and SubbaRao, Mark and Tucker, Douglas L. and {Vanden Berk}, Daniel and Vogeley, Michael S. and Weinberg, David H. and Yanny, Brian}, -doi = {10.1086/323717}, -eprint = {0108153}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Eisenstein et al. - 2001 - Spectroscopic Target Selection for the Sloan Digital Sky Survey The Luminous Red Galaxy Sample.pdf:pdf}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2267--2280}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample}}, -url = {http://arxiv.org/abs/astro-ph/0108153%0Ahttp://dx.doi.org/10.1086/323717}, -volume = {122}, -year = {2001} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, n=10[cm-3], results in strong expansion of the DM halo in galaxies with stellar masses in the range 107.5 ≤ Mstar ≤ 109.5 M⊙. We find that lower thresholds such as n = 0.1 (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e. ≤50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with n = 10 have gas fractions of ∼0.2 and variations of ∼0.1, while n = 0.1 simulations have order of magnitude lower gas fractions and hence do not expand the halo. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with n = 0.1 and n = 1, but in a reasonable agreement with n = 10. Star formation rates are more variable for higher n, lower galaxy masses, and when star formation is measured on shorter time-scales. For example, simulations with n = 10 have up to 0.4 dex higher scatter in specific star formation rates than simulations with n = 0.1. Thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625}, -author = {Dutton, Aaron A and MacCi{\`{o}}, Andrea V and Buck, Tobias and Dixon, Keri L and Blank, Marvin and Obreja, Aura}, -doi = {10.1093/mnras/stz889}, -eprint = {1811.10625}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure,methods: numerical}, -number = {1}, -pages = {655--671}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://arxiv.org/abs/1811.10625%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stz889}, -volume = {486}, -year = {2019} -} -@article{Version2018, -abstract = {We perform a systematic search for sub-parsec binary supermassive black holes (BHs) in normal broad-line quasars at z {\textless} 0.8, using multi-epoch Sloan Digital Sky Survey (SDSS) spectroscopy of the broad H$\beta$ line. Our working model is that (1) one and only one of the two BHs in the binary is active; (2) the active BH dynamically dominates its own broad-line region (BLR) in the binary system, so that the mean velocity of the BLR reflects the mean velocity of its host BH; (3) the inactive companion BH is orbiting at a distance of a few R BLR, where R BLR 0.01-0.1 pc is the BLR size. We search for the expected line-of-sight acceleration of the broad-line velocity from binary orbital motion by cross-correlating SDSS spectra from two epochs separated by up to several years in the quasar rest frame. Out of 00 pairs of spectra for which we have good measurements of the velocity shift between two epochs (1$\sigma$ error 0 km s-1), we detect 28 systems with significant velocity shifts in broad H$\beta$, among which 7 are the best candidates for the hypothesized binaries, 4 are most likely due to broad-line variability in single BHs, and the rest are ambiguous. Continued spectroscopic observations of these candidates will easily strengthen or disprove these claims. We use the distribution of the observed accelerations (mostly non-detections) to place constraints on the abundance of such binary systems among the general quasar population. Excess variance in the velocity shift is inferred for observations separated by longer than 0.4 yr (quasar rest frame). Attributing all the excess to binary motion would imply that most of the quasars in this sample must be in binaries, that the inactive BH must be on average more massive than the active one, and that the binary separation is at most a few times the size of the BLR. However, if this excess variance is partly or largely due to long-term broad-line variability, the requirement of a large population of close binaries is much weakened or even disfavored for massive companions. Future time-domain spectroscopic surveys of normal quasars can provide vital prior information on the structure function of stochastic velocity shifts induced by broad-line variability in single BHs. Such surveys with improved spectral quality, increased time baseline, and more epochs can greatly improve the statistical constraints of this method on the general binary population in broad-line quasars, further shrink the allowed binary parameter space, and detect true sub-parsec binaries. {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1306.4330}, -author = {Shen, Yue and Liu, Xin and Loeb, Abraham and Tremaine, Scott}, -doi = {10.1088/0004-637X/775/1/49}, -eprint = {1306.4330}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {black hole physics,galaxies: active,line: profiles,quasars: general,surveys}, -number = {1}, -title = {{Constraining sub-parsec binary supermassive black holes in quasars with multi-epoch spectroscopy. I. the general quasar population}}, -volume = {775}, -year = {2013} -} -@article{Dullo2019, -abstract = {[Abridged] Luminous spheroids (M_V < - 21.50 +- 0.75 mag) contain partially depleted cores with sizes (R_ b) typically 0.02 - 0.5 kpc. However, galaxies with R_b > 0.5 kpc are rare and poorly understood. Here we perform detailed decompositions of the composite surface brightness profiles, extracted from archival Hubble Space Telescope and ground-based images, of 12 extremely luminous "large-core" galaxies that have R_b > 0.5 kpc and M_V < -23.50 +- 0.10 mag, fitting a core-S\'ersic model to the galaxy spheroids. Using 28 "normal-core" (i.e., R_b < 0.5 kpc) galaxies and 1 "large-core" (i.e., R_b > 0.5 kpc) galaxy from the literature, we constructed a final sample of 41 core-S\'ersic galaxies. We find that large-core spheroids (with stellar masses M_* > 10^12 M_sun) are not simple high-mass extensions of the less luminous normal-core spheroids having M_* $\sim$ 8 x 10^10 - 10^12 M_sun. While the two types follow the same strong relations between the spheroid luminosity L_V and R_b (R_b prop L_V^(1.38 +- 0.13), and the spheroid half-light radius R_e (R_e prop L_V^(1.08 +- 0.09), for ellipticals plus BCGs), we discover a break in the core-S\'ersic sigma-L_V relation occurring at M_V $\sim$ -23.50 +- 0.10 mag. Furthermore, we find a strong log-linear R_b-M_BH relation for the 11 galaxies in the sample with directly determined SMBH masses M_BH---3/11 galaxies are large-core galaxies ---such that R_b prop M_BH^(0.83 +- 0.10). However, for the large-core galaxies the SMBH masses estimated from the M_BH-sigma and core-S\'ersic M_BH-L relations are undermassive, by up to a factor of 40, relative to expectations from their large R_b values, confirming earlier results. Our findings suggest that large-core galaxies harbour overmassive SMBHs (M_BH > 10^10 M_sun), considerably ($\sim$ 3.7-15.6 sigma and $\sim$ 0.6-1.7 sigma) larger than expectations from the spheroid sigma and L, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1910.10240}, -author = {Dullo, Bililign T.}, -doi = {10.3847/1538-4357/ab4d4f}, -eprint = {1910.10240}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dullo - 2019 - The Most Massive Galaxies with Large Depleted Cores Structural Parameter Relations and Black Hole Masses.pdf:pdf}, -issn = {1538-4357}, -journal = {ApJ}, -number = {2}, -pages = {80}, -title = {{The Most Massive Galaxies with Large Depleted Cores: Structural Parameter Relations and Black Hole Masses}}, -url = {http://arxiv.org/abs/1910.10240}, -volume = {886}, -year = {2019} -} -@article{Spavone2017, -abstract = {{\textcopyright}2017 ESO. Observations of diffuse starlight in the outskirts of galaxies are thought to be a fundamental source of constraint on the cosmological context of galaxy assembly in the $\Lambda$CDM model. Such observations are not trivial because of the extreme faintness of such regions. In this work, we investigated the photometric properties of six massive early-type galaxies (ETGs) in the VEGAS sample (NGC 1399, NGC 3923, NGC 4365, NGC 4472, NGC 5044, and NGC 5846) out to extremely low surface brightness levels with the goal of characterizing the global structure of their light profiles for comparison to state-of-the-art galaxy formation models. We carried out deep and detailed photometric mapping of our ETG sample taking advantage of deep imaging with VST/OmegaCAM in the g and i bands. By fitting the light profiles, and comparing the results to simulations of elliptical galaxy assembly, we have identified signatures of a transition between relaxed and unrelaxed accreted components and can constrain the balance between in situ and accreted stars. The very good agreement of our results with predictions from theoretical simulations demonstrates that the full VEGAS sample of {\$\sim${}}100 ETGs will allow us to use the distribution of diffuse light as a robust statistical probe of the hierarchical assembly of massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1703.10835}, -author = {Spavone, Marilena and Capaccioli, Massimo and Napolitano, Nicola R and Iodice, Enrichetta and Grado, Aniello and Limatola, Luca and Cooper, Andrew P and Cantiello, Michele and Forbes, Duncan A and Paolillo, Maurizio and Schipani, Pietro}, -doi = {10.1051/0004-6361/201629111}, -eprint = {1703.10835}, -issn = {0004-6361}, -journal = {Astronomy {\&} Astrophysics}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: halos,Techniques: image processing,cD}, -number = {3}, -pages = {A38}, -title = {{VEGAS: A VST Early-type GAlaxy Survey}}, -url = {http://www.aanda.org/10.1051/0004-6361/201629111}, -volume = {603}, -year = {2017} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the foreground lenses and background sources are early-type galaxies. Using imaging from Hubble Space Telescope (HST)/Advanced Camera for Studies (ACS) andKeck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population ofmassive, compact galaxies at redshifts 0.4 ≲ z ≲ 0.7, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of highredshift red nuggets or their partly evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar populations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S{\'{e}}rsic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still compact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterized by red-to-blue colour gradients as a function of radius which are stronger at low redshift - indicative of ongoing accretion - but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are pre-dominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W. and Fassnacht, Christopher D. and Treu, Tommaso and Brewer, Brendon J. and Koopmans, L. V.E. and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oldham et al. - 2017 - Red nuggets grow inside-out Evidence from gravitational lensing.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Geometryep, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Morishita2018a, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {evolution,formation,galaxies,star formation}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Calore2014, -abstract = {Millisecond pulsars (MSPs) are old fast-spinning neutron stars that represent the second most abundant source population discovered by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope (Fermi). As guaranteed $\gamma$-ray emitters, they might contribute non-negligibly to the diffuse emission measured at high latitudes by Fermi-LAT (i.e., the Isotropic Diffuse $\gamma$-Ray Background (IDGRB)), which is believed to arise from the superposition of several components of galactic and extragalactic origin. Additionally, $\gamma$-ray sources also contribute to the anisotropy of the IDGRB measured on small scales by Fermi-LAT. In this manuscript we aim to assess the contribution of the unresolved counterpart of the detected MSPs population to the IDGRB and the maximal fraction of the measured anisotropy produced by this source class. To this end, we model the MSPs' spatial distribution in the Galaxy and the $\gamma$-ray emission parameters by considering observational constraints coming from the Australia Telescope National Facility pulsar catalog and the Second Fermi-LAT Catalog of $\gamma$-ray pulsars. By simulating a large number of MSP populations through a Monte Carlo simulation, we compute the average diffuse emission and the anisotropy 1$\sigma$ upper limit. We find that the emission from unresolved MSPs at 2 GeV, where the peak of the spectrum is located, is at most 0.9% of the measured IDGRB above 10° in latitude. The 1$\sigma$ upper limit on the angular power for unresolved MSP sources turns out to be about a factor of 60 smaller than Fermi-LAT measurements above 30°. Our results indicate that this galactic source class represents a negligible contributor to the high-latitude $\gamma$-ray sky and confirm that most of the intensity and geometrical properties of the measured diffuse emission are imputable to other extragalactic source classes (e.g., blazars, misaligned active galactic nuclei, or star-forming galaxies). Nevertheless, because MSPs are more concentrated toward the galactic center, we expect them to contribute significantly to the $\gamma$-ray diffuse emission at low latitudes. Because, along the galactic disk, the population of young pulsars overcomes in number that of MSPs, we compute the $\gamma$-ray emission from the whole population of unresolved pulsars, both young and millisecond, in two low-latitude regions: the inner Galaxy and the galactic center.}, -archivePrefix = {arXiv}, -arxivId = {1406.2706}, -author = {Calore, F. and {Di Mauro}, M. and Donato, F.}, -doi = {10.1088/0004-637X/796/1/14}, -eprint = {1406.2706}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {gamma rays: diffuse background}, -number = {1}, -pages = {14}, -title = {{Diffuse $\gamma$-ray emission from galactic pulsars}}, -url = {http://stacks.iop.org/0004-637X/796/i=1/a=14?key=crossref.f8fce2f05305d1112c8bc78e23f499d0}, -volume = {796}, -year = {2014} -} -@article{Mendez-Abreu2010a, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A < 0.9). This fraction is 33%, 55%, and 43% if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C < (A + B)/2). Only 18% of the observed bulges have a probability >50% and none has a probability >90% of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n > 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T > 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n > 2 and B/T > 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n > 2 and with B/T > 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n > 2 and B/T > 0.3. {\textcopyright} 2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J. and Simonneau, E. and Aguerri, J. A.L. and Corsini, E. M.}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/M{\'{e}}ndez-Abreu et al. - 2010 - Structural properties of disk galaxies II. Intrinsic shape of bulges.pdf:pdf}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {galaxies: bulges,galaxies: elliptical and lenticular, cD,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Barkana1998, -abstract = {Because of their simplicity, axisymmetric mass distributions are often used to model gravitational lenses. Since galaxies are usually observed to have elliptical light distributions, mass distributions with elliptical density contours offer more general and realistic lens models. They are difficult to use, however, since previous studies have shown that the deflection angle (and magnification) in this case can only be obtained by rather expensive numerical integrations. We present a family of lens models for which the deflection can be calculated to high relative accuracy (10-5) with a greatly reduced numerical effort, for small and large ellipticity alike. This makes it easier to use these distributions for modeling individual lenses as well as for applications requiring larger computing times, such as statistical lensing studies. A program implementing this method can be obtained from the author. 1}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9802002}, -author = {Barkana, Rennan}, -doi = {10.1086/305950}, -eprint = {9802002}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Structure}, -month = {aug}, -number = {2}, -pages = {531--537}, -primaryClass = {astro-ph}, -title = {{Fast Calculation of a Family of Elliptical Gravitational Lens Models}}, -url = {http://stacks.iop.org/0004-637X/502/i=2/a=531}, -volume = {502}, -year = {2002} -} -@article{Kormendy1995, -abstract = {Predicting the binding mode of flexible polypeptides to proteins is an important task that falls outside the domain of applicability of most small molecule and protein−protein docking tools. Here, we test the small molecule flexible ligand docking program Glide on a set of 19 non-$\alpha$-helical peptides and systematically improve pose prediction accuracy by enhancing Glide sampling for flexible polypeptides. In addition, scoring of the poses was improved by post-processing with physics-based implicit solvent MM- GBSA calculations. Using the best RMSD among the top 10 scoring poses as a metric, the success rate (RMSD ≤ 2.0 {\AA} for the interface backbone atoms) increased from 21% with default Glide SP settings to 58% with the enhanced peptide sampling and scoring protocol in the case of redocking to the native protein structure. This approaches the accuracy of the recently developed Rosetta FlexPepDock method (63% success for these 19 peptides) while being over 100 times faster. Cross-docking was performed for a subset of cases where an unbound receptor structure was available, and in that case, 40% of peptides were docked successfully. We analyze the results and find that the optimized polypeptide protocol is most accurate for extended peptides of limited size and number of formal charges, defining a domain of applicability for this approach.}, -author = {Kormendy, John and Richstone, Douglas}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Kormendy1995SearchInward.pdf:pdf}, -journal = {Annual Review of Astronomy and Astrophysics}, -pages = {581}, -title = {{Inward Bound---The Search For Supermassive Black Holes In Galactic Nuclei}}, -volume = {33}, -year = {1995} -} -@article{Eales2010, -abstract = {The Herschel ATLAS is the largest open-time key project that will be carried out on the Herschel Space Observatory. It will survey 510 square degrees of the extragalactic sky, four times larger than all the other Herschel surveys combined, in five far-infrared and submillimetre bands. We describe the survey, the complementary multi-wavelength datasets that will be combined with the Herschel data, and the six major science programmes we are undertaking. Using new models based on a previous submillimetre survey of galaxies, we present predictions of the properties of the ATLAS sources in other wavebands.}, -archivePrefix = {arXiv}, -arxivId = {0910.4279}, -author = {Eales, S. and Dunne, L. and Clements, D. and Cooray, A. and {De Zotti}, G. and Dye, S. and Ivison, R. and Jarvis, M. and Lagache, G. and Maddox, S. and Negrello, M. and Serjeant, S. and Thompson, M. A. and Kampen, E. Van and Amblard, A. and Andreani, P. and Baes, M. and Beelen, A. and Bendo, G. J. and Benford, D. and Bertoldi, F. and Bock, J. and Bonfield, D. and Boselli, A. and Bridge, C. and Buat, V. and Burgarella, D. and Carlberg, R. and Cava, A. and Chanial, P. and Charlot, S. and Christopher, N. and Coles, P. and Cortese, L. and Dariush, A. and da Cunha, E. and Dalton, G. and Danese, L. and Dannerbauer, H. and Driver, S. and Dunlop, J. and Fan, L. and Farrah, D. and Frayer, D. and Frenk, C. and Geach, J. and Gardner, J. and Gomez, H. and Gonz{\'{a}}lez-Nuevo, J. and Gonz{\'{a}}lez-Solares, E. and Griffin, M. and Hardcastle, M. and Hatziminaoglou, E. and Herranz, D. and Hughes, D. and Ibar, E. and Jeong, Woong-Seob and Lacey, C. and Lapi, A. and Lawrence, A. and Lee, M. and Leeuw, L. and Liske, J. and L{\'{o}}pez-Caniego, M. and M{\"{u}}ller, T. and Nandra, K. and Panuzzo, P. and Papageorgiou, A. and Patanchon, G. and Peacock, J. and Pearson, C. and Phillipps, S. and Pohlen, M. and Popescu, C. and Rawlings, S. and Rigby, E. and Rigopoulou, M. and Robotham, A. and Rodighiero, G. and Sansom, A. and Schulz, B. and Scott, D. and Smith, D. J. B. and Sibthorpe, B. and Smail, I. and Stevens, J. and Sutherland, W. and Takeuchi, T. and Tedds, J. and Temi, P. and Tuffs, R. and Trichas, M. and Vaccari, M. and Valtchanov, I. and van der Werf, P. and Verma, A. and Vieria, J. and Vlahakis, C. and White, Glenn J.}, -doi = {10.1086/653086}, -eprint = {0910.4279}, -isbn = {0004-6280}, -issn = {0004-6280}, -journal = {Publications of the Astronomical Society of the Pacific}, -number = {891}, -pages = {499--515}, -pmid = {277175800001}, -title = {{The Herschel ATLAS}}, -url = {http://iopscience.iop.org/article/10.1086/653086}, -volume = {122}, -year = {2010} -} -@article{Talbot2018, -abstract = {We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for 8 of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with 2 background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched {\$\sim${}} 1.5 million spectra, of which 3065 contained multiple high signal-to-noise background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius {\textgreater} 1.7", which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely.}, -archivePrefix = {arXiv}, -arxivId = {1803.03604}, -author = {Talbot, Michael S and Brownstein, Joel R and Bolton, Adam S and Bundy, Kevin and Andrews, Brett H and Cherinka, Brian and Collett, Thomas E and More, Anupreeta and More, Surhud and Sonnenfeld, Alessandro and Vegetti, Simona and Wake, David A and Weijmans, Anne Marie and Westfall, Kyle B}, -doi = {10.1093/mnras/sty653}, -eprint = {1803.03604}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: General,Gravitational lensing: Strong}, -number = {1}, -pages = {195--209}, -title = {{SDSS-IV MaNGA: The spectroscopic discovery of strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1803.03604%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty653}, -volume = {477}, -year = {2018} -} -@article{Deason2011, -abstract = {(Abridged) We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the GIMIC suite of simulations. GIMIC consists of re-simulations of 5 cosmologically representative regions from the Millennium simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r {\$\sim${}} 0.1r{\_}200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r {\$\sim${}} r{\_}200). Misalignments of {\textgreater} 45 deg are seen in {\$\sim${}} 30{\%} of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20{\%} of the satellite systems with ten bright galaxies within r{\_}200 exhibit a polar spatial alignment with respect to the galaxy --- an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction ({\$\sim${}}10{\%}) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z=0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation --- the memory of their accretion history can remain intact to z=0.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A J and Mccarthy, I G and Font, A S and Evans, N W and Frenk, C S and Belokurov, V and Libeskind, N I and Crain, R A and Theuns, T}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Sales2012, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V. and Navarro, Julio F. and Theuns, Tom and Schaye, Joop and White, Simon D.M. and Frenk, Carlos S. and Crain, Robert A. and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sales et al. - 2012 - The origin of discs and spheroids in simulated galaxies(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Keeton2003b, -abstract = {When the source in a four-image gravitational lens system lies sufficiently close to a fold caustic, two of the lensed images lie very close together. If the lens potential is smooth on the scale of the separation between the two close images, the difference between their fluxes should approximately vanish, Rfold ≡ (F+ - F-)/(F+ + F-) ≈ 0. (The subscript indicates the image parity.) Violations of this fold relation in observed lenses are thought to indicate the presence of structure on scales smaller than the separation between the close images. We present a detailed study of the fold relation in realistic smooth lenses, finding it to be more subtle and rich than was previously realized. The degree to which Rfold can differ from zero for smooth lenses depends not only on the distance of the source from the caustic, but also on its location along the caustic, and then on the angular structure of the lens potential (ellipticity, multipole modes, and external shear). Since the source position is unobservable, it is impossible to say from Rfold alone whether the flux ratios in an observed lens are anomalous or not. Instead, we must consider the full distribution of Rfold values that can be obtained from smooth lens potentials that reproduce the separation d1 between the two close images and the distance d2 to the next nearest image. (By reducing the image configuration to these two numbers, we limit our model dependence and obtain a generic analysis.) We show that the generic features of this distribution can be understood, which means that the fold relation provides a robust probe of small-scale structure in lens galaxies. We then compute the full distribution using Monte Carlo simulations of realistic smooth lenses. Comparing these predictions with the data, we find that five of the 12 known lenses with fold configurations have flux ratio anomalies: B0712+472, SDSS 0924+0219, PG 1115+080, B1555+375, and B1933+503. Combining this with our previous analysis revealing anomalies in three of the four known lenses with cusp configurations, we conclude that at least half (8/16) of all four-image lenses that admit generic, local analyses exhibit flux ratio anomalies. The fold and cusp relations do not reveal the nature of the implied small-scale structure, but do provide the formal foundation for substructure studies, and also indicate which lenses deserve further study. Although our focus is on close pairs of images, we show that the fold relation can be used—with great care—to analyze all image pairs in all 22 known four-image lenses and reveal lenses with some sort of interesting structure.}, -author = {Keeton, Charles R. and Gaudi, B. Scott and Petters, A. O.}, -doi = {10.1086/497324}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Cosmology: Dark Matter,Cosmology: Gravitational Lensing,Cosmology: Large-Scale Structure of Universe,Cosmology: Theory,Galaxies: Formation}, -month = {nov}, -number = {1}, -pages = {35--59}, -title = {{Identifying Lenses with Small‐Scale Structure. II. Fold Lenses}}, -url = {http://iopscience.iop.org/0004-637X/635/1/35/fulltext/}, -volume = {635}, -year = {2005} -} -@article{Bundy2005, -abstract = {We present an analysis of the growth of stellar mass with cosmic time partitioned according to galaxy morphology. Using a well-defined catalog of 2150 galaxies based, in part, on archival data in the GOODS fields, we assign morphological types in three broad classes (Ellipticals, Spirals, Peculiar/Irregulars) to a limit of z_AB=22.5 and make the resulting catalog publicly available. We combine redshift information, optical photometry from the GOODS catalog and deep K-band imaging to assign stellar masses. We find little evolution in the form of the galaxy stellar mass function from z$\sim$1 to z=0, especially at the high mass end where our results are most robust. Although the population of massive galaxies is relatively well established at z$\sim$1, its morphological mix continues to change, with an increasing proportion of early-type galaxies at later times. By constructing type-dependent stellar mass functions, we show that in each of three redshift intervals, E/S0's dominate the higher mass population, while spirals are favored at lower masses. This transition occurs at a stellar mass of 2--3 times 10^{10} Msun at z$\sim$0.3 (similar to local studies) but there is evidence that the relevant mass scale moves to higher mass at earlier epochs. Such evolution may represent the morphological extension of the ``downsizing'' phenomenon, in which the most massive galaxies stop forming stars first, with lower mass galaxies becoming quiescent later. We infer that more massive galaxies evolve into spheroidal systems at earlier times, and that this morphological transformation may only be completed 1--2 Gyr after the galaxies emerge from their active star forming phase. We discuss several lines of evidence suggesting that merging may play a key role in generating this pattern of evolution.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502204}, -author = {Bundy, Kevin and Ellis, Richard S. and Conselice, Christopher J.}, -doi = {10.1086/429549}, -eprint = {0502204}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Formation,cosmology: observations,galaxies: evolution}, -month = {jun}, -number = {2}, -pages = {621--632}, -primaryClass = {astro-ph}, -title = {{The Mass Assembly Histories of Galaxies of Various Morphologies in the GOODS Fields}}, -url = {http://arxiv.org/abs/astro-ph/0502204%0Ahttp://dx.doi.org/10.1086/429549}, -volume = {625}, -year = {2005} -} -@article{Alexander2019, -abstract = {Dark matter substructure has the potential to discriminate between broad classes of dark matter models. With this in mind, we construct novel solutions to the equations of motion governing condensate dark matter candidates, namely axion Bose-Einstein condensates and superfluids. These solutions are highly compressed along one axis and thus have a disk-like geometry. We discuss linear stability of these solutions, consider the astrophysical implications as a large-scale dark disk or as small scale substructure, and find a characteristic signal in strong gravitational lensing. This adds to the growing body of work that indicates that the morphology of dark matter substructure is a powerful probe of the nature of dark matter.}, -archivePrefix = {arXiv}, -arxivId = {1901.03694}, -author = {Alexander, Stephon and Bramburger, Jason J and McDonough, Evan}, -doi = {10.1016/j.physletb.2019.134871}, -eprint = {1901.03694}, -issn = {03702693}, -journal = {Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics}, -pages = {1--7}, -title = {{Dark disk substructure and superfluid dark matter}}, -url = {http://arxiv.org/abs/1901.03694}, -volume = {797}, -year = {2019} -} -@article{2001eu, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{2001eu, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales (∼500 kpc) in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the virial radius of the haloes while describing the infalling matter via fluxes through a spherical shell; and we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP described for the first time in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one- and two-point statistics. The peripheral and advected momenta are correlated with the spin of the embedded halo at levels of 30 and 50 per cent. The infall takes place preferentially in the plane perpendicular to the direction defined by the spin of the halo. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be ∼15 per cent. The substructures have their spin orthogonal to their velocity vector in the rest frame of the halo at a level of about 5 per cent, suggestive of an image of a flow along filamentary structures, which provides an explanation for the measured anisotropy. Using a 'synthetic' stacked halo, it is shown that the positions and orientations of satellites relative to the direction of spin of the halo are not random even in projection. The average ellipticity of stacked haloes is 10 per cent, while the alignment excess in projection reaches 2 per cent. All measured correlations are fitted by a simple three-parameter model. We conclude that a halo does not see its environment as an Isotropic perturbation, we investigate how the anisotropy is propagated inwards using perturbation theory, and we discuss briefly the implications for weak lensing, warps and the thickness of galactic discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D and Pichon, C and Colombi, S}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Geometryeh, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Tinker2013, -abstract = {We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2, 1.0]. For massive galaxies, M ≳ 1010.6 M , our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M ∼ 1010 M , the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency. {\textcopyright}2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1308.2974}, -author = {Tinker, Jeremy L and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H}, -doi = {10.1088/0004-637X/778/2/93}, -eprint = {1308.2974}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: halos}, -number = {2}, -title = {{Evolution of the stellar-to-dark matter relation: Separating star-forming and passive galaxies from z = 1 to 0}}, -volume = {778}, -year = {2013} -} -@article{Moore2018, -abstract = {The next generation of giant-segmented mirror telescopes ({\textgreater}20 m) will enable us to observe galactic nuclei at much higher angular resolution and sensitivity than ever before. These capabilities will introduce a revolutionary shift in our understanding of the origin and evolution of supermassive black holes by enabling more precise black hole mass measurements in a mass range that is unreachable today. We present simulations and predictions of the observations of nuclei that will be made with the Thirty Meter Telescope (TMT) and the adaptive optics assisted integral-field spectrograph IRIS, which is capable of diffraction-limited spectroscopy from Z band (0.9 $\mu$m) to K band (2.2 $\mu$m). These simulations, for the first time, use realistic values for the sky, telescope, adaptive optics system, and instrument to determine the expected signal-to-noise ratio of a range of possible targets spanning intermediate mass black holes of 104 M⊙to the most massive black holes known today of {\textgreater}1010 M ⊙. We find that IRIS will be able to observe Milky Way mass black holes out the distance of the Virgo Cluster, and will allow us to observe many more of the brightest cluster galaxies where the most massive black holes are thought to reside. We also evaluate how well the kinematic moments of the velocity distributions can be constrained at the different spectral resolutions and plate scales designed for IRIS. We find that a spectral resolution of 8000 will be necessary to measure the masses of intermediate mass black holes. By simulating the observations of galaxies found in Sloan Digital Sky Survey DR7, we find that over 105 massive black holes will be observable at distances between 0.005 {\textless} z {\textless} 0.18 with the estimated sensitivity and angular resolution provided by access to Z-band (0.9 $\mu$m) spectroscopy from IRIS and the TMT adaptive optics system. These observations will provide the most accurate dynamical measurements of black hole masses to enable the study of the demography of massive black holes, address the origin of the M BH-$\sigma$ and M BH-L relationships, and evolution of black holes through cosmic time. {\textcopyright}2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1401.7988}, -author = {Do, Tuan and Wright, Shelley A and Barth, Aaron J and Barton, Elizabeth J and Simard, Luc and Larkin, James E and Moore, Anna M and Wang, Lianqi and Ellerbroek, Brent}, -doi = {10.1088/0004-6256/147/4/93}, -eprint = {1401.7988}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {adaptive opticsinstrumentation,galaxies,imaging spectroscopytelescopes,kinematics and dynamicsinstrumentation,spectrographstechniques}, -number = {4}, -pages = {1--19}, -title = {{Prospects for measuring supermassive black hole masses with future extremely large telescopes}}, -volume = {147}, -year = {2014} -} -@article{Talbot2018, -abstract = {We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for eight of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with two background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched $\sim$1.5 million spectra, of which 3065 contained multiple high signal-to-noise ratio background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius ≳ 1.7 arcsec, which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely.}, -archivePrefix = {arXiv}, -arxivId = {1803.03604}, -author = {Talbot, Michael S. and Brownstein, Joel R. and Bolton, Adam S. and Bundy, Kevin and Andrews, Brett H. and Cherinka, Brian and Collett, Thomas E. and More, Anupreeta and More, Surhud and Sonnenfeld, Alessandro and Vegetti, Simona and Wake, David A. and Weijmans, Anne Marie and Westfall, Kyle B.}, -doi = {10.1093/mnras/sty653}, -eprint = {1803.03604}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Talbot et al. - 2018 - SDSS-IV MaNGA The spectroscopic discovery of strongly lensed galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: General,Gravitational lensing: Strong}, -number = {1}, -pages = {195--209}, -title = {{SDSS-IV MaNGA: The spectroscopic discovery of strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1803.03604%0Ahttp://dx.doi.org/10.1093/mnras/sty653}, -volume = {477}, -year = {2018} -} -@techreport{VISReport2021, -author = {EUCL-MSS-TR-6-129}, -doi = {EUCL-MSS-TR-6-129}, -file = {:C\:/Users/Jammy/Documents/Papers/Euclid/Azzollini2021CIReport.pdf:pdf}, -title = {{VIS Ground Calibration Campaign: Test Report}}, -year = {2021} -} -@article{Ma2014, -abstract = {Massive early-type galaxies represent the modern day remnants of the earliest major star formation episodes in the history of the universe. These galaxies are central to our understanding of the evolution of cosmic structure, stellar populations, and supermassive black holes, but the details of their complex formation histories remain uncertain. To address this situation, we have initiated the MASSIVE Survey, a volume-limited, multi-wavelength, integral-field spectroscopic (IFS) and photometric survey of the structure and dynamics of the ∼100 most massive early-type galaxies within a distance of 108 Mpc. This survey probes a stellar mass range M∗ ≳ 1011.5 M⊙ and diverse galaxy environments that have not been systematically studied to date. Our wide-field IFS data cover about two effective radii of individual galaxies, and for a subset of them, we are acquiring additional IFS observations on sub-arcsecond scales with adaptive optics. We are also acquiring deep K-band imaging to trace the extended halos of the galaxies and measure accurate total magnitudes. Dynamical orbit modeling of the combined data will allow us to simultaneously determine the stellar, black hole, and dark matter halo masses. The primary goals of the project are to constrain the black hole scaling relations at high masses, investigate systematically the stellar initial mass function and dark matter distribution in massive galaxies, and probe the late-time assembly of ellipticals through stellar population and kinematical gradients. In this paper, we describe the MASSIVE sample selection, discuss the distinct demographics and structural and environmental properties of the selected galaxies, and provide an overview of our basic observational program, science goals and early survey results.}, -archivePrefix = {arXiv}, -arxivId = {1407.1054}, -author = {Ma, Chung Pei and Greene, Jenny E. and McConnell, Nicholas and Janish, Ryan and Blakeslee, John P. and Thomas, Jens and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/795/2/158}, -eprint = {1407.1054}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ma et al. - 2014 - The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies wi.pdf:pdf}, -isbn = {0000000000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: elliptical and lenticular, cD,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content,galaxies: structure}, -number = {2}, -pages = {158}, -pmid = {28562576}, -title = {{The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...795..158M}, -volume = {795}, -year = {2014} -} -@article{Pulsoni2017, -abstract = {Wolbachia is an intracellular endosymbiont that induces a variety of reproductive alterations in diverse arthropods. The almond moth, Cadra cautella, is double infected with two Wolbachia variants, wCauA and wCauB, and expresses complete cytoplasmic incompatibility (CI). The individual contribution of wCauA and wCauB to the expression of CI are unclear, however, because the two variants have not been separated in this host. The effect of wCauA is of particular interest because it induces male killing when transferred into the Mediterranean flour moth, Ephestia kuehniella. In the present study, we generated C. cautella infected with only wCauA by treating double-infected insects with tetracycline. Single-infected C. cautella exhibited strong CI, demonstrating that wCauA induces two distinct reproductive phenotypes in different hosts: CI in C. cautella and male killing in E. kuehniella. CI was also observed in the cross of double-infected males and single-infected females. Comparison of the single- and double-infected insects by real-time quantitative polymerase chain reaction suggested that the wCauA density is not affected much by the presence or absence of wCauB.}, -archivePrefix = {arXiv}, -arxivId = {http://www.R-project.org}, -author = {Sasaki, T and Massaki, N and Kubo, T}, -doi = {10.1038/sj.hdy.6800737}, -eprint = {/www.R-project.org}, -isbn = {0018-067X}, -issn = {0018067X}, -journal = {Heredity}, -keywords = {Cadra cautella,Cytoplasmic incompatibility,Double infection,Male killing,Real-time quantitative PCR,Wolbachia}, -number = {5}, -pages = {389--393}, -pmid = {16106260}, -primaryClass = {http:}, -title = {{Wolbachia variant that induces two distinct reproductive phenotypes in different hosts}}, -url = {http://arxiv.org/abs/1712.05833}, -volume = {95}, -year = {2005} -} -@article{Ferrero2017, -abstract = {The Tully-Fisher relation (TFR) links the stellar mass of a disc galaxy, Mstr, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling (M ∝ V3) of dark matter haloes, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to deviate substantially from a single power law and to evolve rapidly with redshift. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of $\Lambda$ cold dark matter ($\Lambda$CDM) cosmological simulations. Matching both relations requires disc sizes to satisfy constraints given by the concentration of haloes and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. $\Lambda$CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1607.03100}, -author = {Ferrero, Ismael and Navarro, Julio F. and Abadi, Mario G. and Sales, Laura V. and Bower, Richard G. and Crain, Robert A. and Frenk, Carlos S. and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw2691}, -eprint = {1607.03100}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ferrero et al. - 2017 - Size matters Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {4}, -pages = {4736--4746}, -title = {{Size matters: Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE}}, -volume = {464}, -year = {2017} -} -@article{Nightingale2023, -abstract = {Supermassive black holes (SMBHs) are a key catalyst of galaxy formation and evolution, leading to an observed correlation between SMBH mass MBH and host galaxy velocity dispersion $\sigma$e. Outside the local Universe, measurements of MBH are usually only possible for SMBHs in an active state: limiting sample size and introducing selection biases. Gravitational lensing makes it possible to measure the mass of non-active SMBHs. We present models of the z = 0.169 galaxy-scale strong lens Abell 1201. A cD galaxy in a galaxy cluster, it has sufficient ‘external shear' that a magnified image of a z = 0.451 background galaxy is projected just ∼1 kpc from the galaxy centre. Using multiband Hubble Space Telescope imaging and the lens modelling software PYAUTOLENS, we reconstruct the distribution of mass along this line of sight. Bayesian model comparison favours a point mass with MBH = 3.27 ± 2.12 × 1010 M⊙ (3$\sigma$ confidence limit); an ultramassive black hole. One model gives a comparable Bayesian evidence without an SMBH; however, we argue this model is nonphysical given its base assumptions. This model still provides an upper limit of MBH ≤ 5.3 × 1010 M⊙, because an SMBH above this mass deforms the lensed image ∼1 kpc from Abell 1201's centre. This builds on previous work using central images to place upper limits on MBH, but is the first to also place a lower limit and without a central image being observed. The success of this method suggests that surveys during the next decade could measure thousands more SMBH masses, and any redshift evolution of the MBH−$\sigma$e relation. Results are available at https://github.com/Jammy2211/autolens_abell_1201.}, -author = {Nightingale, J W and Smith, Russell J and He, Qiuhan and Riordan, Conor M O and Kegerreis, Jacob A and Amvrosiadis, Aristeidis and Edge, Alastair C and Etherington, Amy and Hayes, Richard G and Kelly, Ash and Lucey, John R and Massey, Richard J}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Nightingale2023SMBH.pdf:pdf}, -journal = {MNRAS}, -keywords = {2004,and reverberation,dunlop 2004,evolution,formation,galactic nuclei,galaxies,gravitational lensing,how these relations evolve,mclure,nearby galaxies,peterson et al,preventing the study of,quasars,shen 2013,spectral fitting of active,strong,supermassive black holes,with redshift}, -number = {3}, -pages = {3298--3322}, -title = {{Abell 1201 : detection of an ultramassi v e black hole in a strong gravitational lens 1 I N T RO D U C T I O N}}, -volume = {521}, -year = {2023} -} -@article{Pontzen2012, -abstract = {We propose and successfully test against new cosmological simulations a novel analytical description of the physical processes associated with the origin of cored dark matter density profiles. In the simulations, the potential in the central kiloparsec changes on sub-dynamical time-scales over the redshift interval 4 > z > 2, as repeated, energetic feedback generates large underdense bubbles of expanding gas from centrally concentrated bursts of star formation. The model demonstrates how fluctuations in the central potential irreversibly transfer energy into collisionless particles, thus generating a dark matter core. A supply of gas undergoing collapse and rapid expansion is therefore the essential ingredient. The framework, based on a novel impulsive approximation, breaks with the reliance on adiabatic approximations which are inappropriate in the rapidly changing limit. It shows that both outflows and galactic fountains can give rise to cusp flattening, even when only a few per cent of the baryons form stars. Dwarf galaxies maintain their core to the present time. The model suggests that constant density dark matter cores will be generated in systems of a wide mass range if central starbursts or active galactic nucleus phases are sufficiently frequent and energetic. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1106.0499}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1111/j.1365-2966.2012.20571.x}, -eprint = {1106.0499}, -isbn = {doi:10.1111/j.1365-2966.2012.20571.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: dwarf}, -month = {apr}, -number = {4}, -pages = {3464--3471}, -title = {{How supernova feedback turns dark matter cusps into cores}}, -volume = {421}, -year = {2012} -} -@article{Bentabol2016, -abstract = {We examine a sample of 1495 galaxies in the CANDELS fields to determine the evolution of two-component galaxies, including bulges and discs, within massive galaxies at the epoch 1 < z <3 when the Hubble sequence forms. We fit all of our galaxies' light profiles with a single S{\'{e}}rsic fit, as well as with a combination of exponential and S{\'{e}}rsic profiles. The latter is done in order to describe a galaxy with an inner and an outer component, or bulge and disc component. We develop and use three classification methods (visual, F-test and the residual flux fraction) to separate our sample into one-component galaxies (disc/spheroidslike galaxies) and two-component galaxies (galaxies formed by an 'inner part' or bulge and an 'outer part' or disc). We then compare the results from using these three different ways to classify our galaxies.We find that the fraction of galaxies selected as two-component galaxies increases on average 50 per cent from the lowest mass bin to the most massive galaxies, and decreases with redshift by a factor of 4 from z = 1 to 3. We find that single S{\'{e}}rsic 'disc-like' galaxies have the highest relative number densities at all redshifts, and that two-component galaxies have the greatest increase and become at par with S{\'{e}}rsic discs by z = 1. We also find that the systems we classify as two-component galaxies have an increase in the sizes of their outer components, or 'discs', by about a factor of 3 from z = 3 to 1.5, while the inner components or 'bulges' stay roughly the same size. This suggests that these systems are growing from the inside out, whilst the bulges or protobulges are in place early in the history of these galaxies. This is also seen to a lesser degree in the growth of single 'disc-like' galaxies versus 'spheroid-like' galaxies over the same epoch.}, -archivePrefix = {arXiv}, -arxivId = {1606.07405}, -author = {Margalef-Bentabol, Berta and Conselice, Christopher J. and Mortlock, Alice and Hartley, Will and Duncan, Kenneth and Ferguson, Harry C. and Dekel, Avishai and Primack, Joel R.}, -doi = {10.1093/mnras/stw1451}, -eprint = {1606.07405}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Margalef-Bentabol et al. - 2016 - The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z 3(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure}, -number = {3}, -pages = {1--21}, -title = {{The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z < 3}}, -volume = {461}, -year = {2016} -} -@article{Cautun2015, -abstract = {The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model ({\$}\backslashLambda{\$}CDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of the MW and M31 planes in {\$}\backslashLambda{\$}CDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high resolution cosmological simulations. We find that planar structures are very common, and that {\$\sim${}}10{\%} of {\$}\backslashLambda{\$}CDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and {\$}\backslashLambda{\$}CDM predictions. In fact, {\$\sim${}}10{\%} of {\$}\backslashLambda{\$}CDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1506.04151}, -author = {Cautun, Marius and Bose, Sownak and Frenk, Carlos S and Guo, Qi and Han, Jiaxin and Hellwing, Wojciech A and Sawala, Till and Wang, Wenting}, -doi = {10.1093/mnras/stv1557}, -eprint = {1506.04151}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {4}, -pages = {3838--3852}, -title = {{Planes of satellite galaxies: When exceptions are the rule}}, -volume = {452}, -year = {2015} -} -@article{Jaroszynski2012, -abstract = {We investigate strong lensing by non-singular finite isothermal ellipsoids taking into account the influence of the matter along the line of sight and in the close lens vicinity. We compare three descriptions of light propagation: the full approach taking into account all matter inhomogeneities along the rays, the single plane approach, where we take into account the influence of the strong lens neighbours but neglect the foreground and background objects, and the single lens approach. In each case we simulate many strong lensing configurations placing a point source at the same redshift but in different locations inside the region surrounded by caustics. We further analyze configurations of four or five images. For every simulated strong lensing configuration we attempt to fit a simplified lens model using a single isothermal ellipsoid or a single isothermal ellipsoid with external shear. The single lens fits to configurations obtained in the full approach are rejected in majority of cases with 95{\%} significance. For configurations obtained in the single plane approach the rejection rate is substantially lower. Also the inclusion of external shear in simplified modeling improves the chances of obtaining acceptable fits, but the problem is not solved completely. The quantitative estimates of the rates of rejection of simplified models depend on the required accuracy of the models, and we present few illustrative examples, which show that both matter close to the lens and matter along the rays do have important influence on lens modeling. We also estimate the typical value of the external shear and compare the fitted parameters of the simplified models with the parameters of the lenses used in the simulations.}, -archivePrefix = {arXiv}, -arxivId = {1204.6223}, -author = {Jaroszynski, M and Kostrzewa-Rutkowska, Z}, -doi = {10.1111/j.1365-2966.2012.21197.x}, -eprint = {1204.6223}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: strong,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {1}, -pages = {325--332}, -title = {{Background, foreground and nearby matter influence on strong gravitational lenses}}, -volume = {424}, -year = {2012} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyse sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in 255 deg2 of the Kilo Degree Survey (KiDS), one of the currentgeneration optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii ≳1.4 arcsec, about twice the r-band seeing in KiDS. In a sample of 21 789 colour-magnitude selected luminous red galaxies (LRGs), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find $\sim$100 massive LRGgalaxy lenses at z ≲ 0.4 in KiDS when completed. In the most optimistic scenario, this number can grow considerably (to maximally $\sim$2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C. E. and Tortora, C. and Chatterjee, S. and Vernardos, G. and Koopmans, L. V.E. and Kleijn, G. Verdoes and Napolitano, N. R. and Covone, G. and Schneider, P. and Grado, A. and McFarland, J.}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Petrillo et al. - 2017 - Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{Kennicutt, -archivePrefix = {arXiv}, -arxivId = {arXiv:1204.3552v2}, -author = {Kennicutt, Robert C}, -eprint = {arXiv:1204.3552v2}, -title = {{Star formation in the milky way and nearby galaxies}}, -volume = {50} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and discs are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disc components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to Calar Alto Integral Field Area integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux, they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P. and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tabor et al. - 2017 - Untangling galaxy components Full spectral bulge-disc decomposition.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Dynamics,Galaxies: elliptical and lenticular,Galaxies: kinematics}, -number = {2}, -pages = {2024--2033}, -title = {{Untangling galaxy components: Full spectral bulge-disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {466}, -year = {2017} -} -@article{Ellison2017, -abstract = {The tight correlation between total galaxy stellar mass and star formation rate (SFR) has become known as the star-forming main sequence. Using {\$\sim${}}487 000 spaxels from galaxies observed as part of the Sloan Digital Sky Survey Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, we confirm previous results that a correlation also exists between the surface densities of star formation ($\Sigma$SFR) and stellar mass ($\Sigma$*) on kpc scales, representing a 'resolved' main sequence. Using a new metric ($\Delta$$\Sigma$SFR), which measures the relative enhancement or deficit of star formation on a spaxel-by-spaxel basis relative to the resolved main sequence, we investigate the SFR profiles of 864 galaxies as a function of their position relative to the global star-forming main sequence ($\Delta$SFR). For galaxies above the global main sequence (positive $\Delta$SFR) $\Delta$$\Sigma$SFR is elevated throughout the galaxy, but the greatest enhancement in star formation occurs at small radii ({\textless} 3 kpc, or 0.5Re). Moreover, galaxies that are at least a factor of 3 above the main sequence show diluted gas phase metallicities out to 2Re, indicative of metal-poor gas inflows accompanying the starbursts. For quiescent/passive galaxies that lie at least a factor of 10 below the star-forming main sequence, there is an analogous deficit of star formation throughout the galaxy with the lowest values of $\Delta$$\Sigma$SFR in the central 3 kpc. Our results are in qualitative agreement with the 'compaction' scenario in which a central starburst leads to mass growth in the bulge and may ultimately precede galactic quenching from the inside-out.}, -archivePrefix = {arXiv}, -arxivId = {1711.00915}, -author = {Ellison, Sara L and S{\'{a}}nchez, Sebastian F and Ibarra-Medel, Hector and Antonio, Braulio and Mendel, J Trevor and Barrera-Ballesteros, Jorge}, -doi = {10.1093/mnras/stx2882}, -eprint = {1711.00915}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: interactions,Galaxies: star formation}, -number = {2}, -pages = {2039--2054}, -title = {{Star formation is boosted (and quenched) from the inside-out: Radial star formation profiles from MaNGA}}, -url = {http://arxiv.org/abs/1711.00915}, -volume = {474}, -year = {2018} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}$\backslash${\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashsigma{\$} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and Gonzalez, Pablo G Perez and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -title = {{CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z{\$\sim${}}2}}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -year = {2017} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print){\$}\backslash{\$}r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Huang2018, -abstract = {We use {\$\sim${}}100 square deg of deep ({\textgreater}28.5 mag arcsec{\$}{\^{}}{\{}-2{\}}{\$} in i-band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach {\$\sim${}}4 magnitudes deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with {\$}\backslashlog M{\_}{\{}\backslashstar, 100\backslash \backslashmathrm{\{}kpc{\}}{\}}{\textgreater}11.6{\$} in more massive haloes at 0.3 {\textless} z {\textless} 0.5 have shallower inner stellar mass density profiles (within {\$\sim${}}10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with {\$}\backslashlog M{\_}{\{}\backslashrm{\{}Halo{\}}{\}}{\textgreater}14.0{\$} are {\$\sim${}}20{\%} larger in {\$}R{\_}{\{}\backslashmathrm{\{}50{\}}{\}}{\$} at fixed stellar mass. Such dependence is also reflected in the relationship between the stellar mass within 10 and 100 kpc. Comparing to the mass--size relation, the {\$}\backslashlog M{\_}{\{}\backslashstar, 100\backslash \backslashrm{\{}kpc{\}}{\}}{\$}-{\$}\backslashlog M{\_}{\{}\backslashstar, 10\backslash \backslashrm{\{}kpc{\}}{\}}{\$} relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kremer et al. - 2017 - Big Universe, Big Data Machine Learning and Image Analysis for Astronomy.pdf:pdf}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z ∼ 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u - g color profiles for these galaxies and show that most z ∼ 2galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z ∼ 2galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: ($\Delta$(u - g rest)/$\Delta$(log r))median = -0.47, -0.33, and -0.46 for z ∼ 2, z ∼ 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z ∼ 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u - g colors, and lower S{\'{e}}rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch. {\textcopyright}2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J and {Van Dokkum}, Pieter G and Labb{\'{e}}, Ivo and Illingworth, Garth D and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from $\sim$1011 to > 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above $\sim$1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K.}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/K{\"{u}}ng et al. - 2018 - Models of gravitational lens candidates from SpaceWarps CFHTLS(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Harrington2016, -abstract = {We present 8.5 arcsec resolution 1.1-mm continuum imaging and CO spectroscopic redshift measurements of eight extremely bright submillimetre galaxies identified from the Planck and Herschel surveys, taken with the Large Millimeter Telescope's AzTEC and Redshift Search Receiver instruments. We compiled a candidate list of high-redshift galaxies by cross-correlating the Planck Surveyor mission's highest frequency channel (857 GHz, full width at half-maximum = 4.5 arcmin) with the archival Herschel Spectral and Photometric Imaging Receiver imaging data, and requiring the presence of a unique, single Herschel counterpart within the 150-arcsec search radius of the Planck source positions with 350-$\mu$m flux density larger than 100 mJy, excluding known blazars and foreground galaxies. All eight candidate objects observed are detected in 1.1 mm continuum by AzTEC bolometer camera, and at least one CO line is detected in all cases with a spectroscopic redshift between 1.3 < zCO < 3.3. Their infrared (IR) spectral energy distributions (SEDs) mapped using the Herschel and AzTEC photometry are consistent with cold dust emission with characteristic temperature between Td = 43 and 84 K. With apparent IR luminosity of up to LIR = 3 × 1014$\mu$-1L⊙, they are some of the most luminous galaxies ever found (with yet unknown gravitational magnification factor $\mu$). The analysis of their SEDs suggests that star formation is powering the bulk of their extremely large IR luminosities. Derived molecular gas masses of MH2 = (0.6-7.8) × 1011 M⊙ (for $\mu$ ≈ 10) also make them some of the most gas-rich high-redshift galaxies ever detected.}, -archivePrefix = {arXiv}, -arxivId = {1603.05622}, -author = {Harrington, K. C. and Yun, Min S. and Cybulski, R. and Wilson, G. W. and Aretxaga, I. and Chavez, M. and {De la Luz}, V. and Erickson, N. and Ferrusca, D. and Gallup, A. D. and Hughes, D. H. and Monta{\~{n}}a, A. and Narayanan, G. and S{\'{a}}nchez-Arg{\"{u}}elles, D. and Schloerb, F. P. and Souccar, K. and Terlevich, E. and Terlevich, R. and Zeballos, M. and Zavala, J. A.}, -doi = {10.1093/mnras/stw614}, -eprint = {1603.05622}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Harrington2016PlanckSLSources.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: High-redshift,Galaxies: ISM,Galaxies: Starburst,Gravitational lensing: Strong,Infrared: Galaxies,Submillimetre: Galaxies}, -number = {4}, -pages = {4383--4399}, -title = {{Early science with the Large Millimeter Telescope: Observations of extremely luminous high-z sources identified by Planck}}, -volume = {458}, -year = {2016} -} -@article{Zavala2010, -abstract = {If dark matter is composed of neutralinos, one of the most exciting prospects for its detection lies in observations of the gamma-ray radiation created in pair annihilations between neutralinos, a process that may contribute significantly to the extragalactic gamma-ray background (EGB) radiation. We here use the high-resolution Millennium-II simulation of cosmic structure formation to produce the first full sky maps of the expected radiation coming from extragalactic dark matter structures. Our map-making procedure takes into account the total gamma-ray luminosity from all haloes and their subhaloes, and includes corrections for unresolved components of the emission as well as an extrapolation to the damping scale limit of neutralinos. Our analysis also includes a proper normalization of the signal according to a specific supersymmetric model based on minimal supergravity. The new simulated maps allow a study of the angular power spectrum of the gamma-ray background from dark matter annihilation, which has distinctive features associated with the nature of the annihilation process and may be detectable in forthcoming observations by the recently launched Fermi satellite. Our results are in broad agreement with analytic models for the gamma-ray background, but they also include higher order correlations not readily accessible in analytic calculations and, in addition, provide detailed spectral information for each pixel. In particular, we find that difference maps at different energies can reveal cosmic large-scale structure at low and intermediate redshifts. If the intrinsic emission spectrum is characterized by an emission peak, cosmological tomography with gamma-ray annihilation radiation is in principle possible. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0908.2428}, -author = {Zavala, Jes{\'{u}}s and Springel, Volker and Boylan-Kolchin, Michael}, -doi = {10.1111/j.1365-2966.2010.16482.x}, -eprint = {0908.2428}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Methods: numerical}, -number = {1}, -pages = {593--612}, -title = {{Extragalactic gamma-ray background radiation from dark matter annihilation}}, -volume = {405}, -year = {2010} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for {\$\sim${}}20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Czoske2012, -abstract = {This paper presents the full Very Large Telescope (VLT)/VIMOS-IFU data set and related data products from an ESO Large Programme with the observational goal of obtaining two-dimensional kinematic data of early-type lens galaxies, out to one effective radius. The sample consists of 17 early-type galaxies (ETGs) selected from the SLACS gravitational-lens survey. The galaxies cover the redshift range from 0.08 to 0.35 and have stellar velocity dispersions between 200 and 350 kms-1. This programme is complemented by a similar observational programme on Keck, using long-slit spectroscopy. In combination with multi-band imaging data, the kinematic data provide stringent constraints on the inner mass profiles of ETGs beyond the local Universe. Our Large Programme thus extends studies of nearby ETGs (e.g. SAURON/ATLAS3D) by an order of magnitude in distance and towards higher masses. We provide an overview of our observational strategy, the data products (luminosity-weighted spectra andHubble Space Telescopeimages) and derived products (i.e. two-dimensional fields of velocity dispersions and streaming motions) that have been used in a number of published and forthcoming lensing, kinematic and stellar-population studies. These studies also pave the way for future studies of ETGs atz≈ 1 with the upcoming extremely large telescopes. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1108.0577}, -author = {Czoske, Oliver and Barnab{\`{e}}, Matteo and Koopmans, L{\'{e}}on V.E. and Treu, Tommaso and Bolton, Adam S.}, -doi = {10.1111/j.1365-2966.2011.19726.x}, -eprint = {1108.0577}, -isbn = {00358711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: kinematics and dynamics,Galaxies: structure,Gravitational lensing: strong,Techniques: spectroscopic}, -number = {1}, -pages = {656--668}, -title = {{Two-dimensional kinematics of SLACS lenses - IV. The complete VLT-VIMOS data set}}, -volume = {419}, -year = {2012} -} -@article{Tenneti2016, -abstract = {We study the shapes and intrinsic alignments of discs and elliptical galaxies in the MassiveBlack-II (MBII) and Illustris cosmological hydrodynamic simulations, with volumes of (100 h-1 Mpc)3and (75 h-1 Mpc)3, respectively. We find that simulated disc galaxies are more oblate in shape and more misaligned with the shape of their host dark matter subhalo when compared with ellipticals. The discmajor axis is found to be oriented towards the location of nearby elliptical galaxies. We also find that the discs are thinner in MBII and misalignments with dark matter halo orientations are smaller in both discs and ellipticals when compared with Illustris. As a result, the intrinsic alignment correlation functions at fixed mass have a higher amplitude in MBII than in Illustris. Finally, at scales above $\sim$0.1 h-1 Mpc, the intrinsic alignment two-point correlation functions for disc galaxies in both simulations are consistent with a null detection, unlike those for ellipticals. Despite significant differences in the treatments of hydrodynamics and baryonic physics in the simulations, we find that the w$\delta$ + correlation function scales similarly with transverse separation. However, the less massive galaxies show different scale dependence in the ellipticity-direction correlation. This result indicates that, while hydrodynamic simulations are a promising tool to study intrinsic alignments, further study is needed to understand the impact of differences in the implementations of hydrodynamics and baryonic feedback.}, -archivePrefix = {arXiv}, -arxivId = {1510.07024}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana}, -doi = {10.1093/mnras/stw1823}, -eprint = {1510.07024}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tenneti, Mandelbaum, Di Matteo - 2016 - Intrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris sim(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies,Gravitational lensing: weak,Hydrodynamics,Kinematics and dynamics,Methods,Numerical}, -number = {3}, -pages = {2668--2680}, -title = {{Intrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris simulations}}, -volume = {462}, -year = {2016} -} -@article{Carpenter2017, -abstract = {Stan is a probabilistic programming language for specifying statistical models. A Stan program imperatively defines a log probability function over parameters conditioned on specified data and constants. As of version 2.14.0, Stan provides full Bayesian inference for continuous-variable models through Markov chain Monte Carlo methods such as the No-U-Turn sampler, an adaptive form of Hamiltonian Monte Carlo sampling. Penalized maximum likelihood estimates are calculated using optimization methods such as the limited memory Broyden-Fletcher-Goldfarb-Shanno algorithm. Stan is also a platform for computing log densities and their gradients and Hessians, which can be used in alternative algorithms such as variational Bayes, expectation propagation, and marginal inference using approximate integration. To this end, Stan is set up so that the densities, gradients, and Hessians, along with intermediate quantities of the algorithm such as acceptance probabilities, are easily accessible. Stan can be called from the command line using the cmdstan package, through R using the rstan package, and through Python using the pystan package. All three interfaces support sampling and optimization-based inference with diagnostics and posterior analysis. rstan and pystan also provide access to log probabilities, gradients, Hessians, parameter transforms, and specialized plotting.}, -author = {Carpenter, Bob and Gelman, Andrew and Hoffman, Matthew D and Lee, Daniel and Goodrich, Ben and Betancourt, Michael and Brubaker, Marcus A and Guo, Jiqiang and Li, Peter and Riddell, Allen}, -doi = {10.18637/jss.v076.i01}, -issn = {15487660}, -journal = {Journal of Statistical Software}, -keywords = {Algorithmic differentiation,Bayesian inference,Probabilistic program,Stan}, -number = {1}, -title = {{Stan: A probabilistic programming language}}, -volume = {76}, -year = {2017} -} -@article{Clark2015, -abstract = {We present the properties of the first 250 $\mu$m blind sample of nearby galaxies (15 < D < 46 Mpc) containing 42 objects from the Herschel Astrophysical Terahertz Large Area Survey. Herschel's sensitivity probes the faint end of the dust luminosity function for the first time, spanning a range of stellar mass (7.4 < M*< 11.3 log10M⊙), star formation activity (-11.8 < SSFR < -8.9 log10 yr-1), gas fraction (3-96 per cent), and colour (0.6 < FUV-KS < 7.0 mag). The median cold dust temperature is 14.6 K, colder than in the Herschel Reference Survey (18.5 K) and Planck Early Release Compact Source Catalogue (17.7 K). The mean dust-to-stellar mass ratio in our sample is higher than these surveys by factors of 3.7 and 1.8, with a dust mass volume density of (3.7 ± 0.7) × 105M⊙Mpc-3. Counter-intuitively, we find that the more dust rich a galaxy, the lower its UV attenuation. Over half of our dust-selected sample are very blue in FUV-KScolour, with irregular and/or highly flocculent morphology; these galaxies account for only 6 per cent of the sample's stellar mass but contain over 35 per cent of the dust mass. They are the most actively star-forming galaxies in the sample, with the highest gas fractions and lowest UV attenuation. They also appear to be in an early stage of converting their gas into stars, providing valuable insights into the chemical evolution of young galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1502.03843}, -author = {Clark, C. J.R. and Dunne, L. and Gomez, H. L. and Maddox, S. and {De Vis}, P. and Smith, M. W.L. and Eales, S. A. and Baes, M. and Bendo, G. J. and Bourne, N. and Driver, S. P. and Dye, S. and Furlanetto, C. and Grootes, M. W. and Ivison, R. J. and Schofield, S. P. and Robotham, A. S.G. and Rowlands, K. and Valiante, E. and Vlahakis, C. and van der Werf, P. and Wright, A. H. and De zotti, G.}, -doi = {10.1093/mnras/stv1276}, -eprint = {1502.03843}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: general,Galaxies: irregular,Infrared: galaxies,Submillimetre: galaxies}, -number = {1}, -pages = {397--430}, -title = {{Herschel-ATLAS: The surprising diversity of dust-selected galaxies in the local submillimetre Universe}}, -volume = {452}, -year = {2015} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M{\textless}inf{\textgreater}*{\textless}/inf{\textgreater} {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M{\textless}inf{\textgreater}⊙{\textless}/inf{\textgreater} galaxies at 1 {\textless} z {\textless} 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 {\textless} z {\textless} 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{Talbot2018, -abstract = {We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for eight of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with two background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched {\$\sim${}}1.5 million spectra, of which 3065 contained multiple high signal-to-noise ratio background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius ≳ 1.7 arcsec, which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely.}, -archivePrefix = {arXiv}, -arxivId = {1803.03604}, -author = {Talbot, Michael S and Brownstein, Joel R and Bolton, Adam S and Bundy, Kevin and Andrews, Brett H and Cherinka, Brian and Collett, Thomas E and More, Anupreeta and More, Surhud and Sonnenfeld, Alessandro and Vegetti, Simona and Wake, David A and Weijmans, Anne Marie and Westfall, Kyle B}, -doi = {10.1093/mnras/sty653}, -eprint = {1803.03604}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: General,Gravitational lensing: Strong}, -number = {1}, -pages = {195--209}, -title = {{SDSS-IV MaNGA: The spectroscopic discovery of strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1803.03604%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty653}, -volume = {477}, -year = {2018} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of {\$\sim${}}3692 galaxies, with -18.5 {\textless}= M{\_}g {\textless}-22.0 mag and redshift 0.01 {\textless}= z {\textless}0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of {\$\sim${}}2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined ({\textgreater}60 degrees) systems, we find the following results. (1) The optical r-band fraction (f{\_}opt-r) of barred galaxies is {\$\sim${}}48{\%}-52{\%}. (2) When galaxies are separated according to normalized half light radius (r{\_}e/R{\_}24), a remarkable result is seen: f{\_}opt-r rises sharply, from {\$\sim${}}40{\%} in galaxies that have small r{\_}e/R{\_}24 and visually appear to host prominent bulges, to {\$\sim${}}70{\%} for galaxies that have large r{\_}e/R{\_}24 and appear disk-dominated. (3) f{\_}opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that {\$\sim${}}20{\%} of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity {\textgreater}=0.4) and large enough (semi-major axis {\textgreater}=1.5 kpc) to be reliably characterized via ellipse-fitting out to z{\$\sim${}}0.8, we get an optical r-band fraction for strong bars f{\_}opt-s of {\$\sim${}}34{\%}. This value is higher only by a modest factor of 1.4, compared to the value of {\$\sim${}}24{\%}+-4{\%} reported at z{\$\sim${}}0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z{\$\sim${}}0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Barazza, Fabio D and Jogee, Shardha and Marinova, Irina}, -doi = {10.1179/sre.1993.32.248.122}, -eprint = {0802.3961}, -issn = {17522706}, -journal = {ArXiv e-prints}, -keywords = {Astrophysics}, -pages = {3961}, -title = {{Bars in Local Galaxies: Evidence for a higher Optical Bar Fraction in Disk-Dominated Galaxies}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {0802}, -year = {2008} -} -@article{Lin2013, -abstract = {The details of the stellar mass assembly of brightest cluster galaxies (BCGs) remain an unresolved problem in galaxy formation. We have developed a novel approach that allows us to construct a sample of clusters that form an evolutionary sequence, and have applied it to the Spitzer IRAC Shallow Cluster Survey (ISCS) to examine the evolution of BCGs in progenitors of present-day clusters with mass of (2.5-4.5) × 1014 M⊙. We follow the cluster mass growth history extracted from a high resolution cosmological simulation, and then use an empirical method that infers the cluster mass based on the ranking of cluster luminosity to select high-z clusters of appropriate mass from ISCS to be progenitors of the given set of z = 0 clusters. We find that, between z = 1.5 and 0.5, the BCGs have grown in stellar mass by a factor of 2.3, which is well-matched by the predictions from a state-of-the-art semi-analytic model. Below z = 0.5 we see hints of differences in behavior between the model and observation. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1305.5254}, -author = {Lin, Yen Ting and Brodwin, Mark and Gonzalez, Anthony H. and Bode, Paul and Eisenhardt, Peter R.M. and Stanford, S. A. and Vikhlinin, Alexey}, -doi = {10.1088/0004-637X/771/1/61}, -eprint = {1305.5254}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: clusters: general,galaxies: elliptical and lenticular, cD,galaxies: evolution,galaxies: luminosity function, mass function}, -number = {1}, -pages = {61}, -title = {{The stellar mass growth of brightest cluster galaxies in the IRAC shallow cluster survey}}, -url = {http://stacks.iop.org/0004-637X/771/i=1/a=61?key=crossref.37eb28ce31a672162ad2f02dfef54c8b}, -volume = {771}, -year = {2013} -} -@article{Geometryei, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(11).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Cole2000, -abstract = {We describe the GALFORM semi-analytic model for calculating the formation and evolution of galaxies in hierarchical models. It improves upon, and extends, the Cole et al 1994 model. The model employs a new Monte-Carlo algorithm to follow the merging evolution of dark matter halos with arbitrary mass resolution. It incorporates realistic descriptions of the density profiles of dark matter halos and their gas content; follows the chemical evolution of gas and stars, and the associated production of dust; and includes a detailed calculation of the sizes of disks and spheroids. Wherever possible, our prescriptions for modelling individual physical processes are based on results of numerical simulations. We apply our methods to the LCDM cosmology (Omega{\_}0=0.3, Lambda{\_}0=0.7), and find good agreement with a wide range of properties of the local galaxy population: the B-band and K-band luminosity functions, the distribution of colours for the population as a whole, the ratio of ellipticals to spirals, the distribution of disk sizes, and the current cold gas content of disks. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0007281}, -author = {Cole, Shaun and Lacey, Cedric G and Baugh, Carlton M and Frenk, Carlos S}, -doi = {10.1046/j.1365-8711.2000.03879.x}, -eprint = {0007281}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {formation,galaxies}, -number = {1}, -pages = {168--204}, -primaryClass = {astro-ph}, -title = {{Hierarchical galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0007281%7B%5C%25%7D0Ahttp://dx.doi.org/10.1046/j.1365-8711.2000.03879.x}, -volume = {319}, -year = {2002} -} -@article{Baudis2017, -abstract = {The dark matter problem is almost a century old. Since the 1930s evidence has been growing that our cosmos is dominated by a new form of non-baryonic matter that holds galaxies and clusters together and influences cosmic structures up to the largest observed scales. At the microscopic level, we still do not know the composition of this dark, or invisible, matter, which does not interact directly with light. The simplest assumption is that it is made of new particles that interact with gravity and, at most, weakly with known elementary particles. I will discuss searches for such new particles, both space- and Earth-bound, including those experiments placed in deep underground laboratories. While a dark matter particle has not yet been identified, even after decades of concerted efforts, new technological developments and experiments have reached sensitivities where a discovery might be imminent, albeit certainly not guaranteed.}, -archivePrefix = {arXiv}, -arxivId = {1801.08128}, -author = {Baudis, Laura}, -doi = {10.1017/S1062798717000783}, -eprint = {1801.08128}, -issn = {14740575}, -journal = {European Review}, -pages = {1--12}, -title = {{The Search for Dark Matter}}, -year = {2017} -} -@article{Hopkins2011, -abstract = {We present analytic calculations of angular momentum transport and gas inflow in galaxies, from scales of {\$\sim${}}kpc to deep inside the potential of a central massive black hole (BH). We compare these analytic calculations to numerical simulations and use them to develop a sub-grid model of BH growth that can be incorporated into semi-analytic calculations or cosmological simulations. Motivated by both analytic calculations and simulations of gas inflow in galactic nuclei, we argue that the strongest torque on gas arises when non-axisymmetric perturbations to the stellar gravitational potential produce orbit crossings and shocks in the gas. This is true both at large radii {\$\sim${}}0.01-1kpc, where bar-like stellar modes dominate the non-axisymmetric potential, and at smaller radii ≲10pc, where a lopsided/eccentric stellar disc dominates. The traditional orbit-crossing criterion is not always adequate to predict the locations of, and inflow due to, shocks in gas+stellar discs with finite sound speeds. We derive a modified criterion that predicts the presence of shocks in stellar-dominated systems even absent formal orbit crossing. We then derive analytic expressions for the loss of angular momentum and the resulting gas inflow rates in the presence of such shocks. We test our analytic predictions using hydrodynamic simulations at a range of galactic scales, and show that they successfully predict the mass inflow rates and quasi-steady gas surface densities with a small scatter ≃0.3dex. We use our analytic results to construct a new estimate of the BH accretion rate given galaxy properties at larger radii, for use in galaxy and cosmological simulations and semi-analytic models. While highly simplified, this accretion rate predictor captures the key scalings in the numerical simulations. By contrast, alternate estimates such as the local viscous accretion rate or the spherical Bondi rate fail systematically to reproduce the simulations and have significantly larger scatter. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1007.2647}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1365-2966.2011.18542.x}, -eprint = {1007.2647}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Quasars: general}, -number = {2}, -pages = {1027--1050}, -title = {{An analytic model of angular momentum transport by gravitational torques: From galaxies to massive black holes}}, -volume = {415}, -year = {2011} -} -@article{Dawson2013, -abstract = {The Baryon Oscillation Spectroscopic Survey (BOSS) is designed to measure the scale of baryon acoustic oscillations (BAO) in the clustering of matter over a larger volume than the combined efforts of all previous spectroscopic surveys of large-scale structure. BOSS uses 1.5 million luminous galaxies as faint as i = 19.9 over 10,000deg2 to measure BAO to redshifts z < 0.7. Observations of neutral hydrogen in the Ly$\alpha$ forest in more than 150,000quasar spectra (g < 22) will constrain BAO over the redshift range 2.15 < z < 3.5. Early results from BOSS include the first detection of the large-scale three-dimensional clustering of the Ly$\alpha$ forest and a strong detection from the Data Release 9 data set of the BAO in the clustering of massive galaxies at an effective redshift z = 0.57. We project that BOSS will yield measurements of the angular diameter distance dA to an accuracy of 1.0% at redshifts z = 0.3 and z = 0.57 and measurements of H(z) to 1.8% and 1.7% at the same redshifts. Forecasts for Ly$\alpha$ forest constraints predict a measurement of an overall dilation factor that scales the highly degenerate DA (z) and H -1(z) parameters to an accuracy of 1.9% at z ∼ 2.5 when the survey is complete. Here, we provide an overview of the selection of spectroscopic targets, planning of observations, and analysis of data and data quality of BOSS. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1208.0022}, -author = {Dawson, Kyle S. and Schlegel, David J. and Ahn, Christopher P. and Anderson, Scott F. and Aubourg, {\'{E}}ric and Bailey, Stephen and Barkhouser, Robert H. and Bautista, Julian E. and Beifiori, Alessandra and Berlind, Andreas A. and Bhardwaj, Vaishali and Bizyaev, Dmitry and Blake, Cullen H. and Blanton, Michael R. and Blomqvist, Michael and Bolton, Adam S. and Borde, Arnaud and Bovy, Jo and Brandt, W. N. and Brewington, Howard and Brinkmann, Jon and Brown, Peter J. and Brownstein, Joel R. and Bundy, Kevin and Busca, N. G. and Carithers, William and Carnero, Aurelio R. and Carr, Michael A. and Chen, Yanmei and Comparat, Johan and Connolly, Natalia and Cope, Frances and Croft, Rupert A.C. and Cuesta, Antonioj and Dacosta, Luizn and Davenport, James R.A. and Delubac, Timoth{\'{e}}e and {De Putter}, Roland and Dhital, Saurav and Ealet, Anne and Ebelke, Garrett L. and Eisenstein, Daniel J. and Escoffier, S. and Fan, Xiaohui and {Filiz Ak}, N. and Finley, Hayley and Font-Ribera, Andreu and G{\'{e}}nova-Santos, R. and Gunn, James E. and Guo, Hong and Haggard, Daryl and Hall, Patrick B. and Hamilton, Jean Christophe and Harris, Ben and Harris, David W. and Ho, Shirley and Hogg, David W. and Holder, Diana and Honscheid, Klaus and Huehnerhoff, Joe and Jordan, Beatrice and Jordan, Wendell P. and Kauffmann, Guinevere and Kazin, Eyala and Kirkby, David and Klaene, Mark A. and Kneib, Jean Paul and Legoff, Jean Marc and Lee, Khee Gan and Long, Daniel C. and Loomis, Craig P. and Lundgren, Britt and Lupton, Roberth and Maia, Marcio A.G. and Makler, Martin and Malanushenko, Elena and Malanushenko, Viktor and Mandelbaum, Rachel and Manera, Marc and Maraston, Claudia and Margala, Daniel and Masters, Karen L. and McBride, Cameron K. and McDonald, Patrick and McGreer, Iand and McMahon, Richardg and Mena, Olga and Miralda-Escud{\'{e}}, Jordi and Montero-Dorta, Antonio D. and Montesano, Francesco and Muna, Demitri and Myers, Adam D. and Naugle, Tracy and Nichol, Robert C. and Noterdaeme, Pasquier and Nuza, Sebasti{\'{a}}n E. and Olmstead, Matthew D. and Oravetz, Audrey and Oravetz, Danielj and Owen, Russell and Padmanabhan, Nikhil and Palanque-Delabrouille, Nathalie and Pan, Kaike and Parejko, Johnk and P{\^{a}}ris, Isabelle and Percival, Will J. and P{\'{e}}rez-Fournon, Ismael and P{\'{e}}rez-R{\`{a}}fols, Ignasi and Petitjean, Patrick and Pfaffenberger, Robert and Pforr, Janine and Pieri, Matthew M. and Prada, Francisco and Price-Whelan, Adrianm and Raddick, M. Jordan and Rebolo, Rafael and Rich, James and Richards, Gordon T. and Rockosi, Constancem and Roe, Nataliea and Ross, Ashley J. and Ross, Nicholas P. and Rossi, Graziano and Rubi{\~{n}}o-Martin, J. A. and Samushia, Lado and S{\'{a}}nchez, Arielg and Sayres, Conor and Schmidt, Sarah J. and Schneider, Donald P. and Sc{\'{o}}ccola, C. G. and Seo, Hee Jong and Shelden, Alaina and Sheldon, Erin and Shen, Yue and Shu, Yiping and Slosar, An{\v{z}}e and Smee, Stephena and Snedden, Stephanie A. and Stauffer, Fritz and Steele, Oliver and Strauss, Michaela and Streblyanska, Alina and Suzuki, Nao and Swanson, Mollye C. and Tal, Tomer and Tanaka, Masayuki and Thomas, Daniel and Tinker, Jeremy L. and Tojeiro, Rita and Tremonti, Christya and {Vargas Maga{\~{n}}a}, M. and Verde, Licia and Viel, Matteo and Wake, David A. and Watson, Mike and Weaver, Benjamina and Weinberg, David H. and Weiner, Benjamin J. and West, Andrew A. and White, Martin and Wood-Vasey, W. M. and Yeche, Christophe and Zehavi, Idit and Zhao, Gong Bo and Zheng, Zheng}, -doi = {10.1088/0004-6256/145/1/10}, -eprint = {1208.0022}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {cosmology: observations,surveys}, -month = {jan}, -number = {1}, -pages = {10}, -title = {{The baryon oscillation spectroscopic survey of SDSS-III}}, -url = {http://stacks.iop.org/1538-3881/145/i=1/a=10?key=crossref.af65e7d4595bf6350e8598f97f044dc6}, -volume = {145}, -year = {2013} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Greene2017, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10^12.5 h^-1 M_sun < M_200b < 10^15 h^-1 M_sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that $\sim$ 70% of galaxies with stellar mass M_* > 10^11 h^-2 M_sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The $\sim$ 30% of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20\% level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J. E. and Leauthaud, A. and Emsellem, E. and Ge, J. and Arag{\'{o}}n-Salamanca, A. and Greco, J. and Lin, Y.-T. and Mao, S. and Masters, K. and Merrifield, M. and More, S. and Okabe, N. and Schneider, D. P. and Thomas, D. and Wake, D. A. and Pan, K. and Bizyaev, D. and Oravetz, D. and Simmons, A. and Yan, R. and van den Bosch, F.}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2018 - SDSS-IV MaNGA Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of {\$\sim${}}3692 galaxies, with -18.5 {\textless}= M{\_}g {\textless} -22.0 mag and redshift 0.01 {\textless}= z {\textless} 0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of {\$\sim${}}2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined ({\textgreater}60 degrees) systems, we find the following results. (1) The optical r-band fraction (f{\_}opt-r) of barred galaxies is {\$\sim${}}48{\%}-52{\%}. (2) When galaxies are separated according to normalized half light radius (r{\_}e/R{\_}24), a remarkable result is seen: f{\_}opt-r rises sharply, from {\$\sim${}}40{\%} in galaxies that have small r{\_}e/R{\_}24 and visually appear to host prominent bulges, to {\$\sim${}}70{\%} for galaxies that have large r{\_}e/R{\_}24 and appear disk-dominated. (3) f{\_}opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that {\$\sim${}}20{\%} of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity {\textgreater}=0.4) and large enough (semi-major axis {\textgreater}=1.5 kpc) to be reliably characterized via ellipse-fitting out to z{\$\sim${}}0.8, we get an optical r-band fraction for strong bars f{\_}opt-s of {\$\sim${}}34{\%}. This value is higher only by a modest factor of 1.4, compared to the value of {\$\sim${}}24{\%}+-4{\%} reported at z{\$\sim${}}0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z{\$\sim${}}0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Johnson, Crockett}, -doi = {10.2307/3616804}, -eprint = {0802.3961}, -issn = {00255572}, -journal = {The Mathematical Gazette}, -keywords = {Astrophysics}, -number = {407}, -pages = {17}, -title = {{A Construction for a Regular Heptagon}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {59}, -year = {1975} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for {\$\sim${}}20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Tian2017, -abstract = {We study themass discrepancy-acceleration relation (MDAR) of 57 elliptical galaxies by their Einstein rings from the Sloan Lens ACS Survey (SLACS). The mass discrepancy between the lensing mass and the baryonic mass derived from population synthesis is larger when the acceleration of the elliptical galaxy lenses is smaller. TheMDAR is also related to surface mass density discrepancy. At the Einstein ring, these lenses belong to high-surface-mass density galaxies. Similarly, we find that the discrepancy between the lensing and stellar surface mass density is small. It is consistent with the recent discovery of dynamical surface mass density discrepancy in disc galaxies where the discrepancy is smaller when surface density is larger. We also find relativistic modified Newtonian dynamics (MOND) can naturally explain the MDAR and surface mass density discrepancy in 57 Einstein rings. Moreover, the lensing mass, the dynamical mass and the stellar mass of these galaxies are consistent with each other in relativistic MOND.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1702.00183}, -author = {Tian, Yong and Ko, Chung Ming}, -doi = {10.1093/MNRAS/STX2056}, -eprint = {1702.00183}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tian, Ko - 2017 - Mass discrepancy-acceleration relation in Einstein rings.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: kinematics and dynamics,Dark matter,Galaxies: elliptical and lenticular,Gravitation,Gravitational lensing: strong}, -number = {1}, -pages = {765--771}, -title = {{Mass discrepancy-acceleration relation in Einstein rings}}, -url = {http://arxiv.org/abs/1702.00183}, -volume = {472}, -year = {2017} -} -@article{Libeskind2014, -abstract = {We examine the angular infall pattern of subhaloes onto host haloes in the context of the large-scale structure. We find that this infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are found to be preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that its always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range ({\$\sim${}}10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group}, -archivePrefix = {arXiv}, -arxivId = {1407.0394}, -author = {Libeskind, Noam I and Knebe, Alexander and Hoffman, Yehuda and Gottl{\"{o}}ber, Stefan}, -doi = {10.1093/mnras/stu1216}, -eprint = {1407.0394}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Large-scale structure of universe}, -number = {2}, -pages = {1274--1280}, -title = {{The universal nature of subhalo accretion}}, -volume = {443}, -year = {2014} -} -@article{Shuntov2024, -abstract = {We study the stellar mass function (SMF) and the co-evolution with dark matter halos via abundance matching in the largest redshift range to date $0.25$, we find increased abundances of massive (log$\, M_{\star}/M_{\odot}>10.5$) implying integrated star formation efficiencies (SFE) $\epsilon_{\star}\equiv M_{\star}\, f_{\rm b}^{-1} M_{\rm halo}^{-1} \gtrsim 0.5$. We find a flattening of the SMF at the high-mass end that is better described by a double power law at $z>5.5$. At $z \lesssim 5.5$ it transitions to a Schechter law which coincides with the emergence of the first massive quiescent galaxies in the Universe. We trace the cosmic stellar mass density (SMD) and infer the star formation rate density (SFRD), which at $z>7.5$ agrees remarkably with recent \JWST{} UV luminosity function-derived estimates. However, at $z \lesssim 3.5$, we find significant tension ($\sim 0.3$ dex) with the cosmic star formation (SF) history from instantaneous SF measures, the causes of which remain poorly understood. We infer the stellar-to-halo mass relation (SHMR) and the SFE from abundance matching out to $z=12$, finding a non-monotonic evolution. The SFE has the characteristic strong dependence with mass in the range of $0.02 - 0.2$, and mildly decreases at the low mass end out to $z\sim3.5$. At $z\sim3.5$ the SFE increases sharply from $\sim 0.1$ to approach high SFE of $0.8-1$ by $z\sim 10$ for log$(M_{\rm h}/M_{\odot})\approx11.5$, albeit with large uncertainties. Finally, we use the SHMR to track the SFE and stellar mass growth throughout the halo history and find that they do not grow at the same rate -- from the earliest times up until $z\sim3.5$ the halo growth rate outpaces galaxy assembly, but at $z>3.5$ halo growth stagnates and accumulated gas reservoirs keep the SF going and galaxies outpace halos.}, -archivePrefix = {arXiv}, -arxivId = {2410.08290}, -author = {Shuntov, M. and Ilbert, O. and Toft, S. and Arango-Toro, R. C. and Akins, H. B. and Casey, C. M. and Franco, M. and Harish, S. and Kartaltepe, J. S. and Koekemoer, A. M. and McCracken, H. J. and Paquereau, L. and Laigle, C. and Bethermin, M. and Dubois, Y. and Drakos, N. E. and Faisst, A. and Gozaliasl, G. and Gillman, S. and Hayward, C. C. and Hirschmann, M. and Huertas-Company, M. and Jespersen, C. K. and Jin, S. and Kokorev, V. and Lambrides, E. and Borgne, D. Le and Liu, D. and Magdis, G. and Massey, R. and McPartland, C. J. R. and Mercier, W. and McCleary, J. E. and McKinney, J. and Oesch, P. A. and Rhodes, J. D. and Rich, R. M. and Robertson, B. E. and Sanders, D. and Trebitsch, M. and Tresse, L. and Valentino, F. and Vijayan, A. P. and Weaver, J. R. and Weibel, A. and Wilkins, S. M.}, -eprint = {2410.08290}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Shuntvo2024reduction.pdf:pdf}, -keywords = {evolution,galaxies,high-redshift,luminosity function,mass function,statistics}, -pages = {1--31}, -title = {{COSMOS-Web: stellar mass assembly in relation to dark matter halos across $0.2 10^11 h^-2 M_sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The $\sim$ 30% of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20\% level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J. E. and Leauthaud, A. and Emsellem, E. and Ge, J. and Arag{\'{o}}n-Salamanca, A. and Greco, J. and Lin, Y.-T. and Mao, S. and Masters, K. and Merrifield, M. and More, S. and Okabe, N. and Schneider, D. P. and Thomas, D. and Wake, D. A. and Pan, K. and Bizyaev, D. and Oravetz, D. and Simmons, A. and Yan, R. and van den Bosch, F.}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2018 - SDSS-IV MaNGA Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Du2020, -abstract = {We recently developed an automated method, auto-GMM, to kinematically decompose simulated galaxies. It extracts the kinematic structures in an accurate, efficient, and unsupervised way. Here we use auto-GMM to study the stellar kinematic structures of disk galaxies from the TNG100 run of the cosmological suite IllustrisTNG. We identify four to five kinematic structures that are commonly present among the diverse galaxy population. Structures having strong to moderate rotation are defined as cold and warm disks, respectively. Spheroidal structures dominated by random motions are classified as bulges or stellar halos, depending on how tightly bound they are. Disky bulges are defined as structures that have moderate rotation but compact morphology. TNG100 returns multiple structures that have reasonable properties, qualitatively consistent with our general expectations. Across all disky galaxies and accounting for the stellar mass within 3 half-mass radii, the kinematic spheroidal structures, obtained by summing up stars of bulges and halos, contribute $\sim 45\%$ of the total stellar mass, while the disky structures constitute $\sim 55\%$. This study also provides important insights about the relationship between kinematically and morphologically derived galactic structures. Comparing the morphology of kinematic structures with that of traditional bulge+disk decomposition, we conclude: (1) the morphologically decomposed bulges are composite structures comprised of a slowly rotating bulge, an inner halo, and a disky bulge; (2) kinematically disky bulges, akin to what are commonly called pseudo bulges in observations, are compact disk-like components that have rotation similar to warm disks; (3) halos contribute almost $30\%$ of the surface density of the outer part of morphological disks when viewed face-on; and (4) both cold and warm disks are often truncated in central regions.}, -archivePrefix = {arXiv}, -arxivId = {2002.04182}, -author = {Du, Min and Ho, Luis C. and Debattista, Victor P. and Pillepich, Annalisa and Nelson, Dylan and Zhao, Dongyao and Hernquist, Lars}, -doi = {10.3847/1538-4357/ab8fa8}, -eprint = {2002.04182}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Du et al. - 2020 - Kinematic Decomposition of IllustrisTNG Disk Galaxies Morphology and Relation with Morphological Structures.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {391,591,602,622,767,corresponding author,disk galaxies,galaxy dynamics,galaxy kinematics,galaxy structure,hydrodynamical simulations,min du}, -number = {2}, -pages = {139}, -title = {{Kinematic Decomposition of IllustrisTNG Disk Galaxies: Morphology and Relation with Morphological Structures}}, -url = {http://arxiv.org/abs/2002.04182}, -volume = {895}, -year = {2020} -} -@article{Naab2007, -abstract = {We describe high-resolution smoothed particle hydrodynamics (SPH) simulations of three approximately M* field galaxies starting from {\$}\Lambda{\$}CDM initial conditions. The simulations are made intentionally simple, and include photoionization, cooling of the intergalactic medium, and star formation, but not feedback from AGNs or supernovae. All of the galaxies undergo an initial burst of star formation at z{\$\sim${}}5, accompanied by the formation of a bubble of heated gas. Two out of three galaxies show early-type properties at present, whereas only one of them experienced a major merger. Heating from shocks and PdV work dominates over cooling so that for most of the gas the temperature is an increasing function of time. By z{\$\sim${}}1 a significant fraction of the final stellar system is in place and the spectral energy distribution resembles those of observed massive red galaxies. The galaxies have grown from z=1--{\textgreater}0 on average by 25{\%} in mass and in size by gas-poor (dry) stellar mergers. By the present day the simulated galaxies are old ({\$\sim${}}10 Gyr), kinematically hot stellar systems surrounded by hot gaseous haloes. Stars dominate the mass of the galaxies up to {\$\sim${}}4 effective radii ({\$\sim${}}10 kpc). Kinematic and most photometric properties are in good agreement with those of observed elliptical galaxies. The galaxy with a major merger develops a counter-rotating core. Our simulations show that realistic intermediate-mass giant elliptical galaxies with plausible formation histories can be formed from {\$}\Lambda{\$}CDM initial conditions even without requiring recent major mergers or feedback from supernovae or AGNs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0512235}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P and Efstathiou, George}, -doi = {10.1086/510841}, -eprint = {0512235}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {710--720}, -primaryClass = {astro-ph}, -title = {{Formation of Early‐Type Galaxies from Cosmological Initial Conditions}}, -url = {http://stacks.iop.org/0004-637X/658/i=2/a=710}, -volume = {658}, -year = {2007} -} -@article{Wertz2018, -abstract = {The modern time-delay cosmography aims to infer the cosmological parameters with a competitive precision from observing a multiply imaged quasar. The success of this technique relies upon a robust modeling of the lens mass distribution. Unfortunately strong degeneracies between density profiles that lead to almost the same lensing observables may bias precise estimate for the Hubble constant. The source position transformation (SPT), which covers the well-known mass sheet transformation (MST) as a special case, defines a new framework to investigate these degeneracies. In this paper, we present pySPT, a Python package dedicated to the SPT. We describe how it can be used to evaluate the impact of the SPT on lensing observables. We review most of its capabilities and elaborate on key features that we used in a companion paper regarding SPT and time delays. pySPT also comes with a sub-package dedicated to simple lens modeling. It can be used to generate lensing related quantities for a wide variety of lens models, independently from any SPT analysis. As a first practical application, we present a correction to the first estimate of the impact on time delays of the SPT, which has been experimentally found in Schneider and Sluse (2013) between a softened power-law and a composite (baryons + dark matter) lenses. We find that the large deviations predicted in Schneider and Sluse (2014) have been overestimated due to a minor bug (now fixed) in the public lens modeling code lensmodel (v1.99). We conclude that the predictions for the Hubble constant deviate by {\$}\backslashsim 7{\$}$\backslash${\%}, first and foremost caused by an MST. The latest version of pySPT is available at https://github.com/owertz/pySPT. We also provide tutorials to describe in detail how making the best use of pySPT at https://github.com/owertz/pySPT{\_}tutorials.}, -archivePrefix = {arXiv}, -arxivId = {1801.04151}, -author = {Wertz, Olivier and Orthen, Bastian}, -doi = {10.1051/0004-6361/201732242}, -eprint = {1801.04151}, -keywords = {cosmological parameters,gravitational lensing,strong}, -pages = {1--9}, -title = {{pySPT: a package dedicated to the source position transformation}}, -url = {http://arxiv.org/abs/1801.04151%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201732242}, -year = {2018} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of $\sim$3692 galaxies, with -18.5 <= M_g < -22.0 mag and redshift 0.01 <= z < 0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of $\sim$2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined (>60 degrees) systems, we find the following results. (1) The optical r-band fraction (f_opt-r) of barred galaxies is $\sim$48%-52%. (2) When galaxies are separated according to normalized half light radius (r_e/R_24), a remarkable result is seen: f_opt-r rises sharply, from $\sim$40% in galaxies that have small r_e/R_24 and visually appear to host prominent bulges, to $\sim$70% for galaxies that have large r_e/R_24 and appear disk-dominated. (3) f_opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that $\sim$20% of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity >=0.4) and large enough (semi-major axis >=1.5 kpc) to be reliably characterized via ellipse-fitting out to z$\sim$0.8, we get an optical r-band fraction for strong bars f_opt-s of $\sim$34%. This value is higher only by a modest factor of 1.4, compared to the value of $\sim$24%+-4% reported at z$\sim$0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z$\sim$0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Johnson, Crockett}, -doi = {10.2307/3616804}, -eprint = {0802.3961}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Johnson - 1975 - A Construction for a Regular Heptagon.pdf:pdf}, -issn = {00255572}, -journal = {The Mathematical Gazette}, -keywords = {Astrophysics}, -number = {407}, -pages = {17}, -title = {{A Construction for a Regular Heptagon}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {59}, -year = {1975} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Baugh:1996aa, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9602085}, -author = {Baugh, C. M. and Cole, S. and Frenk, C. S.}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Baugh, Cole, Frenk - 1996 - Evolution of the Bubble sequence in hierarchical models for galaxy formation(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function, mass function}, -month = {dec}, -number = {4}, -pages = {1361--1378}, -primaryClass = {astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -url = {http://adsabs.harvard.edu/abs/1996MNRAS.283.1361B}, -volume = {283}, -year = {1996} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright} 2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel, Sari, Ceverino - 2009 - Formation of massive galaxies at high redshift Cold streams, clumpy disks, and compact spheroids(2).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@inproceedings{MartinNavarro2013, -author = {Mart$\backslash$'$\backslash$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Huang2018, -abstract = {We use $\sim$100 deg2 of deep (> 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach $\sim$4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) > 11.6 in more massive haloes at 0.3 < z < 0.5 have shallower inner stellar mass density profiles (within $\sim$10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) > 14.0 are $\sim$20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2018 - A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{Peng2002, -abstract = {We present a two-dimensional (2-D) fitting algorithm (GALFIT) designed to extract structural components from galaxy images, with emphasis on closely modeling light profiles of spatially well-resolved, nearby galaxies observed with the Hubble Space Telescope. Our algorithm improves on previous techniques in two areas, by being able to simultaneously fit a galaxy with an arbitrary number of components, and with optimization in computation speed, suited for working on large galaxy images. We use 2-D models such as the ``Nuker'' law, the Sersic (de Vaucouleurs) profile, an exponential disk, and Gaussian or Moffat functions. The azimuthal shapes are generalized ellipses that can fit disky and boxy components. Many galaxies with complex isophotes, ellipticity changes, and position-angle twists can be modeled accurately in 2-D. When examined in detail, we find that even simple-looking galaxies generally require at least three components to be modeled accurately, rather than the one or two components more often employed. We illustrate this by way of 7 case studies, which include regular and barred spiral galaxies, highly disky lenticular galaxies, and elliptical galaxies displaying various levels of complexities. A useful extension of this algorithm is to accurately extract nuclear point sources in galaxies. We compare 2-D and 1-D extraction techniques on simulated images of galaxies having nuclear slopes with different degrees of cuspiness, and we then illustrate the application of the program to several examples of nearby galaxies with weak nuclei.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0204182}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans-Walter}, -doi = {10.1086/340952}, -eprint = {0204182}, -isbn = {0004-6256}, -issn = {00046256}, -primaryClass = {astro-ph}, -title = {{Detailed Structural Decomposition of Galaxy Images}}, -url = {http://arxiv.org/abs/astro-ph/0204182%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/340952}, -year = {2002} -} -@article{Dutton2010, -abstract = {Using estimates of dark halo masses from satellite kinematics, weak gravitational lensing and halo abundance matching, combined with the Tully-Fisher (TF) and Faber-Jackson relations, we derive the mean relation between the optical, Vopt, and virial, V200, circular velocities of early- and late-type galaxies at redshift z≃ 0. For late-type galaxies, Vopt≃V200 over the velocity range Vopt= 90-260 km s-1, and is consistent with Vopt=Vmax,h[the maximum circular velocity of NFW dark matter haloes in the concordance $\Lambda$ cold dark matter ($\Lambda$ CDM) cosmology]. However, for early-type galaxies Vopt≠V200, with the exception of early-type galaxies with Vopt≃ 350 km s-1. This is inconsistent with early-type galaxies being, in general, globally isothermal. For low-mass (Vopt≲ 250 km s-1) early-types Vopt > Vmax,h, indicating that baryons have modified the potential well, while high-mass (Vopt > rsim 400 km s-1) early-types have Vopt < Vmax,h. Folding in measurements of the black hole mass-velocity dispersion relation, our results imply that the supermassive black hole-halo mass relation has a logarithmic slope which varies from ≃1.4 at halo masses of ≃ 1012 h-1 M⊙ to ≃0.65 at halo masses of 1013.5 h-1 M⊙. The values of Vopt/V200 we infer for the Milky Way (MW) and M31 are lower than the values currently favoured by direct observations and dynamical models. This offset is due to the fact that the MW and M31 have higher Vopt and lower V200 compared to typical late-type galaxies of the same stellar masses. We show that current high-resolution cosmological hydrodynamical simulations are unable to form galaxies which simultaneously reproduce both the Vopt/V200 ratio and the Vopt-Mstar (Tully-Fisher/Faber-Jackson) relation. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1004.4626}, -author = {Dutton, Aaron A. and Conroy, Charlie and van den Bosch, Frank C. and Prada, Francisco and More, Surhud}, -doi = {10.1111/j.1365-2966.2010.16911.x}, -eprint = {1004.4626}, -isbn = {doi:10.1111/j.1365-2966.2010.16911.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: kinematics and dynamics,Galaxies: spiral}, -month = {sep}, -number = {1}, -pages = {2--16}, -title = {{The kinematic connection between galaxies and dark matter haloes}}, -volume = {407}, -year = {2010} -} -@article{Schombert2015a, -abstract = {Using isophotal radius correlations for a sample of Two Micron All Sky Survey ellipticals, we have constructed a series of template surface brightness profiles to describe the profile shapes of ellipticals as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that ellipticals are weakly nonhomologous with respect to structure. Through comparison to the templates, it is discovered that ellipticals are divided into two families: those well matched to the templates, and a second class of ellipticals with distinctly shallower profile slopes. We refer to this second type of ellipticals as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D ellipticals cover the same range of luminosity, size, and kinematics as normal ellipticals, but maintain a signature of recent equal-mass dry mergers. We propose that normal ellipticals grow after an initial dissipation formation era by accretion of low-mass companions as outlined in hierarchical formation scenarios, while D ellipticals are the result of later equal-mass mergers producing shallow luminosity profiles.}, -archivePrefix = {arXiv}, -arxivId = {1509.08381}, -author = {Schombert, James M}, -doi = {10.1088/0004-6256/150/5/162}, -eprint = {1509.08381}, -isbn = {doi:10.1088/0004-6256/150/5/162}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: structure}, -number = {5}, -pages = {162}, -publisher = {IOP Publishing}, -title = {{The structure of galaxies. III. Two structural families of ellipticals}}, -url = {http://dx.doi.org/10.1088/0004-6256/150/5/162}, -volume = {150}, -year = {2015} -} -@inproceedings{MartinNavarro2013, -author = {Mart$\backslash$'$\backslash$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Kriek2009, -abstract = {We present Hubble Space Telescope NIC2 morphologies of a spectroscopic sample of massive galaxies at z 2.3 by extending our sample of 9 compact quiescent galaxies (re 0.9kpc) with 10 massive emission-line galaxies. The emission-line galaxies are classified by the nature of their ionized emission; there are six star-forming galaxies and four galaxies hosting an active galactic nucleus (AGN). The star-forming galaxies are the largest among the emission-line galaxies, with a median size of re = 2.8kpc. The three galaxies with the highest star formation rates (≳100 M ⊙ 1 yr-1) have irregular and clumpy morphologies. The AGN host galaxies are more similar to the compact quiescent galaxies in terms of their structures (re ∼ 1.1 kpc) and spectral energy distributions. The total sample clearly separates into two classes in a color-mass diagram: the large star-forming galaxies that form the blue cloud, and the compact quiescent galaxies on the red sequence. However, it is unclear how or even if the two classes are evolutionary related. Three out of six massive star-forming galaxies have dense cores and thus may passively evolve into compact galaxies due to fading of outer star-forming regions. For these galaxies, a reverse scenario in which compact galaxies grow inside-out by star formation is also plausible. We do caution though that the sample is small. Nonetheless, it is evident that a Hubble sequence of massive galaxies with strongly correlated galaxy properties is already in place at z > 2. {\textcopyright} 2009. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0909.0260}, -author = {Kriek, Mariska and {Van Dokkum}, Pieter G. and Franx, Marijn and Illingworth, Garth D. and Magee, Daniel K.}, -doi = {10.1088/0004-637X/705/1/L71}, -eprint = {0909.0260}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: high-redshift}, -month = {nov}, -number = {1 PART 2}, -pages = {L71--L75}, -title = {{The hubble sequence beyond z = 2 for massive galaxies: Contrasting large star-forming and compact quiescent galaxies}}, -url = {http://stacks.iop.org/1538-4357/705/i=1/a=L71?key=crossref.a63f47133fb5eb550976715d6b334b17}, -volume = {705}, -year = {2009} -} -@article{EuclidCollaboration2025b, -abstract = {We present a search for strong gravitational lenses in Euclid imaging with high stellar velocity dispersion ($\sigma_\nu > 180$ km/s) reported by SDSS and DESI. We performed expert visual inspection and classification of $11\,660$ \Euclid images. We discovered 38 grade A and 40 grade B candidate lenses, consistent with an expected sample of $\sim$32. Palomar spectroscopy confirmed 5 lens systems, while DESI spectra confirmed one, provided ambiguous results for another, and help to discard one. The \Euclid automated lens modeler modelled 53 candidates, confirming 38 as lenses, failing to model 9, and ruling out 6 grade B candidates. For the remaining 25 candidates we could not gather additional information. More importantly, our expert-classified non-lenses provide an excellent training set for machine learning lens classifiers. We create high-fidelity simulations of \Euclid lenses by painting realistic lensed sources behind the expert tagged (non-lens) luminous red galaxies. This training set is the foundation stone for the \Euclid galaxy-galaxy strong lensing discovery engine.}, -archivePrefix = {arXiv}, -arxivId = {2503.15325}, -author = {{Euclid Collaboration} and Rojas, K. and Collett, T. E. and Barroso, J. A. Acevedo and Nightingale, J. W. and Stern, D. and Moustakas, L. A. and Schuldt, S. and Despali, G. and Melo, A. and Walmsley, M. and Ballard, D. J. and Enzi, W. J. R. and Li, T. and de Murieta, A. Sainz and Andika, I. T. and Cl{\'{e}}ment, B. and Courbin, F. and Ecker, L. R. and Gavazzi, R. and Jackson, N. and Kov{\'{a}}cs, A. and Matavulj, P. and Meneghetti, M. and Serjeant, S. and Sluse, D. and Tortora, C. and Verma, A. and Marchetti, L. and O'Riordan, C. M. and McCarthy, K. and Suyu, S. H. and Metcalf, R. B. and Aghanim, N. and Altieri, B. and Amara, A. and Andreon, S. and Auricchio, N. and Aussel, H. and Baccigalupi, C. and Baldi, M. and Balestra, A. and Bardelli, S. and Battaglia, P. and Bender, R. and Biviano, A. and Bonchi, A. and Branchini, E. and Brescia, M. and Brinchmann, J. and Camera, S. and Ca{\~{n}}as-Herrera, G. and Capobianco, V. and Carbone, C. and Cardone, V. F. and Carretero, J. and Casas, S. and Castellano, M. and Castignani, G. and Cavuoti, S. and Chambers, K. C. and Cimatti, A. and Colodro-Conde, C. and Congedo, G. and Conselice, C. J. and Conversi, L. and Copin, Y. and Courtois, H. M. and Cropper, M. and {Da Silva}, A. and Degaudenzi, H. and {De Lucia}, G. and {Di Giorgio}, A. M. and Dolding, C. and Dole, H. and Dubath, F. and Dupac, X. and Escoffier, S. and Fabricius, M. and Farina, M. and Farinelli, R. and Faustini, F. and Ferriol, S. and Finelli, F. and Fotopoulou, S. and Frailis, M. and Franceschi, E. and Galeotta, S. and George, K. and Gillard, W. and Gillis, B. and Giocoli, C. and G{\'{o}}mez-Alvarez, P. and Gracia-Carpio, J. and Granett, B. R. and Grazian, A. and Grupp, F. and Guzzo, L. and Gwyn, S. and Haugan, S. V. H. and Holmes, W. and Hook, I. M. and Hormuth, F. and Hornstrup, A. and Hudelot, P. and Jahnke, K. and Jhabvala, M. and Keih{\"{a}}nen, E. and Kermiche, S. and Kiessling, A. and Kubik, B. and Kuijken, K. and K{\"{u}}mmel, M. and Kunz, M. and Kurki-Suonio, H. and Boulc'h, Q. Le and Brun, A. M. C. Le and Mignant, D. Le and Liebing, P. and Ligori, S. and Lilje, P. B. and Lindholm, V. and Lloro, I. and Mainetti, G. and Maino, D. and Maiorano, E. and Mansutti, O. and Marcin, S. and Marggraf, O. and Martinelli, M. and Martinet, N. and Marulli, F. and Massey, R. and Maurogordato, S. and McCracken, H. J. and Medinaceli, E. and Mei, S. and Melchior, M. and Mellier, Y. and Merlin, E. and Meylan, G. and Mora, A. and Moresco, M. and Moscardini, L. and Nakajima, R. and Neissner, C. and Nichol, R. C. and Niemi, S. -M. and Padilla, C. and Paltani, S. and Pasian, F. and Pedersen, K. and Percival, W. J. and Pettorino, V. and Pires, S. and Polenta, G. and Poncet, M. and Popa, L. A. and Pozzetti, L. and Raison, F. and Rebolo, R. and Renzi, A. and Rhodes, J. and Riccio, G. and Romelli, E. and Roncarelli, M. and Saglia, R. and Sakr, Z. and S{\'{a}}nchez, A. G. and Sapone, D. and Sartoris, B. and Schewtschenko, J. A. and Schirmer, M. and Schneider, P. and Schrabback, T. and Secroun, A. and Seidel, G. and Seiffert, M. and Serrano, S. and Simon, P. and Sirignano, C. and Sirri, G. and Stanco, L. and Steinwagner, J. and Tallada-Cresp{\'{i}}, P. and Taylor, A. N. and Tereno, I. and Toft, S. and Toledo-Moreo, R. and Torradeflot, F. and Tutusaus, I. and Valenziano, L. and Valiviita, J. and Vassallo, T. and Kleijn, G. Verdoes and Veropalumbo, A. and Wang, Y. and Weller, J. and Zacchei, A. and Zamorani, G. and Zerbi, F. M. and Zucca, E. and Ballardini, M. and Bolzonella, M. and Bozzo, E. and Burigana, C. and Cabanac, R. and Cappi, A. and {Di Ferdinando}, D. and Vigo, J. A. Escartin and Gabarra, L. and Mart{\'{i}}n-Fleitas, J. and Matthew, S. and Mauri, N. and Pezzotta, A. and P{\"{o}}ntinen, M. and Porciani, C. and Risso, I. and Scottez, V. and Sereno, M. and Tenti, M. and Viel, M. and Wiesmann, M. and Akrami, Y. and Alvi, S. and Anselmi, S. and Archidiacono, M. and Atrio-Barandela, F. and Benoist, C. and Benson, K. and Bergamini, P. and Bertacca, D. and Bethermin, M. and Blanchard, A. and Blot, L. and Brown, M. L. and Bruton, S. and Calabro, A. and Quevedo, B. Camacho and Caro, F. and Carvalho, C. S. and Castro, T. and Cogato, F. and Cooray, A. R. and Cucciati, O. and Davini, S. and {De Paolis}, F. and Desprez, G. and D{\'{i}}az-S{\'{a}}nchez, A. and Diaz, J. J. and {Di Domizio}, S. and Diego, J. M. and Duc, P. -A. and Enia, A. and Fang, Y. and Ferrari, A. G. and Ferreira, P. G. and Finoguenov, A. and Fontana, A. and Franco, A. and Ganga, K. and Garc{\'{i}}a-Bellido, J. and Gasparetto, T. and Gautard, V. and Gaztanaga, E. and Giacomini, F. and Gianotti, F. and Gozaliasl, G. and Guidi, M. and Gutierrez, C. M. and Hall, A. and Hartley, W. G. and Hern{\'{a}}ndez-Monteagudo, C. and Hildebrandt, H. and Hjorth, J. and Kajava, J. J. E. and Kang, Y. and Kansal, V. and Karagiannis, D. and Kiiveri, K. and Kirkpatrick, C. C. and Kruk, S. and Graet, J. Le and Legrand, L. and Lembo, M. and Lepori, F. and Leroy, G. and Lesci, G. F. and Lesgourgues, J. and Leuzzi, L. and Liaudat, T. I. and Loureiro, A. and Macias-Perez, J. and Maggio, G. and Magliocchetti, M. and Magnier, E. A. and Mannucci, F. and Maoli, R. and Martins, C. J. A. P. and Maurin, L. and Miluzio, M. and Monaco, P. and Moretti, C. and Morgante, G. and Nadathur, S. and Naidoo, K. and Navarro-Alsina, A. and Nesseris, S. and Passalacqua, F. and Paterson, K. and Patrizii, L. and Pisani, A. and Potter, D. and Quai, S. and Radovich, M. and Rocci, P. -F. and Sacquegna, S. and Sahl{\'{e}}n, M. and Sanders, D. B. and Sarpa, E. and Scarlata, C. and Schneider, A. and Sciotti, D. and Sellentin, E. and Smith, L. C. and Tanidis, K. and Testera, G. and Teyssier, R. and Troja, A. and Tucci, M. and Valieri, C. and Venhola, A. and Vergani, D. and Vernardos, G. and Verza, G. and Vielzeuf, P. and Walton, N. A. and Wilde, J. and Scott, D.}, -eprint = {2503.15325}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/EuclidQ12025paperIII.pdf:pdf}, -journal = {https://arxiv.org/pdf/2503.15325}, -keywords = {catalogs,gravitational lensing,methods,statistical,strong}, -title = {{Euclid Quick Data Release (Q1) The Strong Lensing Discovery Engine B -- Early strong lens candidates from visual inspection of high velocity dispersion galaxies}}, -url = {http://arxiv.org/abs/2503.15325}, -year = {2025} -} -@article{Richings2021, -abstract = {We present a cosmological hydrodynamical simulation of a 1013 MO galaxy group and its environment (out to 10 times the virial radius) carried out using the eagle model of galaxy formation. Exploiting a novel technique to increase the resolution of the dark matter calculation independently of that of the gas, the simulation resolves dark matter haloes and subhaloes of mass 5 × 106 MO. It is therefore useful for studying the abundance and properties of the haloes and subhaloes targeted in strong lensing tests of the cold dark matter model. We estimate the halo and subhalo mass functions and discuss how they are affected both by the inclusion of baryons in the simulation and by the environment. We find that the halo and subhalo mass functions have lower amplitude in the hydrodynamical simulation than in its dark-matter-only counterpart. This reflects the reduced growth of haloes in the hydrodynamical simulation due to the early loss of gas by reionization and galactic winds and, additionally, in the case of subhaloes, disruption by enhanced tidal effects within the host halo due to the presence of a massive central galaxy. The distribution of haloes is highly anisotropic reflecting the filamentary character of mass accretion on to the cluster. As a result, there is significant variation in the number of structures with viewing direction. The median number of structures near the centre of the halo, when viewed in projection, is reduced by a factor of 2 when baryons are included.}, -archivePrefix = {arXiv}, -arxivId = {2005.14495}, -author = {Richings, Jack and Frenk, Carlos and Jenkins, Adrian and Robertson, Andrew and Schaller, Matthieu}, -doi = {10.1093/mnras/staa4013}, -eprint = {2005.14495}, -file = {:C\:/Users/Jammy/Documents/Papers/Ellipticals/Richings2020StrongLEnsSim.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cosmology: theory,dark matter,gravitational lensing: strong}, -number = {3}, -pages = {4657--4668}, -title = {{A high-resolution cosmological simulation of a strong gravitational lens}}, -volume = {501}, -year = {2021} -} -@article{Fadely2012, -abstract = {We investigate the properties of dark matter substructure in the gravitational lens HE 0435-1223 (zl=0.455) via its effects on the positions and flux ratios of the quadruply imaged background quasar (zs= 1.689). We start with a smooth mass model, add individual, truncated isothermal clumps near the lensed images and use the Bayesian evidence to compare the quality of different models. Compared with smooth models, models with at least one clump near image A are strongly favoured. The mass of this clump within its Einstein radius is log10(MAEin) = 7.65+0.87- 0.84 (in units of h-170M⊙). The Bayesian evidence provides weaker support for a second clump near image B, with log10(MBEin) = 6.55+1.01- 1.51. We also examine models with a full population of substructure, and find the mass fraction in substructure at the Einstein radius to be fsub>rsim 0.00077, assuming the total clump masses follow a mass function dN/dM∝M-1.9 over the range M= 107-1010M⊙. Few-clump and population models produce similar Bayesian evidence values, so neither type of model is objectively favoured. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1109.0548}, -author = {Fadely, Ross and Keeton, Charles R.}, -doi = {10.1111/j.1365-2966.2011.19729.x}, -eprint = {1109.0548}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Gravitational lensing: strong,Methods: statistical}, -month = {jan}, -number = {2}, -pages = {936--951}, -title = {{Substructure in the lens HE 0435-1223}}, -volume = {419}, -year = {2012} -} -@article{DiCintio2014b, -abstract = {Some tumor-specific near-infrared (NIR) fluorescent dyes such as indocyanine green (ICG), IDRye800CW, and 5-aminolevulinic acid have been used clinically for detecting tumor margins or micro-cancer lesions. In this study, we evaluated the physicochemical properties of liposomally formulated phospholipid-conjugated ICG, denoted by LP-iDOPE, as a clinically translatable NIR imaging nanoparticle for brain tumors. We also confirmed its brain-tumor-specific biodistribution and its characteristics as the intra-operative NIR imaging nanoparticles for brain tumor surgery. These properties of LP-iDOPE may enable neurosurgeons to achieve more accurate identification and more complete resection of brain tumor.}, -archivePrefix = {arXiv}, -arxivId = {1404.5959}, -author = {Suganami, Akiko and Iwadate, Yasuo and Shibata, Sayaka and Yamashita, Masamichi and Tanaka, Tsutomu and Shinozaki, Natsuki and Aoki, Ichio and Saeki, Naokatsu and Shirasawa, Hiroshi and Okamoto, Yoshiharu and Tamura, Yutaka}, -doi = {10.1016/j.ijpharm.2015.10.001}, -eprint = {1404.5959}, -isbn = {0378-5173}, -issn = {18733476}, -journal = {International Journal of Pharmaceutics}, -keywords = {Brain tumor surgery,Indocyanine green (ICG),Intra-operative imaging,Liposome,Near-infrared (NIR)}, -number = {2}, -pages = {401--406}, -pmid = {26453781}, -title = {{Liposomally formulated phospholipid-conjugated indocyanine green for intra-operative brain tumor detection and resection}}, -volume = {496}, -year = {2015} -} -@article{Talbot2018, -abstract = {We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for eight of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with two background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched {\$\sim${}}1.5 million spectra, of which 3065 contained multiple high signal-to-noise ratio background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius ≳ 1.7 arcsec, which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely.}, -archivePrefix = {arXiv}, -arxivId = {1803.03604}, -author = {Talbot, Michael S and Brownstein, Joel R and Bolton, Adam S and Bundy, Kevin and Andrews, Brett H and Cherinka, Brian and Collett, Thomas E and More, Anupreeta and More, Surhud and Sonnenfeld, Alessandro and Vegetti, Simona and Wake, David A and Weijmans, Anne Marie and Westfall, Kyle B}, -doi = {10.1093/mnras/sty653}, -eprint = {1803.03604}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: General,Gravitational lensing: Strong}, -number = {1}, -pages = {195--209}, -title = {{SDSS-IV MaNGA: The spectroscopic discovery of strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1803.03604%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty653}, -volume = {477}, -year = {2018} -} -@article{Harvey2015, -abstract = {Collisions between galaxy clusters provide a test of the nongravitational forces acting on dark matter. Dark matter's lack of deceleration in the "bullet cluster" collision constrained its self-interaction cross section $\sigma$DM/m {\textless} 1.25 square centimeters per gram (cm2/g) [68{\%} confidence limit (CL)] ($\sigma$DM, self-interaction cross section; m, unit mass of dark matter) for long-ranged forces. Using the Chandra and Hubble Space Telescopes, we have now observed 72 collisions, including both major and minor mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6s significance. The position of the dark mass has remained closely aligned within 5.8 T 8.2 kiloparsecs of associated stars, implying a self-interaction cross section $\sigma$DM/m {\textless} 0.47 cm2/g (95{\%} CL) and disfavoring some proposed extensions to the standard model.}, -archivePrefix = {arXiv}, -arxivId = {1503.07675}, -author = {Harvey, David and Massey, Richard and Kitching, Thomas and Taylor, Andy and Tittley, Eric}, -doi = {10.1126/science.1261381}, -eprint = {1503.07675}, -issn = {10959203}, -journal = {Science}, -number = {6229}, -pages = {1462--1465}, -pmid = {25814581}, -title = {{The nongravitational interactions of dark matter in colliding galaxy clusters}}, -volume = {347}, -year = {2015} -} -@article{Buitrago2017a, -abstract = {Using the exquisite depth of the Hubble Ultra Deep Field (HUDF12 programme) data set, we explore the ongoing assembly of the outermost regions of the most massive galaxies (Mstellar ≥ 5× 1010 M) at z ≤ 1. The outskirts of massive objects, particularly early-type Galaxies (ETGs), are expected to suffer a dramatic transformation across cosmic time due to continuous accretion of small galaxies. HUDF imaging allows us to study this process at intermediate redshifts in six massive galaxies, exploring the individual surface brightness profiles out to ∼25 effective radii. We find that 5–20 per cent of the total stellar mass for the galaxies in our sample is contained within 10 {\textless} R {\textless} 50 kpc. These values are in close agreement with numerical simulations, and higher than those reported for local late-type galaxies (5 per cent). The fraction of stellar mass stored in the outer envelopes/haloes of massive ETGs increases with decreasing redshift, being 28.7 per cent at {\textless}z {\textgreater}= 0.1, 15.1 per cent at {\textless}z {\textgreater}= 0.65 and 3.5 per cent at {\textless}z {\textgreater}= 2. The fraction of mass in diffuse features linked with ongoing minor merger events is {\textgreater}1–2 per cent, very similar to predictions based on observed close pair counts. Therefore, the results for our small albeit meaningful sample suggest that the size and mass growth of the most massive galaxies have been solely driven by minor and major merging from z = 1 to today.}, -archivePrefix = {arXiv}, -arxivId = {1602.01846}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Curtis-Lake, Emma and Montes, Mireia and Cooper, Andrew P and Bruce, Victoria A and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Cirasuolo, Michele}, -doi = {10.1093/mnras/stw3382}, -eprint = {1602.01846}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: haloes,Galaxies: high-redshift,Galaxies: structure,cD}, -number = {4}, -pages = {4888--4903}, -title = {{The cosmic assembly of stellar haloes in massive early-type Galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3382}, -volume = {466}, -year = {2017} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of {\$\sim${}}1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Gadotti2008a, -abstract = {We have performed 2D bulge/bar/disc decompositions using g, r and i-band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for the bulge-to-total ratio than the global S{\'{e}}rsic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour-magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between the bulge S{\'{e}}rsic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass-size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass-size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0810.1953}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2008.14257.x}, -eprint = {0810.1953}, -isbn = {0372-9311 (Print)$\backslash$r0372-9311 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {1531--1552}, -pmid = {20063786}, -title = {{Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: A Sloan Digital Sky Survey perspective}}, -url = {http://arxiv.org/abs/0810.1953%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2008.14257.x}, -volume = {393}, -year = {2009} -} -@article{Cohen2018, -abstract = {We present HST/ACS imaging of twenty-three very low surface brightness ({\$}\backslashmu{\_}{\{}e,V{\}}{\$}=25-27.5) galaxies detected in the fields of four nearby galaxy groups. These objects were selected from deep optical imaging obtained with the Dragonfly Telephoto Array. Seven are new discoveries, while most of the others had been identified previously in visual surveys of deep photographic plates and more recent surveys. Few have previously been studied in detail. From the ACS images, we measure distances to the galaxies using both the tip of the red giant branch method and the surface brightness fluctuations method. We demonstrate that the two methods are consistent with each other in the regime where both can be applied. The distances to 15 out of 20 galaxies with stable measurements are consistent with that of the targeted group within errors. This suggests that assuming group membership based solely on projected proximity is {\$\sim${}}75{\%} successful in this regime. The galaxies are nearly round, with a median axis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The objects have a range of sizes, from {\$}R{\_}e{\$}=0.4 kpc to {\$}R{\_}e{\$}=1.8 kpc, with a median of 1.0 kpc. They range in luminosity from {\$}M{\_}V{\$}=-11.4 to {\$}M{\_}V{\$}=-15.6, with a median of -12.4. Galaxies with {\$}R{\_}e{\$}{\$\sim${}}1 kpc and {\$}M{\_}V{\$}{\$\sim${}}-12 are fairly rare in the Local Group but we find many of them in this relatively small sample. Four of the objects fall in the class of ultra diffuse galaxies (UDGs), with {\$}R{\_}e{\$}{\textgreater}1.5 kpc and {\$}\backslashmu{\_}{\{}0,V{\}}{\$}{\textgreater}24 mag/arcsec{\^{}}2, including the recently identified dark matter deficient galaxy NGC1052-DF2.}, -archivePrefix = {arXiv}, -arxivId = {1807.06016}, -author = {Cohen, Yotam and van Dokkum, Pieter and Danieli, Shany and Romanowsky, Aaron J and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Mowla, Lamiya and Kruijssen, J M Diederik and Conroy, Charlie and Wasserman, Asher}, -doi = {10.3847/1538-4357/aae7c8}, -eprint = {1807.06016}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {Astrophysics,Astrophysics of Galaxies}, -number = {2}, -pages = {96}, -title = {{ The Dragonfly Nearby Galaxies Survey. V. HST /ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC 1052, NGC 1084, M96, and NGC 4258 }}, -url = {http://arxiv.org/abs/1807.06016%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aae7c8}, -volume = {868}, -year = {2018} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a $\Lambda$CDM concordance cosmology. To that extent we use a large N-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as a function of halo mass and galaxy colour. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by ∼40° (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the colour of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the colour of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion. {\textcopyright}2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X and {Van Den Bosch}, Frank C and Yang, Xiaohu and Mao, Shude and Mo, H J and Li, Cheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@article{Morishita2018a, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {evolution,formation,galaxies,star formation}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Navarro1991, -abstract = {The dynamical evolution of both collisionless 'dark' particles and a dissipative gaseous component in a flat universe is simulated in order to investigate the formation process of the luminous components of galaxies at the center of galactic dark halos. The present models assume that the gas amounts to 10 percent of the mass of the universe, and that both the gas and the dark matter are identically distributed in phase space at high redshifts. The results confirm previous suggestions that the merging history of the surrounding halo is a key factor in the determination of a galaxy's morphological type. The baryonic component is found to lose more angular momentum than could be predicted by dissipationless simulations. The formation of dense, slowly rotating baryonic cores at the center of galactic dark halos is observed, which explains the origin of the slow rotation and large densities observed in spheroids and elliptical galaxies.}, -author = {Navarro, Julio F. and Benz, Willy}, -doi = {10.1086/170590}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Astronomical Models,Collisionless Plasmas,Computational Astrophysics,Cooling Flows (Astrophysics),Dark Matter,Elliptical Galaxies,Galactic Evolution,Galactic Rotation,Galactic Structure,Gas Dynamics,Halos}, -month = {oct}, -pages = {320}, -title = {{Dynamics of cooling gas in galactic dark halos}}, -volume = {380}, -year = {1991} -} -@article{Hall2014a, -abstract = {Charge-Coupled Devices are the detector of choice for the focal planes of many optical and X-ray space telescopes. In recent years, EM-CCDs, SCDs and CMOS sensors have been used, or baselined, for missions in which the detection of X-ray and visible photons are key to the science goals of the mission. When placed in orbit, silicon-based detectors will suffer radiation damage as a consequence of the harsh space radiation environment, creating traps in the silicon. The radiation-induced traps will capture and release signal electrons, effectively "smearing" the image. Without correction, this smearing of the image would have major consequences on the science goals of the missions. Fitting to observed results, through careful planning of observation strategies while the radiation dose received remains low in the early stages of the mission, has previously been used to correct against the radiation damage effects. As the science goals becoming increasingly demanding, however, the correction algorithms require greater accuracy and a more physical approach is required, removing the effects of the radiation damage by modelling the trap capture and release mechanisms to a high level of detail. The drive for increasingly accurate trap parameters has led to the development of new methods of characterisation of traps in the silicon, measuring the trap properties and their effects to the single-trap level in situ. Here, we summarise the latest developments in trap characterisation techniques for n-channel and p-channel devices. ? 2014 SPIE.}, -author = {Hall, David J and Murray, Neil and Gow, Jason and Wood, Daniel and Holland, Andrew}, -doi = {10.1117/12.2055906}, -isbn = {9780819496225}, -issn = {1996756X 0277786X}, -journal = {Proceedings of SPIE - The International Society for Optical Engineering}, -keywords = {CTI,Defect,Euclid,Gaia,HST,N-channel,P,[CCD}, -number = {0}, -pages = {915408}, -title = {{{\textless}i{\textgreater}In situ{\textless}/i{\textgreater}trap parameter studies in CCDs for space applications}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2055906}, -volume = {9154}, -year = {2014} -} -@article{Massey2014, -abstract = {Charge-coupled device (CCD) detectors, widely used to obtain digital imaging, can be damaged by high energy radiation. Degraded images appear blurred, because of an effect known as Charge Transfer Inefficiency (CTI), which trails bright objects as the image is read out. It is often possible to correct most of the trailing during post-processing, by moving flux back to where it belongs. We compare several popular algorithms for this: quantifying the effect of their physical assumptions and tradeoffs between speed and accuracy. We combine their best elements to construct a more accurate model of damaged CCDs in the Hubble Space Telescope's Advanced Camera for Surveys/Wide Field Channel, and update it using data up to early 2013. Our algorithm now corrects 98 per cent of CTI trailing in science exposures, a substantial improvement over previous work. Further progress will be fundamentally limited by the presence of read noise. Read noise is added after charge transfer so does not get trailed-but it is incorrectly untrailed during post-processing. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1401.1151}, -author = {Massey, Richard and Schrabback, Tim and Cordes, Oliver and Marggraf, Ole and Israel, Holger and Miller, Lance and Hall, David and Cropper, Mark and Prod'homme, Thibaut and Niemi, Sami Matias}, -doi = {10.1093/mnras/stu012}, -eprint = {1401.1151}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Massey et al. - 2014 - An improved model of charge transfer inefficiency and correction algorithm for the Hubble Space Telescope.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Instrumentation: Detectors,Methods: Data analysis,Space vehicles: Instruments}, -month = {mar}, -number = {1}, -pages = {887--907}, -title = {{An improved model of charge transfer inefficiency and correction algorithm for the Hubble Space Telescope}}, -url = {http://arxiv.org/abs/1401.1151}, -volume = {439}, -year = {2014} -} -@article{Salucci2019, -abstract = {The distribution of the non-luminous matter in galaxies of different luminosity and Hubble type is much more than a proof of the existence of dark particles governing the structures of the Universe. Here, we will review the complex but well-ordered scenario of the properties of the dark halos also in relation with those of the baryonic components they host. Moreover, we will present a number of tight and unexpected correlations between selected properties of the dark and the luminous matter. Such entanglement evolves across the varying properties of the luminous component and it seems to unequivocally lead to a dark particle able to interact with the Standard Model particles over cosmological times. This review will also focus on whether we need a paradigm shift, from pure collisionless dark particles emerging from “first principles”, to particles that we can discover only by looking to how they have designed the structure of the galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1811.08843}, -author = {Salucci, Paolo}, -doi = {10.1007/s00159-018-0113-1}, -eprint = {1811.08843}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Salucci - 2019 - The distribution of dark matter in galaxies.pdf:pdf}, -issn = {09354956}, -journal = {Astronomy and Astrophysics Review}, -keywords = {Cosmology,Dark matter,Elementary particles,Galaxies}, -number = {1}, -title = {{The distribution of dark matter in galaxies}}, -volume = {27}, -year = {2019} -} -@article{Li2008, -abstract = { We report the discovery that substructures/subhaloes of a galaxy-size halo tend to fall in together in groups in cosmological simulations, something that may explain the oddity of the MW satellite distribution. The original clustering at the time of infall is still discernible in the angular momenta of the subhaloes even for events which took place up to eight Gyrs ago, z {\$\sim${}} 1. This phenomenon appears to be rather common since at least 1/3 of the present-day subhaloes have fallen in groups in our simulations. Hence, this may well explain the Lynden-Bell {\&} Lynden-Bell ghostly streams. We have also found that the probability of building up a flattened distribution similar to the MW satellites is as high as {\$\sim${}} 80{\%} if the MW satellites were from only one group and {\$\sim${}} 20{\%} when five groups are involved. Therefore, we conclude that the ‘peculiar' distribution of satellites around the MW can be expected with the CDM structure formation theory. This non-random assignment of satellites to subhaloes implies an environmental dependence on whether these low-mass objects are able to form stars, possibly related to the nature of reionization in the early Universe. }, -archivePrefix = {arXiv}, -arxivId = {0807.2780}, -author = {Li, Yang Shyang and Helmi, Amina}, -doi = {10.1007/978-1-4020-5573-7_53}, -eprint = {0807.2780}, -isbn = {0000000000000}, -issn = {15706605}, -journal = {Astrophysics and Space Science Proceedings}, -keywords = {Dark matter,Galaxies: Dwarf,Galaxies: Kinematics and dynamics,Galaxy: Formation,Methods: Numerical}, -number = {202409}, -pages = {311--314}, -title = {{Infall of substructures onto a milky way-like dark halo}}, -volume = {385}, -year = {2007} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of Mstar{\textgreater}10{\^{}}11Msolar galaxies at 1{\textless}z{\textless}3 in the CANDELS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disk components according to their H(160)-band morphologies. By extending this analysis to multiple bands we have been able to conduct individual bulge and disk component SED fitting which has provided us with stellar-mass and star-formation rate estimates for the separate bulge and disk components. These have been combined with size measurements to explore the evolution of these massive high-redshift galaxies. By utilising the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the disks. This can be seen from both the fraction of bulge components which lie below the local relation and the median sizes of the bulge components, where the bulges are a median factor of 2.93+/-0.32 times smaller than similarly massive local galaxies at 1{\textless}z{\textless}2 and 3.41+/-0.58 smaller at 2{\textless}z{\textless}3; for the disks the corresponding factors are 1.65+/-0.14 and 1.99+/-0.25. Moreover, by splitting our sample into the passive and star-forming bulge and disk sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming disks are larger, while the passive disks have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-Sersic fits and adopting the overall star-formation rates. Finally, by evolving the star-formation histories of the passive disks back to the redshifts when the passive disks were last active, we show that the passive and star-forming disks have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.5221}, -volume = {444}, -year = {2014} -} -@article{Pope2006, -abstract = {We present spectral energy distributions (SEDs), Spitzer colours, and infrared (IR) luminosities for 850- $\mu$m selected galaxies in the Great Observatories Origins Deep Survey Northern (GOODS-N) field. Using the deep Spitzer Legacy images and new data and reductions of the Very Large knay-Hubble Deep Field (VLA-HDF) radio data, we find statistically secure counterparts for 60 per cent (21/35) of our submillimetre (submm) sample, and identify tentative counterparts for another 12 objects. This is the largest sample of submm galaxies with statistically secure counterparts detected in the radio and with Spitzer. Half of the secure counterparts have spectroscopic redshifts, while the other half have photometric redshifts. We find that in most cases the 850- $\mu$m emission is dominated by a single 24-$\mu$m source, with a median flux density of 241 $\mu$Jy, leading to a median 24-to-850-$\mu$m flux density ratio of 0.040. A composite rest-frame SED shows that the submm sources peak at longer wavelengths than those of local ultraluminous infrared galaxies (ULIRGs). Using a basic grey-body model, 850-$\mu$m selected galaxies appear to be cooler than local ULIRGs of the same luminosity. This demonstrates the strong selection effects, both locally and at high redshift, which may lead to an incomplete census of the ULIRG population. The SEDs of submm galaxies are also different from those of their high-redshift neighbours, the near-IR selected BzK galaxies, whose mid-IR-to-radio SEDs are more like those of local ULIRGs. Using 24-$\mu$m, 850-$\mu$am and 1.4-GHz observations, we fit templates that span the mid-IR through radio to derive the integrated IR luminosity (LIR) of the submm galaxies and find a median value of L IR(8-1000 $\mu$m) = 6.0 × 10 12 LȮ. By themselves, 24-$\mu$m and radio fluxes are able to predict L IR reasonably well because they are relatively insensitive to temperature. However, the submm flux by itself consistently overpredicts L IR when using spectral templates which obey the local ULIRG temperature-luminosity relation. The shorter Spitzer wavelengths sample the stellar bump at the redshifts of the submm sources, and we find that the Spitzer photometry alone provides a model-independent estimate of the redshift, $\sigma$[$\Delta$z/(1 + z)] = 0.07. The median redshift for our secure submm counterparts is 2.0. Using X-ray and mid-IR data, only 5 per cent of our secure counterparts (1/21) show strong evidence for an active galactic nucleus dominating the LIR. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0605573}, -author = {Pope, Alexandra and Scott, Douglas and Dickinson, Mark and Chary, Ranga Ram and Morrison, Glenn and Borys, Colin and Sajina, Anna and Alexander, David M. and Daddi, Emanuele and Frayer, David and MacDonald, Emily and Stern, Daniel}, -doi = {10.1111/j.1365-2966.2006.10575.x}, -eprint = {0605573}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: starburst,Infrared: galaxies,Submillimetre}, -number = {3}, -pages = {1185--1207}, -pmid = {367060}, -primaryClass = {astro-ph}, -title = {{The Bubble Deep Field-North SCUBA Super-map - IV. Characterizing submillimetre galaxies using deep Spitzer imaging}}, -volume = {370}, -year = {2006} -} -@article{Hopkins2009, -abstract = {Transformation of discs into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that the bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in haloes according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the overproduction of spheroids: low- and intermediate-mass galaxies are predicted to be bulge-dominated (B/T ∼ 0.5 at {\textless}10 10 M ⊙, with almost no 'bulgeless' systems), even if they have avoided major mergers. Including the different physical behaviour of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T ∼ 0.1 at {\textless}10 10 M ⊙, with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behaviour of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4111}, -author = {Hopkins, Philip F and Somerville, Rachel S and Cox, Thomas J and Hernquist, Lars and Jogee, Shardha and Kere{\v{s}}, Dusan and Ma, Chung Pei and Robertson, Brant and Stewart, Kyle}, -doi = {10.1111/j.1365-2966.2009.14983.x}, -eprint = {0901.4111}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Galaxies: spiral}, -number = {2}, -pages = {802--814}, -title = {{The effects of gas on morphological transformation in mergers: Implications for bulge and disc demographics}}, -volume = {397}, -year = {2009} -} -@article{Yang2006, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C. and Mo, H. J. and Mao, Shude and Kang, Xi and Weinmann, Simone M. and Guo, Yicheng and Jing, Y. P.}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yang et al. - 2006 - The alignment between the distribution of satellites and the orientation of their central galaxy.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the fore-ground lenses and background sources are early-type galaxies. Using imaging from HST/ACS and Keck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population of massive, compact galaxies at redshifts 0.4 z 0.7, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of high-redshift red nuggets or their partly-evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar pop-ulations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S{\'{e}}rsic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still com-pact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterised by red-to-blue colour gradients as a function of radius which are stronger at low redshift – indicative of ongoing accretion – but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are predominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W and Fassnacht, Christopher D and Treu, Tommaso and Brewer, Brendon J and Koopmans, L V E and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Cyr-Racine2019, -abstract = {Gravitational lensing has emerged as a powerful probe of the matter distribution on subgalactic scales, which itself may contain important clues about the fundamental origins and properties of dark matter. Broadly speaking, two different approaches have been taken in the literature to map the small-scale structure of the Universe using strong lensing, with one focused on measuring the position and mass of a small number of discrete massive subhalos appearing close in projection to lensed images, and the other focused on detecting the collective effect of all the small-scale structure between the lensed source and the observer. In this paper, we follow the latter approach and perform a detailed study of the sensitivity of galaxy-scale gravitational lenses to the ensemble properties of small-scale structure. As in some previous studies, we adopt the language of the substructure power spectrum to characterize the statistical properties of the small-scale density field. We present a comprehensive theory that treats lenses with extended sources as well as those with time-dependent compact sources (such as quasars) in a unified framework for the first time. Our approach uses mode functions to provide both computational advantages and insights about couplings between the lens and source. The goal of this paper is to develop the theory and gain the intuition necessary to understand how the sensitivity to the substructure power spectrum depends on the source and lens properties, with the eventual aim of identifying the most promising targets for such studies.}, -archivePrefix = {arXiv}, -arxivId = {1806.07897}, -author = {Cyr-Racine, Francis-Yan and Keeton, Charles R and Moustakas, Leonidas A}, -doi = {10.1103/physrevd.100.023013}, -eprint = {1806.07897}, -issn = {2470-0010}, -journal = {Physical Review D}, -number = {2}, -pages = {1--30}, -title = {{Beyond subhalos: Probing the collective effect of the Universe's small-scale structure with gravitational lensing}}, -volume = {100}, -year = {2019} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series that re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science data base, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies. This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution that limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ('encounter-driven') rings (such as ring and polar ring galaxies) are recognized in less than 1 per cent of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{2001ex, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Greene2015, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless} $\sigma$∗ {\textless} 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Amorisco:2017aa, -abstract = {The accreted component of stellar halos is composed of the contributions of several satellites, falling onto their host with their different masses, at different times, on different orbits. This work uses a suite of idealised, collisionless N-body simulations of minor mergers and a particle tagging technique to understand how these different ingredients shape each contribution to the accreted halo, in both density and kinematics. I find that more massive satellites deposit their stars deeper into the gravitational potential of the host, with a clear segregation enforced by dynamical friction. Earlier accretion events contribute more to the inner regions of the halo; more concentrated subhaloes sink deeper through increased dynamical friction. The orbital circularity of the progenitor at infall is only important for low-mass satellites: dynamical friction efficiently radialises the most massive minor mergers erasing the imprint of the infall orbit for satellite-to-host virial mass ratios {\$}\backslashgtrsim1/20{\$}. The kinematics of the stars contributed by each satellite is also ordered with satellite mass: low-mass satellites contribute fast-moving populations, in both ordered rotation and radial velocity dispersion. In turn, contributions by massive satellites have lower velocity dispersion and lose their angular momentum to dynamical friction, resulting in a strong radial anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {1511.08806}, -author = {Amorisco, N C}, -doi = {10.1093/mnras/stw2229}, -eprint = {1511.08806}, -journal = {$\backslash$mnras}, -month = {jan}, -pages = {2882--2895}, -title = {{Contributions to the accreted stellar halo: an atlas of stellar deposition}}, -url = {http://arxiv.org/abs/1511.08806%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2229}, -volume = {464}, -year = {2015} -} -@article{Birrer2018, -abstract = {We present a blind time-delay strong lensing (TDSL) cosmographic analysis of the doubly imaged quasar SDSS 1206+4332. We combine the relative time delay between the quasar images, Hubble Space Telescope imaging, the Keck stellar velocity dispersion of the lensing galaxy, and wide-field photometric and spectroscopic data of the field to constrain two angular diameter distance relations. The combined analysis is performed by forward modelling the individual data sets through a Bayesian hierarchical framework, and it is kept blind until the very end to prevent experimenter bias. After unblinding, the inferred distances imply a Hubble constant {\$}H{\_}0 = 68.8{\^{}}{\{}+5.4{\}}{\_}{\{}-5.1{\}}{\$} kms{\$}{\^{}}{\{}-1{\}}{\$}Mpc{\$}{\^{}}{\{}-1{\}}{\$}, assuming a flat Lambda cold dark matter cosmology with uniform prior on {\$}\backslashOmega{\_}{\{}\backslashrm m{\}}{\$} in [0.05, 0.5]. The precision of our cosmographic measurement with the doubly imaged quasar SDSS 1206+4332 is comparable with those of quadruply imaged quasars and opens the path to perform on selected doubles the same analysis as anticipated for quads. Our analysis is based on a completely independent lensing code than our previous three H0LiCOW systems and the new measurement is fully consistent with those. We provide the analysis scripts paired with the publicly available software to facilitate independent analysis. The consistency between blind measurements with independent codes provides an important sanity check on lens modelling systematics. By combining the likelihoods of the four systems under the same prior, we obtain {\$}H{\_}0 = 72.5{\^{}}{\{}+2.1{\}}{\_}{\{}-2.3{\}}{\$}kms{\$}{\^{}}{\{}-1{\}}{\$}Mpc{\$}{\^{}}{\{}-1{\}}{\$}. This measurement is independent of the distance ladder and other cosmological probes.}, -archivePrefix = {arXiv}, -arxivId = {1809.01274}, -author = {Birrer, S and Treu, T and Rusu, C E and Bonvin, V and Fassnacht, C D and Chan, J H H and Agnello, A and Shajib, A J and Chen, G C F and Auger, M and Courbin, F and Hilbert, S and Sluse, D and Suyu, S H and Wong, K C and Marshall, P and Lemaux, B C and Meylan, G}, -doi = {10.1093/mnras/stz200}, -eprint = {1809.01274}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmological parameters,dark energy,ravitational lensing: strong}, -number = {4}, -pages = {4726--4753}, -title = {{H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant}}, -url = {http://arxiv.org/abs/1809.01274}, -volume = {484}, -year = {2019} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo > 1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from $\sim$30° to 10° for M $\sim$ 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tenneti et al. - 2014 - Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@article{Ravasi2019, -abstract = {Linear operators and optimisation are at the core of many algorithms used in signal and image processing, remote sensing, and inverse problems. For small to medium-scale problems, existing software packages (e.g., MATLAB, Python numpy and scipy) allow for explicitly building dense (or sparse) matrices and performing algebraic operations (e.g., computation of matrix-vector products and manipulation of matrices) with syntax that closely represents their corresponding analytical forms. However, many real application, large-scale operators do not lend themselves to explicit matrix representations, usually forcing practitioners to forego of the convenient linear-algebra syntax available for their explicit-matrix counterparts. PyLops is an open-source Python library providing a flexible and scalable framework for the creation and combination of so-called linear operators, class-based entities that represent matrices and inherit their associated syntax convenience, but do not rely on the creation of explicit matrices. We show that PyLops operators can dramatically reduce the memory load and CPU computations compared to explicit-matrix calculations, while still allowing users to seamlessly use their existing knowledge of compact matrix-based syntax that scales to any problem size because no explicit matrices are required.}, -archivePrefix = {arXiv}, -arxivId = {1907.12349}, -author = {Ravasi, Matteo and Vasconcelos, Ivan}, -eprint = {1907.12349}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ravasi, Vasconcelos - 2019 - PyLops -- A Linear-Operator Python Library for large scale optimization.pdf:pdf}, -journal = {Software X}, -number = {100361}, -title = {{PyLops -- A Linear-Operator Python Library for large scale optimization}}, -url = {https://doi.org/10.1016/j.softx.2019.100361}, -volume = {11}, -year = {2019} -} -@article{Moore2018, -abstract = {The next generation of giant-segmented mirror telescopes (>20 m) will enable us to observe galactic nuclei at much higher angular resolution and sensitivity than ever before. These capabilities will introduce a revolutionary shift in our understanding of the origin and evolution of supermassive black holes by enabling more precise black hole mass measurements in a mass range that is unreachable today. We present simulations and predictions of the observations of nuclei that will be made with the Thirty Meter Telescope (TMT) and the adaptive optics assisted integral-field spectrograph IRIS, which is capable of diffraction-limited spectroscopy from Z band (0.9 $\mu$m) to K band (2.2 $\mu$m). These simulations, for the first time, use realistic values for the sky, telescope, adaptive optics system, and instrument to determine the expected signal-to-noise ratio of a range of possible targets spanning intermediate mass black holes of 104 M⊙to the most massive black holes known today of >1010 M ⊙. We find that IRIS will be able to observe Milky Way mass black holes out the distance of the Virgo Cluster, and will allow us to observe many more of the brightest cluster galaxies where the most massive black holes are thought to reside. We also evaluate how well the kinematic moments of the velocity distributions can be constrained at the different spectral resolutions and plate scales designed for IRIS. We find that a spectral resolution of 8000 will be necessary to measure the masses of intermediate mass black holes. By simulating the observations of galaxies found in Sloan Digital Sky Survey DR7, we find that over 105 massive black holes will be observable at distances between 0.005 < z < 0.18 with the estimated sensitivity and angular resolution provided by access to Z-band (0.9 $\mu$m) spectroscopy from IRIS and the TMT adaptive optics system. These observations will provide the most accurate dynamical measurements of black hole masses to enable the study of the demography of massive black holes, address the origin of the M BH-$\sigma$ and M BH-L relationships, and evolution of black holes through cosmic time. {\textcopyright} 2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1401.7988}, -author = {Do, Tuan and Wright, Shelley A. and Barth, Aaron J. and Barton, Elizabeth J. and Simard, Luc and Larkin, James E. and Moore, Anna M. and Wang, Lianqi and Ellerbroek, Brent}, -doi = {10.1088/0004-6256/147/4/93}, -eprint = {1401.7988}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Do et al. - 2014 - Prospects for measuring supermassive black hole masses with future extremely large telescopes.pdf:pdf}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {adaptive opticsinstrumentation,galaxies,imaging spectroscopytelescopes,kinematics and dynamicsinstrumentation,spectrographstechniques}, -number = {4}, -pages = {1--19}, -title = {{Prospects for measuring supermassive black hole masses with future extremely large telescopes}}, -volume = {147}, -year = {2014} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print)$\backslash$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Roy2018, -abstract = {We have obtained structural parameters of about 340 000 galaxies from the Kilo-Degree Survey (KiDS) in 153 deg2 of data release 1, 2, and 3.We have performed a seeing convolved 2D single S{\'{e}}rsic fit to the galaxy images in the four photometric bands (u, g, r, i) observed by KiDS, by selecting high signal-to-noise ratio (S/N > 50) systems in every bands. We have classified galaxies as spheroids and disc-dominated by combining their spectral energy distribution properties and their S{\'{e}}rsic index. Using photometric redshifts derived from a machine learning technique, we have determined the evolution of the effective radius, Re and stellar mass, M*, versus redshift, for both mass complete samples of spheroids and discdominated galaxies up to z$\sim$0.6. Our results show a significant evolution of the structural quantities at intermediate redshift for the massive spheroids (logM*/M⊙ > 11, Chabrier IMF), while almost no evolution has found for less massive ones (logM*/M⊙ < 11). On the other hand, disc dominated systems show a milder evolution in the less massive systems (logM*/M⊙ < 11) and possibly no evolution of the more massive systems. These trends are generally consistent with predictions from hydrodynamical simulations and independent datasets out to redshift z $\sim$ 0.6, although in some cases the scatter of the data is large to drive final conclusions. These results, based on 1/10 of the expected KiDS area, reinforce precedent finding based on smaller statistical samples and show the route towards more accurate results, expected with the the next survey releases.}, -archivePrefix = {arXiv}, -arxivId = {1807.06085}, -author = {Roy, N. and Napolitano, N. R. and {La Barbera}, F. and Tortora, C. and Getman, F. and Radovich, M. and Capaccioli, M. and Brescia, M. and Cavuoti, S. and Longo, G. and Raj, M. A. and Puddu, E. and Covone, G. and Amaro, V. and Vellucci, C. and Grado, A. and Kuijken, K. and {Verdoes Kleijn}, G. and Valentijn, E.}, -doi = {10.1093/mnras/sty1917}, -eprint = {1807.06085}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Roy et al. - 2018 - Evolution of galaxy size-stellar mass relation from the Kilo-Degree Survey(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution}, -number = {1}, -pages = {1057--1080}, -title = {{Evolution of galaxy size-stellar mass relation from the Kilo-Degree Survey}}, -volume = {480}, -year = {2018} -} -@article{Wertz2018, -abstract = {The modern time-delay cosmography aims to infer the cosmological parameters with a competitive precision from observing a multiply imaged quasar. The success of this technique relies upon a robust modeling of the lens mass distribution. Unfortunately strong degeneracies between density profiles that lead to almost the same lensing observables may bias precise estimate for the Hubble constant. The source position transformation (SPT), which covers the well-known mass sheet transformation (MST) as a special case, defines a new framework to investigate these degeneracies. In this paper, we present pySPT, a Python package dedicated to the SPT. We describe how it can be used to evaluate the impact of the SPT on lensing observables. We review most of its capabilities and elaborate on key features that we used in a companion paper regarding SPT and time delays. pySPT also comes with a sub-package dedicated to simple lens modeling. It can be used to generate lensing related quantities for a wide variety of lens models, independently from any SPT analysis. As a first practical application, we present a correction to the first estimate of the impact on time delays of the SPT, which has been experimentally found in Schneider and Sluse (2013) between a softened power-law and a composite (baryons + dark matter) lenses. We find that the large deviations predicted in Schneider and Sluse (2014) have been overestimated due to a minor bug (now fixed) in the public lens modeling code lensmodel (v1.99). We conclude that the predictions for the Hubble constant deviate by {\$}\backslashsim 7{\$}$\backslash${\%}, first and foremost caused by an MST. The latest version of pySPT is available at https://github.com/owertz/pySPT. We also provide tutorials to describe in detail how making the best use of pySPT at https://github.com/owertz/pySPT{\_}tutorials.}, -archivePrefix = {arXiv}, -arxivId = {1801.04151}, -author = {Wertz, Olivier and Orthen, Bastian}, -doi = {10.1051/0004-6361/201732242}, -eprint = {1801.04151}, -keywords = {cosmological parameters,gravitational lensing,strong}, -pages = {1--9}, -title = {{pySPT: a package dedicated to the source position transformation}}, -url = {http://arxiv.org/abs/1801.04151%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201732242}, -year = {2018} -} -@article{Blei2017a, -abstract = {One of the core problems of modern statistics is to approximate difficult-to-compute probability densities. This problem is especially important in Bayesian statistics, which frames all inference about unknown quantities as a calculation involving the posterior density. In this article, we review variational inference (VI), a method from machine learning that approximates probability densities through optimization. VI has been used in many applications and tends to be faster than classical methods, such as Markov chain Monte Carlo sampling. The idea behind VI is to first posit a family of densities and then to find a member of that family which is close to the target density. Closeness is measured by Kullback–Leibler divergence. We review the ideas behind mean-field variational inference, discuss the special case of VI applied to exponential family models, present a full example with a Bayesian mixture of Gaussians, and derive a variant that uses stochastic optimization to scale up to massive data. We discuss modern research in VI and highlight important open problems. VI is powerful, but it is not yet well understood. Our hope in writing this article is to catalyze statistical research on this class of algorithms. Supplementary materials for this article are available online.}, -archivePrefix = {arXiv}, -arxivId = {1601.00670}, -author = {Blei, David M and Kucukelbir, Alp and McAuliffe, Jon D}, -doi = {10.1080/01621459.2017.1285773}, -eprint = {1601.00670}, -issn = {1537274X}, -journal = {Journal of the American Statistical Association}, -keywords = {Algorithms,Computationally intensive methods,Statistical computing}, -number = {518}, -pages = {859--877}, -title = {{Variational Inference: A Review for Statisticians}}, -volume = {112}, -year = {2017} -} -@article{Du2019, -abstract = {We develop an analytic mass model for lensing galaxies, based on a broken power-law (BPL) density profile, which is a power-law profile with a mass deficit or surplus in the central region. Under the assumption of an elliptically symmetric surface mass distribution, the deflection angle and magnification can be evaluated analytically for this new model. We compute the theoretical prediction for various quantities, including the volume and surface mass density profiles of the galaxies, and the aperture and luminosity-weighted line-of-sight velocity dispersions, and compare them to those measured from the Illustris simulation. We find an excellent agreement between our model prediction and the simulation, which validates our modeling. The high efficiency and accuracy of our model manifests itself as a promising tool for studying properties of galaxies with strong lensing.}, -archivePrefix = {arXiv}, -arxivId = {1911.11761}, -author = {Du, Wei and Zhao, Gong-Bo and Fan, Zuhui and Shu, Yiping and Li, Ran and Mao, Shude}, -doi = {10.3847/1538-4357/ab7a15}, -eprint = {1911.11761}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Du et al. - 2020 - An Accurate Analytic Mass Model for Lensing Galaxies.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {dark matter,galaxies,gravitational lensing,halos,kinematics and dynamics}, -number = {1}, -pages = {62}, -title = {{An Accurate Analytic Mass Model for Lensing Galaxies}}, -url = {http://arxiv.org/abs/1911.11761}, -volume = {892}, -year = {2020} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos and predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of {\$}50{\$} keV {\$}\backslashbackslashlesssim m c{\^{}}2 \backslashbackslashlesssim 345{\$} keV, can be an alternative interpretation of the central compact object in Sgr A*. We present in this work the gravitational lensing properties of this novel DM model in Milky Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the Non-Singular Isothermal Sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, {\$}m c{\^{}}2\backslashbackslashapprox 10{\^{}}{\{}2{\}}{\$} keV, we draw the following conclusions. At distances {\$}r\backslashbackslashgtrsim 20{\$} pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. We show that at distances {\$}\backslashbackslashsim 10{\^{}}{\{}-4{\}}{\$} pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances {\$}r\backslashbackslashlesssim 10{\^{}}{\{}-6{\}}{\$} pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used. We find that quantum DM cores do not show a photon sphere what implies that they do not cast a shadow. Similar conclusions apply to the other DM distributions for other fermion masses in the above specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Diemer2018, -abstract = {This paper introduces Colossus, a public, open-source python package for calculations related to cosmology, the large-scale structure (LSS) of matter in the universe, and the properties of dark matter halos. The code is designed to be fast and easy to use, with a coherent, well-documented user interface. The cosmology module implements Friedman-Lemaitre-Robertson-Walker cosmologies including curvature, relativistic species, and different dark energy equations of state, and provides fast computations of the linear matter power spectrum, variance, and correlation function. The LSS module is concerned with the properties of peaks in Gaussian random fields and halos in a statistical sense, including their peak height, peak curvature, halo bias, and mass function. The halo module deals with spherical overdensity radii and masses, density profiles, concentration, and the splashback radius. To facilitate the rapid exploration of these quantities, Colossus implements more than 40 different fitting functions from the literature. I discuss the core routines in detail, with particular emphasis on their accuracy. Colossus is available at bitbucket.org/bdiemer/colossus.}, -archivePrefix = {arXiv}, -arxivId = {1712.04512}, -author = {Diemer, Benedikt}, -doi = {10.3847/1538-4365/aaee8c}, -eprint = {1712.04512}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Diemer - 2018 - COLOSSUS A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos.pdf:pdf}, -issn = {0067-0049}, -journal = {ApJS}, -keywords = {cosmology,cosmology: theory,methods,methods: numerical,numerical,theory}, -number = {2}, -pages = {35}, -publisher = {IOP Publishing}, -title = {{COLOSSUS: A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos}}, -url = {http://dx.doi.org/10.3847/1538-4365/aaee8c}, -volume = {239}, -year = {2018} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10^12.5 h^-1 M_sun < M_200b < 10^15 h^-1 M_sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that $\sim$ 70% of galaxies with stellar mass M_* > 10^11 h^-2 M_sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The $\sim$ 30% of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20\% level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J. E. and Leauthaud, A. and Emsellem, E. and Ge, J. and Arag{\'{o}}n-Salamanca, A. and Greco, J. and Lin, Y.-T. and Mao, S. and Masters, K. and Merrifield, M. and More, S. and Okabe, N. and Schneider, D. P. and Thomas, D. and Wake, D. A. and Pan, K. and Bizyaev, D. and Oravetz, D. and Simmons, A. and Yan, R. and van den Bosch, F.}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2018 - SDSS-IV MaNGA Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S{\`{e}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as Mh(M*) ∝ reff$\eta$ (M*). We find that, on average, our lens galaxies have an $\eta$ = 0.42 ± 0.12, i.e. larger galaxies live in more massive dark matter haloes. The $\eta$ is strongest for high-mass luminous red galaxies. Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed M*, satellite galaxies have a larger $\eta$ and greater scatter in the Mh and reff relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J L and Hudson, Michael J and Balogh, Michael L and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Pontzen2015a, -abstract = {Galaxies and the dark matter halos that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealised calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter core-creation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are "maximally stable", i.e. that do not evolve at first order when external potentials (which arise from baryons, large scale tidal fields or infalling substructure) are applied. We show that a spherically-symmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for near-isotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealised spherically-symmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter halos (formed in collisionless cosmological simulations) nearly attain our maximally-stable limit, but their evolution freezes out before reaching it.}, -archivePrefix = {arXiv}, -arxivId = {1502.07356}, -author = {Pontzen, Andrew and Read, Justin I and Teyssier, Romain and Governato, Fabio and Gualandris, Alessia and Roth, Nina and Devriendt, Julien}, -doi = {10.1093/mnras/stv1032}, -eprint = {1502.07356}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {1366--1379}, -title = {{Milking the spherical cow - on aspherical dynamics in spherical coordinates}}, -volume = {451}, -year = {2015} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ({\$}z = 1.489{\$}), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5{\$}+{\$}2223 ({\$}z = 0.542{\$}), published by Grillo et al. (2016), and explore different {\$}\backslashLambda{\$}CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of {\$}H{\_}{\{}0{\}}{\$} and {\$}\backslashOmega{\_}{\{}\backslashrm m{\}}{\$} with relative (1{\$}\backslashsigma{\$}) statistical errors of, respectively, 6{\%} (7{\%}) and 31{\%} (26{\%}) in flat (general) cosmological models, assuming a conservative 3{\%} uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of {\$}H{\_}{\{}0{\}}{\$}, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C and Rosati, P and Suyu, S H and Balestra, I and Caminha, G B and Halkola, A and Kelly, P L and Lombardi, M and Mercurio, A and Rodney, S A and Treu, T}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -number = {2}, -pages = {94}, -title = {{Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”}}, -url = {http://arxiv.org/abs/1802.01584}, -volume = {860}, -year = {2018} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series that re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science data base, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies. This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution that limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ('encounter-driven') rings (such as ring and polar ring galaxies) are recognized in less than 1 per cent of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J.}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buta - 2017 - Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database(2).pdf:pdf}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{Gomer2018, -abstract = {The positions of multiple images in galaxy lenses are related to the galaxy mass distribution. Smooth elliptical mass profiles were previously shown to be inadequate in reproducing the quad population. In this paper, we explore the deviations from such smooth elliptical mass distributions. Unlike most other work, we use a model-free approach based on the relative polar image angles of quads, and their position in 3D space with respect to the Fundamental Surface of Quads. The FSQ is defined by quads produced by elliptical lenses. We have generated thousands of quads from synthetic populations of lenses with substructure consistent with {\$}\backslashLambda{\$}CDM simulations, and found that such perturbations are not sufficient to match the observed distribution of quads relative to the FSQ. The result is unchanged even when subhalo masses are increased by a factor of ten, and the most optimistic lensing selection bias is applied. We then produce quads from galaxies created using two components, representing baryons and dark matter. The transition from the mass being dominated by baryons in inner radii to being dominated by dark matter in outer radii can carry with it asymmetries, which would affect relative image angles. We run preliminary experiments using lenses with two elliptical mass components with nonidentical axis ratios and position angles, perturbations from ellipticity in the form of nonzero Fourier coefficients {\$}a{\_}4{\$} and {\$}a{\_}6{\$}, and artificially offset ellipse centers as a proxy for asymmetry at image radii. We show that combination of these effects is a promising way of accounting for quad population properties. We conclude that the quad population provides a unique and sensitive tool for constraining detailed mass distribution in the centers of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1712.07665}, -author = {Gomer, Matthew R and Williams, Liliya L R}, -doi = {10.1093/mnras/stx3294}, -eprint = {1712.07665}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1987--2002}, -title = {{The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses}}, -volume = {475}, -year = {2018} -} -@article{He2023a, -abstract = {Carcinoma of unknown primary (CUP) is a type of metastatic cancer with tissue-of-origin (TOO) unidentifiable by traditional methods. CUP patients typically have poor prognosis but therapy targeting the original cancer tissue can significantly improve patients' prognosis. Thus, it's critical to develop accurate computational methods to infer cancer TOO. While qPCR or microarray-based methods are effective in inferring TOO for most cancer types, the overall prediction accuracy is yet to be improved. In this study, we propose a cross-cohort computational framework to trace TOO of 32 cancer types based on RNA sequencing (RNA-seq). Specifically, we employed logistic regression models to select 80 genes for each cancer type to create a combined 1356-gene set, based on transcriptomic data from 9911 tissue samples covering the 32 cancer types with known TOO from the Cancer Genome Atlas (TCGA). The selected genes are enriched in both tissue-specific and tissue-general functions. The cross-validation accuracy of our framework reaches 97.50% across all cancer types. Furthermore, we tested the performance of our model on the TCGA metastatic dataset and International Cancer Genome Consortium (ICGC) dataset, achieving an accuracy of 91.09% and 82.67%, respectively, despite the differences in experiment procedures and pipelines. In conclusion, we developed an accurate yet robust computational framework for identifying TOO, which holds promise for clinical applications. Our code is available at http://github.com/wangbo00129/classifybysklearn .}, -author = {He, Binsheng and Sun, Hongmei and Bao, Meihua and Li, Haigang and He, Jianjun and Tian, Geng and Wang, Bo}, -doi = {10.1038/s41598-023-42465-8}, -file = {:C\:/Users/Jammy/Documents/Papers/Medical/He2023CUPFramework.pdf:pdf}, -isbn = {0123456789}, -issn = {20452322}, -journal = {Scientific Reports}, -number = {1}, -pages = {1--13}, -pmid = {37717102}, -publisher = {Nature Publishing Group UK}, -title = {{A cross-cohort computational framework to trace tumor tissue-of-origin based on RNA sequencing}}, -url = {https://doi.org/10.1038/s41598-023-42465-8}, -volume = {13}, -year = {2023} -} -@article{Blumenthal1986, -abstract = {Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in. radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.}, -author = {Blumenthal, G. R. and Faber, S. M. and Flores, R. and Primack, J. R.}, -doi = {10.1086/163867}, -isbn = {9781848000919}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Astronomical Models,Baryons,Galactic Evolution,Galactic Rotation,Galactic Structure,Gravitational Collapse,Halos,Interstellar Matter,Many Body Problem,Mass Distribution,Missing Mass (Astrophysics),Spiral Galaxies}, -month = {feb}, -pages = {27}, -title = {{Contraction of dark matter galactic halos due to baryonic infall}}, -url = {http://adsabs.harvard.edu/doi/10.1086/163867}, -volume = {301}, -year = {1986} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S.}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Guo et al. - 2016 - Deep learning for visual understanding A review(2).pdf:pdf}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{Geometryel, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful number of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag limit of ∼24. However, gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z ∼ 5-7 for LSST. We find that the LSST Wide Fast Deep survey could detect up to 120 lensed Population (Pop) I and II SNe but no lensed Pop III SNe. Deep-drilling programs in 10 deg2 fields could detect Pop I and II core-collapse SNe at AB magnitudes of 27-28 and 26, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes Erik and Whalen, Daniel J and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S}, -doi = {10.1093/mnras/stz3203}, -eprint = {1805.02662}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: dark ages,Cosmology: observations,First stars: early universe,Galaxies: high,Gravitational lensing: strong,Redshift,Reionization,Stars: Population III,Supernovae: general}, -number = {2}, -pages = {2447--2459}, -title = {{Detecting strongly lensed supernovae at z ∼ 5-7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {491}, -year = {2020} -} -@article{Gadotti2011, -abstract = {I present results from the modelling of stellar bars in nearly 300 barred galaxies in the local universe through parametric multicomponent multiband image fitting. The surface brightness radial profile of bars is described using a S{\'{e}}rsic function and parameters, such as the bar effective radius, ellipticity, boxiness, length and mass, and bar-to-total luminosity and mass ratios, are determined, which is unprecedented for a sample of this size. The properties of bars in galaxies with classical bulges and pseudo-bulges are compared. For a fixed bar-to-total mass ratio, pseudo-bulges are on average significantly less massive than classical bulges, indicating that, if pseudo-bulges are formed through bars, further processes are necessary to build a classical bulge. I find a correlation between bar ellipticity and boxiness, and define a new parameter as the product of these two quantities. I also find correlations between this product and the normalized bar size, between the sizes of bars and bulges, and between the normalized bar size and bulge-to-total ratio. Bars with different ellipticities follow parallel lines in the latter two correlations. These correlations can arise if, starting off with different normalized sizes and ellipticities, bars grow longer and stronger with dynamical age, as a result of angular momentum exchange between the inner and outer parts of galaxies, consistent with previous theoretical predictions. A plausible consequence is that bar pattern speeds should become lower with bar dynamical age and towards galaxies with more prominent bulges. {\textcopyright}2011 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1003.1719}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2011.18945.x}, -eprint = {1003.1719}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {3308--3318}, -title = {{Secular evolution and structural properties of stellar bars in galaxies}}, -volume = {415}, -year = {2011} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 {\textless} z {\textless} 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J{\textless}inf{\textgreater}125{\textless}/inf{\textgreater}, i{\textless}inf{\textgreater}814{\textless}/inf{\textgreater}, v{\textless}inf{\textgreater}606{\textless}/inf{\textgreater} HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.1736}, -volume = {444}, -year = {2014} -} -@article{Geometryef, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Tinker2013, -abstract = {We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2, 1.0]. For massive galaxies, M ≳ 1010.6 M , our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M ∼ 1010 M , the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1308.2974}, -author = {Tinker, Jeremy L. and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R. and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H.}, -doi = {10.1088/0004-637X/778/2/93}, -eprint = {1308.2974}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tinker et al. - 2013 - Evolution of the stellar-to-dark matter relation Separating star-forming and passive galaxies from z = 1 to 0.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: halos}, -number = {2}, -title = {{Evolution of the stellar-to-dark matter relation: Separating star-forming and passive galaxies from z = 1 to 0}}, -volume = {778}, -year = {2013} -} -@article{Newman2012, -abstract = {We describe the design and data analysis of the DEEP2 Galaxy Redshift Survey, the densest and largest high-precision redshift survey of galaxies at z ∼ 1 completed to date. The survey was designed to conduct a comprehensive census of massive galaxies, their properties, environments, and large-scale structure down to absolute magnitude MB = -20 at z ∼ 1 via ∼90 nights of observation on the Keck telescope. The survey covers an area of 2.8 deg2 divided into four separate fields observed to a limiting apparent magnitude of RAB = 24.1. Objects with z ≲ 0.7 are readily identifiable using BRI photometry and rejected in three of the four DEEP2 fields, allowing galaxies with z > 0.7 to be targeted ∼2.5 times more efficiently than in a purely magnitude-limited sample. Approximately 60% of eligible targets are chosen for spectroscopy, yielding nearly 53,000 spectra and more than 38,000 reliable redshift measurements. Most of the targets that fail to yield secure redshifts are blue objects that lie beyond z ∼ 1.45, where the [O II] 3727 {\AA} doublet lies in the infrared. The DEIMOS 1200 line mm-1 grating used for the survey delivers high spectral resolution (R ∼ 6000), accurate and secure redshifts, and unique internal kinematic information. Extensive ancillary data are available in the DEEP2 fields, particularly in the Extended Groth Strip, which has evolved into one of the richest multiwavelength regions on the sky. This paper is intended as a handbook for users of the DEEP2 Data Release 4, which includes all DEEP2 spectra and redshifts, as well as for the DEEP2 DEIMOS data reduction pipelines. Extensive details are provided on object selection, mask design, biases in target selection and redshift measurements, the spec2d two-dimensional data-reduction pipeline, the spec1d automated redshift pipeline, and the zspec visual redshift verification process, along with examples of instrumental signatures or other artifacts that in some cases remain after data reduction. Redshift errors and catastrophic failure rates are assessed through more than 2000 objects with duplicate observations. Sky subtraction is essentially photon-limited even under bright OH sky lines; we describe the strategies that permitted this, based on high image stability, accurate wavelength solutions, and powerful B-spline modeling methods. We also investigate the impact of targets that appear to be single objects in ground-based targeting imaging but prove to be composite in Hubble Space Telescope data; they constitute several percent of targets at z ∼ 1, approaching ∼5%-10% at z > 1.5. Summary data are given that demonstrate the superiority of DEEP2 over other deep high-precision redshift surveys at z ∼ 1 in terms of redshift accuracy, sample number density, and amount of spectral information. We also provide an overview of the scientific highlights of the DEEP2 survey thus far. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1203.3192}, -author = {Newman, Jeffrey A. and Cooper, Michael C. and Davis, Marc and Faber, S. M. and Coil, Alison L. and Guhathakurta, Puragra and Koo, David C. and Phillips, Andrew C. and Conroy, Charlie and Dutton, Aaron A. and Finkbeiner, Douglas P. and Gerke, Brian F. and Rosario, David J. and Weiner, Benjamin J. and Willmer, C. N.A. and Yan, Renbin and Harker, Justin J. and Kassin, Susan A. and Konidaris, N. P. and Lai, Kamson and Madgwick, Darren S. and Noeske, K. G. and Wirth, Gregory D. and Connolly, A. J. and Kaiser, N. and Kirby, Evan N. and Lemaux, Brian C. and Lin, Lihwai and Lotz, Jennifer M. and Luppino, G. A. and Marinoni, C. and Matthews, Daniel J. and Metevier, Anne and Schiavon, Ricardo P.}, -doi = {10.1088/0067-0049/208/1/5}, -eprint = {1203.3192}, -isbn = {00221090}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {cosmology: observations,galaxies: distances and redshifts,galaxies: evolution,galaxies: fundamental parameters,galaxies: high-redshift,galaxies: statistics,large-scale structure of universe,methods: data analysis,surveys}, -number = {1}, -pages = {5}, -title = {{The deep2 galaxy redshift survey: Design, observations, data reduction, and redshifts}}, -url = {http://arxiv.org/abs/1203.3192}, -volume = {208}, -year = {2013} -} -@article{Kotilainen2018, -abstract = {Recently, the relation between the masses of the black hole (MBH) and the host galaxy (Mhost) in quasars has been probed down to the parameter space ofMBH $\sim$ 108M⊙ and Mhost $\sim$ 1011M⊙ at z < 0.5. In this study, we have investigated the MBH-Mhost log-linear relation for a sample of 37 quasars with low black hole masses (107M⊙ < MBH < 108.3M⊙) at 0.5 < z < 1.0. The black hole masses were derived using virial mass estimates from Sloan Digital Sky Survey (SDSS) optical spectra. For 25 quasars, we detected the presence of the host galaxy from deep near-infraredH-band imaging, whereas upper limits for the host galaxy luminosity (mass) were estimated for the 12 unresolved quasars. We combined our previous studies with the results from this work to create a sample of 89 quasars at z < 1.0 having a large range of black hole masses (107M⊙ < MBH < 1010M⊙) and host galaxy masses (1010M⊙ < Mhost < 1013M⊙). Most of the quasars at the low-mass end lie below the extrapolation of the local relation. This apparent break in the linearity of the entire sample is due to increasing fraction of discdominated host galaxies in the low-mass quasars. After correcting for the disc component, and considering only the bulge component, the bilinear regression for the entire quasar sample holds over 3.5 dex in both the black hole mass and the bulge mass, and is in very good agreement with the local relation. We advocate secular evolution of discs of galaxies being responsible for the relatively strong disc domination.}, -archivePrefix = {arXiv}, -arxivId = {1409.1948}, -author = {Sanghvi, J. and Kotilainen, J. K. and Falomo, R. and Decarli, R. and Karhunen, K. and Uslenghi, M.}, -doi = {10.1093/mnras/stu1822}, -eprint = {1409.1948}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sanghvi et al. - 2014 - The black hole-host galaxy relation for very low mass quasars.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: high-redshift,Galaxies: nuclei,Quasars: general}, -number = {2}, -pages = {1261--1268}, -title = {{The black hole-host galaxy relation for very low mass quasars}}, -volume = {445}, -year = {2014} -} -@article{Tinker2013, -abstract = {We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2, 1.0]. For massive galaxies, M ≳ 1010.6 M , our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M ∼ 1010 M , the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency. {\textcopyright}2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1308.2974}, -author = {Tinker, Jeremy L and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H}, -doi = {10.1088/0004-637X/778/2/93}, -eprint = {1308.2974}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: halos}, -number = {2}, -title = {{Evolution of the stellar-to-dark matter relation: Separating star-forming and passive galaxies from z = 1 to 0}}, -volume = {778}, -year = {2013} -} -@article{Gow2016, -abstract = {{\textcopyright} 2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P. D. and Murray, Neil J.}, -doi = {10.1117/12.2232706}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gow, Murray - 2016 - Simplified charge transfer inefficiency correction in CCDs by trap-pumping(2).pdf:pdf}, -isbn = {9781510602090}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{Schaller2015c, -abstract = {We investigate the internal structure and density profiles of haloes of mass 1010-1014M{\textperiodcentered} in the Evolution and Assembly of Galaxies and their Environment (EAGLE) simulations. These follow the formation of galaxies in a $\Delta$ cold dark matter Universe and include a treatment of the baryon physics thought to be relevant. The EAGLE simulations reproduce the observed present-day galaxy stellar mass function, as well as many other properties of the galaxy population as a function of time.We find significant differences between the masses of haloes in the EAGLE simulations and in simulations that follow only the dark matter component. Nevertheless, haloes are well described by the Navarro-Frenk-White density profile at radii larger than $\sim$5 per cent of the virial radius but, closer to the centre, the presence of stars can produce cuspier profiles. Central enhancements in the total mass profile are most important in haloes of mass 1012-1013M{\textperiodcentered}, where the stellar fraction peaks. Over the radial range where they are well resolved, the resulting galaxy rotation curves are in very good agreement with observational data for galaxies with stellar mass M* < 5 × 1010M{\textperiodcentered}.We present an empirical fitting function that describes the total mass profiles and show that its parameters are strongly correlated with halo mass.}, -archivePrefix = {arXiv}, -arxivId = {1409.8617}, -author = {Schaller, Matthieu and Frenk, Carlos S. and Bower, Richard G. and Theuns, Tom and Jenkins, Adrian and Schaye, Joop and Crain, Robert A. and Furlong, Michelle and Vecchia, Claudio Dalla and McCarthy, I. G.}, -doi = {10.1093/mnras/stv1067}, -eprint = {1409.8617}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Large-scale structure of universe}, -month = {aug}, -number = {2}, -pages = {1247--1267}, -title = {{Baryon effects on the internal structure of $\Delta$CDM haloes in the EAGLE simulations}}, -url = {http://adsabs.harvard.edu/abs/2014arXiv1409.8617S}, -volume = {451}, -year = {2015} -} -@article{Algorry2016, -abstract = {We examine the properties of barred disc galaxies in a $\Lambda$CDM cosmological hydrodynamical simulation from the EAGLE project. Our study follows the formation of 269 discs identified at z = 0 in the stellar mass range 10.6 < logM∗/M⊙ < 11. These discs show a wide range of bar strengths, from unbarred discs (≈60 per cent) to weak bars (≈20 per cent) and to strongly barred systems (≈20 per cent). Bars in these systems develop after redshift ≈1.3, on timescales that depend sensitively on the strength of the pattern. Strong bars develop relatively quickly (in a few Gyr, or roughly∼10 disc rotation periods) in systems that are disc dominated, gas poor, and have declining rotation curves.Weak bars develop more slowly in systems where the disc is less gravitationally important, and are still growing at z = 0. Unbarred galaxies are comparatively gas-rich discs whose rotation speeds do not exceed the maximum circular velocity of the haloes they inhabit. Bar lengths compare favourably with observations, ranging from 0.2 to 0.8 times the radius containing 90 per cent of the stars. Bars slow down remarkably quickly as they grow, causing the inner regions of the surrounding dark halo to expand. At z = 0 strong bars in simulated galaxies have corotation radii roughly 10 times the bar length. Such slow bars are inconsistent with the few cases where pattern speeds have been measured or inferred observationally, a discrepancy that, if confirmed, might prove a challenge for disc galaxy formation in $\Lambda$CDM.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1609.05909}, -author = {Algorry, David G. and Navarro, Julio F. and Abadi, Mario G. and Sales, Laura V. and Bower, Richard G. and Crain, Robert A. and Vecchia, Claudio Dalla and Frenk, Carlos S. and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx1008}, -eprint = {1609.05909}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Algorry et al. - 2017 - Barred galaxies in the EAGLE cosmological hydrodynamical simulation(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Kinematics and dynamics,Galaxy: Disc,Galaxy: Formation,Galaxy: Structure}, -number = {1}, -pages = {1054--1064}, -title = {{Barred galaxies in the EAGLE cosmological hydrodynamical simulation}}, -url = {http://arxiv.org/abs/1609.05909%0Ahttp://dx.doi.org/10.1093/mnras/stx1008}, -volume = {469}, -year = {2017} -} -@article{MacArthur2009a, -abstract = {We present a detailed study of the stellar populations (SPs) and kinematics of the bulge and inner disc regions of eight nearby spiral galaxies (Sa-Sd) based on deep Gemini/GMOS data. The long-slit spectra extend to 1-2 disc scalelengths with S/N/{\AA} ≥ 50. Several different model fitting techniques involving absorption-line indices and full spectrum fitting are explored, and found to weigh age, metallicity and abundance ratios differently. We find that the SPs of spiral galaxies are not well matched by single episodes of star formation; more representative SPs must involve average SP values integrated over the star formation history (SFH) of the galaxy. Our 'full population synthesis' method is an optimized linear combination of model templates to the full spectrum with masking of regions poorly represented by the models. Realistic determinations of the SP parameters and kinematics (rotation and velocity dispersion) also rely on careful attention to data/model matching (resolution and flux calibration). The population fits reveal a wide range of age and metallicity gradients (from negative to positive) in the bulge, allowing for diverse formation mechanisms. The observed positive age gradients within the effective radius of some late-type bulges helps reconcile the long-standing conundrum of the coexistence of secular-like kinematics, light profile shape and stellar bar with the 'classical'-like old and $\alpha$-enhanced SPs in the Milky Way bulge. The discs, on the other hand, almost always show mildly decreasing to flat profiles in both age and metallicity, consistent with inside-out formation. Our spiral bulges follow the same correlations of increasing light-weighted age and metallicity with central velocity dispersion as those of elliptical galaxies and early-type bulges found in other studies, but when SFHs more complex and realistic than a single burst are invoked, the trend with age is shallower and the scatter much reduced. In a mass-weighted context, however, all bulges are predominantly composed of old and metal-rich SPs. While secular contributions to the evolution of many of our bulges are clearly evident, with young (0.001-1 Gyr) SPs contributing as much as 90 per cent of the optical (V-band) light, the bulge mass fraction from young stars is small (≲25 per cent). The implies a bulge formation dominated by early processes that are common to all spheroids, whether they currently reside in discs or not. While monolithic collapse cannot be ruled out in some cases, merging must be invoked to explain the SP gradients in most bulges. Further bulge growth via secular processes or 'rejuvenated' star formation generally contributes minimally to the stellar mass budget, with the relative secular weight increasing with decreasing central velocity dispersion. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4135}, -author = {MacArthur, Lauren A. and Gonz{\'{a}}lez, J. Jes{\'{u}}s and Courteau, St{\'{e}}phane}, -doi = {10.1111/j.1365-2966.2009.14519.x}, -eprint = {0901.4135}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/MacArthur, Gonz{\'{a}}lez, Courteau - 2009 - Stellar population and kinematic profiles in spiral bulges and discs Population synthesis of inte.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: spiral,Galaxies: stellar content}, -number = {1}, -pages = {28--63}, -title = {{Stellar population and kinematic profiles in spiral bulges and discs: Population synthesis of integrated spectra}}, -volume = {395}, -year = {2009} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the Tiger principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper reports on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R and Copin, Y and Monnet, G and Miller, Bryan W and Allington-Smith, J R and Bureau, M and Carollo, C Marcella and Davies, Roger L and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F and Verolme, E K and {De Zeeuw}, P Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs,cD}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{Shockley1952, -abstract = {The statistics of the recombination of holes and electrons in semiconductors is analyzed on the basis of a model in which the recombination occurs through the mechanism of trapping. A trap is assumed to have an energy level in the energy gap so that its charge may have either of two values differing by one electronic charge. The dependence of lifetime of injected carriers upon initial conductivity and upon injected carrier density is discussed. {\textcopyright}1952 The American Physical Society.}, -author = {Shockley, W and Read, W T}, -doi = {10.1103/PhysRev.87.835}, -issn = {0031899X}, -journal = {Physical Review}, -keywords = {Shockley1952}, -mendeley-tags = {Shockley1952}, -number = {5}, -pages = {835--842}, -title = {{Statistics of the recombinations of holes and electrons}}, -volume = {87}, -year = {1952} -} -@article{Murray2013, -abstract = {A multi-level clocking scheme has been developed to improve the parallel CTE of four-phase CCDs by suppressing the effects of traps located in the transport channel under barrier phases by inverting one of these phases throughout the transfer sequence. In parallel it was apparent that persistence following optical overload in Euclid VIS detectors would lead to undesirable signal released in subsequent rows and frames and that a suitable scheme for flushing this signal would be required. With care, the negatively biased electrodes during the multi-level transfer sequence can be made to pin the entire surface, row-by-row, and annihilate the problematic charges. This process can also be extended for use during integration to significantly reduce the unusable area of the detector, as per the clocked anti-blooming techniques developed many years ago; however, with the four-phase electrodes architecture of modern CCDs, we can take precautionary measures to avoid the problem of charge pumping and clock induced charge within the science frames. Clock induced charge is not all bad! We also propose the use of on-orbit trap-pumping for Euclid VIS to provide calibration input to ground based correction algorithms and as such a uniform, low noise background is require. Clock induced charge can be manipulated to provide a very suitable, low signal and noise background to the imaging array. Here we describe and present results of multi-level parallel clocking schemes for use in four-phase CCDs that could improve performance of high precision astronomy applications such as Euclid VIS. ? 2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Holland, Andrew D and Stefanov, Konstantin D and Gow, Jason P D and MacCormick, Calum and Dryer, Ben J and Allanwood, Edgar A H}, -doi = {10.1117/12.2024839}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {Blooming,CAB,CCD,CIC,CTE,Euclid VIS,Mu,[BFW}, -pages = {88600K}, -title = {{Multi-level parallel clocking of CCDs for: improving charge transfer efficiency, clearing persistence, clocked anti-blooming, and generating low-noise backgrounds for pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024839}, -volume = {8860}, -year = {2013} -} -@article{Unruh2016, -abstract = {Strong gravitational lensing is regarded as the most precise technique to measure the mass in the inner region of galaxies or galaxy clusters. In particular, the mass within one Einstein radius can be determined with an accuracy of order of a few percent or better, depending on the image configuration. For other radii, however, degeneracies exist between galaxy density profiles, precluding an accurate determination of the enclosed mass. The source position transformation (SPT), which includes the well-known mass-sheet transformation (MST) as a special case, describes this degeneracy of the lensing observables in a more general way. In this paper we explore properties of an SPT, removing the MST to leading order, i.e., we consider degeneracies which have not been described before. The deflection field {\$}\backslashboldsymbol{\{}\backslashhat{\{}\backslashalpha{\}}{\}}(\backslashboldsymbol{\{}\backslashtheta{\}}){\$} resulting from an SPT is not curl-free in general, and thus not a deflection that can be obtained from a lensing mass distribution. Starting from a variational principle, we construct lensing potentials that give rise to a deflection field {\$}\backslashboldsymbol{\{}\backslashtilde{\{}\backslashalpha{\}}{\}}{\$}, which differs from {\$}\backslashboldsymbol{\{}\backslashhat{\{}\backslashalpha{\}}{\}}{\$} by less than an observationally motivated upper limit. The corresponding mass distributions from these 'valid' SPTs are studied: their radial profiles are modified relative to the original mass distribution in a significant and non-trivial way, and originally axi-symmetric mass distributions can obtain a finite ellipticity. These results indicate a significant effect of the SPT on quantitative analyses of lens systems. We show that the mass inside the Einstein radius of the original mass distribution is conserved by the SPT; hence, as is the case for the MST, the SPT does not affect the mass determination at the Einstein radius. [...]}, -archivePrefix = {arXiv}, -arxivId = {1606.04321}, -author = {Unruh, Sandra and Schneider, Peter and Sluse, Dominique}, -doi = {10.1051/0004-6361/201629048}, -eprint = {1606.04321}, -issn = {14320746}, -journal = {ArXiv e-prints}, -keywords = {cosmological parameters,gravitational lensing,strong}, -month = {jun}, -number = {1}, -pages = {1--13}, -title = {{Ambiguities in gravitational lens models: the density field from the source position transformation}}, -url = {http://arxiv.org/abs/1606.04321%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201629048}, -year = {2016} -} -@article{Johnston2016, -abstract = {With the availability of large integral field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, howgalaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present bulge-disc decomposition of IFU data cubes (BUDDI), a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GALFITM, a modified form of GALFIT which can fit multiwaveband images simultaneously. The benefit of this technique over traditional multiwaveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the Sloan Digital Sky Survey-IV Mapping Nearby Galaxies atAPO(MaNGA)survey with redshifts z {\textless} 0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec full width at half-maximum and field of view of {\textgreater} 22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from theMaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data.}, -archivePrefix = {arXiv}, -arxivId = {1611.00609}, -author = {Johnston, Evelyn J and H{\"{a}}u{\ss}ler, Boris and Arag{\'{o}}n-Salamanca, Alfonso and Merrifield, Michael R and Bamford, Steven and Bershady, Matthew A and Bundy, Kevin and Drory, Niv and Fu, Hai and Law, David and Nitschelm, Christian and Thomas, Daniel and Lopes, Alexandre Roman and Wake, David and Yan, Renbin}, -doi = {10.1093/mnras/stw2823}, -eprint = {1611.00609}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content,Galaxies: structure}, -number = {2}, -pages = {2317--2341}, -title = {{SDSS-IV MaNGA: Bulge-disc decomposition of IFU data cubes (BUDDI)}}, -url = {http://arxiv.org/abs/1611.00609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2823}, -volume = {465}, -year = {2017} -} -@article{Morishita2018, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Dekel2009, -author = {Dekel, Avishai and Sari, Re'em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {785--801}, -title = {{Formation of Massive Galaxies At High Redshift: Cold Streams, Clumpy Disks, and Compact Spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism, which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio (M/L) and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R, z) and characterized by the classic anisotropy parameter. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters ($\beta$z and the inclination), the models generally provide remarkably good descriptions of the shape of the first (V) and second () velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the dynamical structure of these objects. With the observationally motivated assumption that $\beta$z ≳ 0, the method is able to recover the inclination. The technique can be used to determine the dynamical M/L and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modelling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy and multiple kinematic components. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cappellari - 2008 - Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stella(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani}, and Nelson Caldwell}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani - 2002 - EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXI(2).pdf:pdf}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Conselice1999, -abstract = {We present a detailed study of rotational asymmetry in galaxies for both morphological and physical diagnostic purposes. An unambiguous method for computing asymmetry is developed, robust for both distant and nearby galaxies. By degrading real galaxy images, we test the reliability of this asymmetry measure over a range of observational conditions, e.g. spatial resolution and signal-to-noise (S/N). Compared to previous methods, this new algorithm avoids the ambiguity associated with choosing a center by using a minimization method, and successfully corrects for variations in S/N. There is, however, a strong relationship between the rotational asymmetry and physical resolution (distance at fixed spatial resolution); objects become more symmetric when less well-resolved. We further investigate asymmetry as a function of galactic radius an rotation. We find the asymmetry index has a strong radial dependence that differs vastly between Hubble types. As a result, a meaningful asymmetry index must be specified within a well-defined radius representative of the physical galaxy scale. We enumerate several viable alternatives, which excludes the use of isophotes. Asymmetry as a function of angle (A[phi]) is also a useful indicator of ellipticity and higher-order azimuthal structure. In general, we show the power of asymmetry as a morphological parameter lies in the strong correlation with (B-V) color for galaxies undergoing normal star formation, spanning all Hubble types from ellipticals to irregular galaxies. Interacting galaxies do not fall on this asymmetry-color ``fiducial sequence,'' as these galaxies are too asymmetric for their color. We propose to use this fact to distinguish between `normal' galaxies and galaxies undergoing an interaction or merger at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9907399}, -author = {Conselice, Christopher J. and Bershady, Matthew A. and Jangren, Anna}, -doi = {10.1086/308300}, -eprint = {9907399}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {GALAXIES: PHOTOMETRY,GALAXIES: STRUCTURE,Galaxies: Photometry,Galaxies: Structure}, -month = {feb}, -number = {2}, -pages = {886--910}, -primaryClass = {astro-ph}, -title = {{The Asymmetry of Galaxies: Physical Morphology for Nearby and High‐Redshift Galaxies}}, -url = {http://arxiv.org/abs/astro-ph/9907399%0Ahttp://dx.doi.org/10.1086/308300}, -volume = {529}, -year = {2000} -} -@article{EuclidCollaboration2025, -abstract = {We present a catalogue of 497 galaxy-galaxy strong lenses in the Euclid Quick Release 1 data (63 deg$^2$). In the initial 0.45\% of Euclid's surveys, we double the total number of known lens candidates with space-based imaging. Our catalogue includes 250 grade A candidates, the vast majority of which (243) were previously unpublished. Euclid's resolution reveals rare lens configurations of scientific value including double-source-plane lenses, edge-on lenses, complete Einstein rings, and quadruply-imaged lenses. We resolve lenses with small Einstein radii ($\theta_{\rm E} < 1''$) in large numbers for the first time. These lenses are found through an initial sweep by deep learning models, followed by Space Warps citizen scientist inspection, expert vetting, and system-by-system modelling. Our search approach scales straightforwardly to Euclid Data Release 1 and, without changes, would yield approximately 7000 high-confidence (grade A or B) lens candidates by late 2026. Further extrapolating to the complete Euclid Wide Survey implies a likely yield of over 100000 high-confidence candidates, transforming strong lensing science.}, -archivePrefix = {arXiv}, -arxivId = {2503.15324}, -author = {{Euclid Collaboration} and Walmsley, M. and Holloway, P. and Lines, N. E. P. and Rojas, K. and Collett, T. E. and Verma, A. and Li, T. and Nightingale, J. W. and Despali, G. and Schuldt, S. and Gavazzi, R. and Melo, A. and Metcalf, R. B. and Andika, I. T. and Leuzzi, L. and Manj{\'{o}}n-Garc{\'{i}}a, A. and Pearce-Casey, R. and Vincken, S. H. and Wilde, J. and Busillo, V. and Tortora, C. and Barroso, J. A. Acevedo and Dole, H. and Ecker, L. R. and Pearson, J. and Marshall, P. J. and More, A. and Saifollahi, T. and Gracia-Carpio, J. and Baeten, E. and Cornen, C. and Johnson, L. C. and Macmillan, C. and Kruk, S. and Remmelgas, K. A. and Cl{\'{e}}ment, B. and Degaudenzi, H. and Courbin, F. and Bovy, J. and Casas, S. and Dannerbauer, H. and Diego, J. M. and Finner, K. and Galan, A. and Giocoli, C. and Hogg, N. B. and Jahnke, K. and Katona, J. and Kov{\'{a}}cs, A. and {De Leo}, C. and Mahler, G. and Millon, M. and Nagam, B. C. and Nugent, P. and de Murieta, A. Sainz and O'Riordan, C. M. and Sluse, D. and Sonnenfeld, A. and Spiniello, C. and Serjeant, S. and Thai, T. T. and Ulivi, L. and Walth, G. L. and Weisenbach, L. and Zumalacarregui, M. and Aghanim, N. and Altieri, B. and Amara, A. and Andreon, S. and Auricchio, N. and Aussel, H. and Baccigalupi, C. and Baldi, M. and Balestra, A. and Bardelli, S. and Battaglia, P. and Bernardeau, F. and Biviano, A. and Bonchi, A. and Bonino, D. and Branchini, E. and Brescia, M. and Brinchmann, J. and Camera, S. and Ca{\~{n}}as-Herrera, G. and Capobianco, V. and Carbone, C. and Cardone, V. F. and Carretero, J. and Castander, F. J. and Castellano, M. and Castignani, G. and Cavuoti, S. and Chambers, K. C. and Cimatti, A. and Colodro-Conde, C. and Congedo, G. and Conselice, C. J. and Conversi, L. and Copin, Y. and Corcione, L. and Courtois, H. M. and Cropper, M. and {Da Silva}, A. and {De Lucia}, G. and {Di Giorgio}, A. M. and Dolding, C. and Dubath, F. and Duncan, C. A. J. and Dupac, X. and Ealet, A. and Escoffier, S. and Fabricius, M. and Farina, M. and Farinelli, R. and Faustini, F. and Finelli, F. and Fotopoulou, S. and Frailis, M. and Franceschi, E. and Fumana, M. and Galeotta, S. and George, K. and Gillard, W. and Gillis, B. and G{\'{o}}mez-Alvarez, P. and Granett, B. R. and Grazian, A. and Grupp, F. and Guzzo, L. and Gwyn, S. and Haugan, S. V. H. and Hoekstra, H. and Holmes, W. and Hook, I. M. and Hormuth, F. and Hornstrup, A. and Hudelot, P. and Jhabvala, M. and Joachimi, B. and Keih{\"{a}}nen, E. and Kermiche, S. and Kiessling, A. and Kubik, B. and K{\"{u}}mmel, M. and Kunz, M. and Kurki-Suonio, H. and Lahav, O. and Boulc'h, Q. Le and Brun, A. M. C. Le and Mignant, D. Le and Ligori, S. and Lilje, P. B. and Lindholm, V. and Lloro, I. and Mainetti, G. and Maino, D. and Maiorano, E. and Mansutti, O. and Marcin, S. and Marggraf, O. and Martinelli, M. and Martinet, N. and Marulli, F. and Massey, R. and Maurogordato, S. and McCracken, H. J. and Medinaceli, E. and Mei, S. and Mellier, Y. and Meneghetti, M. and Merlin, E. and Meylan, G. and Mora, A. and Moresco, M. and Moscardini, L. and Nakajima, R. and Neissner, C. and Nichol, R. C. and Niemi, S. -M. and Padilla, C. and Paltani, S. and Pasian, F. and Pedersen, K. and Percival, W. J. and Pettorino, V. and Pires, S. and Polenta, G. and Poncet, M. and Popa, L. A. and Pozzetti, L. and Raison, F. and Rebolo, R. and Renzi, A. and Rhodes, J. and Riccio, G. and Romelli, E. and Roncarelli, M. and Saglia, R. and Sakr, Z. and S{\'{a}}nchez, A. G. and Sapone, D. and Sartoris, B. and Schewtschenko, J. A. and Schirmer, M. and Schneider, P. and Schrabback, T. and Secroun, A. and Seidel, G. and Seiffert, M. and Serrano, S. and Simon, P. and Sirignano, C. and Sirri, G. and Mancini, A. Spurio and Stanco, L. and Steinwagner, J. and Tallada-Cresp{\'{i}}, P. and Taylor, A. N. and Tereno, I. and Tessore, N. and Toft, S. and Toledo-Moreo, R. and Torradeflot, F. and Tutusaus, I. and Valentijn, E. A. and Valenziano, L. and Valiviita, J. and Vassallo, T. and Kleijn, G. Verdoes and Veropalumbo, A. and Wang, Y. and Weller, J. and Zacchei, A. and Zamorani, G. and Zerbi, F. M. and Zucca, E. and Allevato, V. and Ballardini, M. and Bolzonella, M. and Bozzo, E. and Burigana, C. and Cabanac, R. and Cappi, A. and {Di Ferdinando}, D. and Vigo, J. A. Escartin and Gabarra, L. and Huertas-Company, M. and Mart{\'{i}}n-Fleitas, J. and Matthew, S. and Mauri, N. and Pezzotta, A. and P{\"{o}}ntinen, M. and Porciani, C. and Risso, I. and Scottez, V. and Sereno, M. and Tenti, M. and Viel, M. and Wiesmann, M. and Akrami, Y. and Anselmi, S. and Archidiacono, M. and Atrio-Barandela, F. and Benoist, C. and Benson, K. and Bergamini, P. and Bertacca, D. and Bethermin, M. and Blot, L. and Borgani, S. and Brown, M. L. and Bruton, S. and Calabro, A. and Quevedo, B. Camacho and Caro, F. and Carvalho, C. S. and Castro, T. and Charles, Y. and Cogato, F. and Cooray, A. R. and Cucciati, O. and Davini, S. and {De Paolis}, F. and Desprez, G. and D{\'{i}}az-S{\'{a}}nchez, A. and Diaz, J. J. and {Di Domizio}, S. and Enia, A. and Fang, Y. and Ferrari, A. G. and Finoguenov, A. and Fontana, A. and Franco, A. and Ganga, K. and Garc{\'{i}}a-Bellido, J. and Gasparetto, T. and Gautard, V. and Gaztanaga, E. and Giacomini, F. and Gozaliasl, G. and Guidi, M. and Gutierrez, C. M. and Hall, A. and Hartley, W. G. and Hemmati, S. and Hern{\'{a}}ndez-Monteagudo, C. and Hildebrandt, H. and Hjorth, J. and Kajava, J. J. E. and Kang, Y. and Kansal, V. and Karagiannis, D. and Kiiveri, K. and Kirkpatrick, C. C. and Graet, J. Le and Legrand, L. and Lembo, M. and Lepori, F. and Leroy, G. and Lesci, G. F. and Lesgourgues, J. and Liaudat, T. I. and Loureiro, A. and Macias-Perez, J. and Maggio, G. and Magliocchetti, M. and Magnier, E. A. and Mannucci, F. and Maoli, R. and Martins, C. J. A. P. and Maurin, L. and Miluzio, M. and Monaco, P. and Moretti, C. and Morgante, G. and Murray, C. and Nadathur, S. and Naidoo, K. and Navarro-Alsina, A. and Nesseris, S. and Passalacqua, F. and Paterson, K. and Patrizii, L. and Pisani, A. and Potter, D. and Quai, S. and Radovich, M. and Rocci, P. -F. and Sacquegna, S. and Sahl{\'{e}}n, M. and Sanders, D. B. and Sarpa, E. and Scarlata, C. and Schaye, J. and Schneider, A. and Sciotti, D. and Sellentin, E. and Shankar, F. and Smith, L. C. and Tanidis, K. and Testera, G. and Teyssier, R. and Tosi, S. and Troja, A. and Tucci, M. and Valieri, C. and Venhola, A. and Vergani, D. and Vernardos, G. and Verza, G. and Vielzeuf, P. and Walton, N. A. and Scott, D.}, -eprint = {2503.15324}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/EuclidQ12025paperI.pdf:pdf}, -journal = {https://arxiv.org/abs/2503.15324}, -title = {{Euclid Quick Data Release (Q1): The Strong Lensing Discovery Engine A -- System overview and lens catalogue}}, -url = {http://arxiv.org/abs/2503.15324}, -year = {2025} -} -@article{Cohen2018, -abstract = {We present HST/ACS imaging of twenty-three very low surface brightness ({\$}\backslashmu{\_}{\{}e,V{\}}{\$}=25-27.5) galaxies detected in the fields of four nearby galaxy groups. These objects were selected from deep optical imaging obtained with the Dragonfly Telephoto Array. Seven are new discoveries, while most of the others had been identified previously in visual surveys of deep photographic plates and more recent surveys. Few have previously been studied in detail. From the ACS images, we measure distances to the galaxies using both the tip of the red giant branch method and the surface brightness fluctuations method. We demonstrate that the two methods are consistent with each other in the regime where both can be applied. The distances to 15 out of 20 galaxies with stable measurements are consistent with that of the targeted group within errors. This suggests that assuming group membership based solely on projected proximity is {\$\sim${}}75{\%} successful in this regime. The galaxies are nearly round, with a median axis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The objects have a range of sizes, from {\$}R{\_}e{\$}=0.4 kpc to {\$}R{\_}e{\$}=1.8 kpc, with a median of 1.0 kpc. They range in luminosity from {\$}M{\_}V{\$}=-11.4 to {\$}M{\_}V{\$}=-15.6, with a median of -12.4. Galaxies with {\$}R{\_}e{\$}{\$\sim${}}1 kpc and {\$}M{\_}V{\$}{\$\sim${}}-12 are fairly rare in the Local Group but we find many of them in this relatively small sample. Four of the objects fall in the class of ultra diffuse galaxies (UDGs), with {\$}R{\_}e{\$}{\textgreater}1.5 kpc and {\$}\backslashmu{\_}{\{}0,V{\}}{\$}{\textgreater}24 mag/arcsec{\^{}}2, including the recently identified dark matter deficient galaxy NGC1052-DF2.}, -archivePrefix = {arXiv}, -arxivId = {1807.06016}, -author = {Cohen, Yotam and van Dokkum, Pieter and Danieli, Shany and Romanowsky, Aaron J and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Mowla, Lamiya and Kruijssen, J M Diederik and Conroy, Charlie and Wasserman, Asher}, -doi = {10.3847/1538-4357/aae7c8}, -eprint = {1807.06016}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {Astrophysics,Astrophysics of Galaxies}, -number = {2}, -pages = {96}, -title = {{ The Dragonfly Nearby Galaxies Survey. V. HST /ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC 1052, NGC 1084, M96, and NGC 4258 }}, -url = {http://arxiv.org/abs/1807.06016%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aae7c8}, -volume = {868}, -year = {2018} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales (∼500 kpc) in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the virial radius of the haloes while describing the infalling matter via fluxes through a spherical shell; and we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP described for the first time in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one- and two-point statistics. The peripheral and advected momenta are correlated with the spin of the embedded halo at levels of 30 and 50 per cent. The infall takes place preferentially in the plane perpendicular to the direction defined by the spin of the halo. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be ∼15 per cent. The substructures have their spin orthogonal to their velocity vector in the rest frame of the halo at a level of about 5 per cent, suggestive of an image of a flow along filamentary structures, which provides an explanation for the measured anisotropy. Using a 'synthetic' stacked halo, it is shown that the positions and orientations of satellites relative to the direction of spin of the halo are not random even in projection. The average ellipticity of stacked haloes is 10 per cent, while the alignment excess in projection reaches 2 per cent. All measured correlations are fitted by a simple three-parameter model. We conclude that a halo does not see its environment as an Isotropic perturbation, we investigate how the anisotropy is propagated inwards using perturbation theory, and we discuss briefly the implications for weak lensing, warps and the thickness of galactic discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D. and Pichon, C. and Colombi, S.}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Aubert, Pichon, Colombi - 2004 - The origin and implications of dark matter anisotropic cosmic infall on ≈ L haloes.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies, in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the SDSS in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on the UV-optical colour {\$}NUV-r{\$}. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings that green valley galaxies have intermediate morphologies, moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of green valley galaxies, we find that they tend to be more massive in the field than in denser environments. On average, green valley galaxies account for {\$}\backslashsim 20\backslash{\%}{\$} of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming low mass galaxies. Green valley galaxies have average star formation histories intermediate between passive and star forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time, and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Croom2009, -abstract = {We present the QSO luminosity function of the completed 2dF-SDSS LRG and QSO (2SLAQ) survey, based on QSOs photometrically selected from Sloan Digital Sky Survey imaging data and then observed spectroscopically using the 2dF instrument on the Anglo-Australian Telescope. We analyse 10637 QSOs in the redshift range 0.4{\textless}z{\textless}2.6 to a g-band flux limit of 21.85 (extinction corrected) and an absolute continuum magnitude of Mg(z=2){\textless}-21.5. This sample covers an area of 191.9 deg{\^{}}2. The binned QSO luminosity function agrees with that of the brighter SDSS main QSO sample, but extends {\$\sim${}}2.5 mags fainter, clearly showing the flattening of the luminosity function towards faint absolute magnitudes. 2SLAQ finds an excess of QSOs compared to the 2dF QSO Redshift Survey at g{\textgreater}20.0, as found previously by Richards et al. (2005). The luminosity function is consistent with other previous, much smaller, samples produced to the depth of 2SLAQ. By combining the 2SLAQ and SDSS QSO samples we produce a QSO luminosity function with an unprecedented combination of precision and dynamic range. With this we are able to accurately constrain both the bright and faint ends of the QSO LF. While the overall trends seen in the evolution of the QSO LF appear similar to pure luminosity evolution, the data show very significant departures from such a model. Most notably we see clear evidence that the number density of faint QSOs peaks at lower redshift than bright QSOs: QSOs with Mg{\textgreater}-23 have space densities which peak at z{\textless}1, while QSOs at Mg{\textless}-26 peak at z{\textgreater}2. By fitting simple luminosity function models in narrow Mg intervals we find that this downsizing is significant at the 99.98 per cent level (abridged).}, -archivePrefix = {arXiv}, -arxivId = {0907.2727}, -author = {Croom, Scott M and Richards, Gordon T and Shanks, Tom and Boyle, Brian J and Strauss, Michael A and Myers, Adam D and Nichol, Robert C and Pimbblet, Kevin A and Ross, Nicholas P and Schneider, Donald P and Sharp, Robert G and Wake, David A}, -doi = {10.1111/j.1365-2966.2009.15398.x}, -eprint = {0907.2727}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Seyfert,Galaxies: active,Quasars: general}, -month = {nov}, -number = {4}, -pages = {1755--1772}, -title = {{The 2dF-SDSS LRG and QSO survey: The QSO luminosity function at 0.4 {\textless} z {\textless} 2.6}}, -volume = {399}, -year = {2009} -} -@article{Naab2009, -abstract = {Using a high-resolution hydrodynamical cosmological simulation of the formation of a massive spheroidal galaxy we show that elliptical galaxies can be very compact and massive at high redshift in agreement with recent observations. Accretion of stripped infalling stellar material increases the size of the system with time and the central concentration is reduced by dynamical friction of the surviving stellar cores. In a specific case of a spheroidal galaxy with a final stellar mass of 1.5 × 1011 M ⊙ we find that the effective radius re increases from 0.7 ± 0.2 kpc at z = 3 to re = 2.4 ± 0.4 kpc at z = 0 with a concomitant decrease in the effective density of an order of magnitude and a decrease of the central velocity dispersion by approximately 20{\%} over this time interval. A simple argument based on the virial theorem shows that during the accretion of weakly bound material (minor mergers) the radius can increase as the square of the mass in contrast to the usual linear rate of increase for major mergers. By undergoing minor mergers compact high-redshift spheroids can evolve into present-day systems with sizes and concentrations similar to observed local ellipticals. This indicates that minor mergers may be the main driver for the late evolution of sizes and densities of early-type galaxies. {\textcopyright}2009 The American Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {0903.1636}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P}, -doi = {10.1088/0004-637X/699/2/L178}, -eprint = {0903.1636}, -issn = {2041-821}, -journal = {Astrophysical Journal Letters}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: interactions,Galaxies: structure,Methods: numerical,cd}, -month = {jul}, -number = {2 PART 2}, -pages = {L178----L182}, -title = {{Minor mergers and the size evolution of elliptical galaxies}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L178?key=crossref.405faa44137f4be9a7e3800a4c3e7dea}, -volume = {699}, -year = {2010} -} -@article{Naab2009, -abstract = {Using a high resolution hydrodynamical cosmological simulation of the formation of a massive spheroidal galaxy we show that elliptical galaxies can be very compact and massive at high redshift in agreement with recent observations. Accretion of stripped in-falling stellar material increases the size of the system with time and the central concentration is reduced by dynamical friction of the surviving stellar cores. In a specific case of a spheroidal galaxy with a final stellar mass of {\$}1.5 \backslashbackslashtimes 10{\^{}}{\{}11{\}} M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} we find that the effective radius {\$}r{\_}e{\$} increases from {\$}0.7 \backslashbackslashpm 0.2 \backslashbackslashrm kpc{\$} at z = 3 to {\$}r{\_}e = 2.4 \backslashbackslashpm 0.4 \backslashbackslashrm kpc{\$} at z = 0 with a concomitant decrease in the effective density of an order of magnitude and a decrease of the central velocity dispersion by approximately 20{\%} over this time interval. A simple argument based on the virial theorem shows that during the accretion of weakly bound material (minor mergers) the radius can increase as the square of the mass in contrast to the usual linear rate of increase for major mergers. By undergoing minor mergers compact high redshift spheroids can evolve into present-day systems with sizes and concentrations similar to observed local ellipticals. This indicates that minor mergers may be the main driver for the late evolution of sizes and densities of early-type galaxies.}, -archivePrefix = {arXiv}, -arxivId = {0903.1636}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P}, -doi = {10.1088/0004-637X/699/2/L178}, -eprint = {0903.1636}, -issn = {2041-821}, -journal = {Astrophysical Journal Letters}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: interactions,Galaxies: structure,Methods: numerical,cd}, -month = {jul}, -number = {2 PART 2}, -pages = {L178--------L182}, -title = {{Minor mergers and the size evolution of elliptical galaxies}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L178?key=crossref.405faa44137f4be9a7e3800a4c3e7dea}, -volume = {699}, -year = {2010} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, {\$}n=10\backslash, {\{}\backslashrm cm{\}}{\^{}}{\{}-3{\}}{\$}, results in strong expansion of the DM halo in galaxies with stellar masses in the range {\$}10{\^{}}{\{}7.5{\}} {\textless} M{\_}{\{}star{\}} {\textless} 10{\^{}}{\{}9.5{\}} M{\_}{\{}\backslashodot{\}}{\$}. We find that lower thresholds such as {\$}n=0.1{\$} (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e., {\textless} 50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with {\$}n=10{\$} have gas fractions of {\$}\backslashsimeq 0.2{\$} and variations of {\$}\backslashsimeq 0.1{\$}, while {\$}n=0.1{\$} simulations have order of magnitude lower gas fractions and hence do not expand the halo. Star formation rates are more variable for higher {\$}n{\$}, lower galaxy masses, and when star formation is measured on shorter time scales. Simulations with {\$}n=10{\$} have up to 0.4 dex higher scatter in specific star formation rates than simulations with {\$}n=0.1{\$}. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with {\$}n=0.1{\$} and {\$}n=1{\$}, but in reasonable agreement with {\$}n=10{\$}. While the strong dependence of the halo response to {\$}n{\$} currently prevents a robust prediction for dark halo structure in CDM cosmologies, it is reassuring that different {\$}n{\$} result in testable predictions for the properties of gas and star formation, and thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625}, -author = {Dutton, Aaron A and Macci{\`{o}}, Andrea V and Buck, Tobias and Dixon, Keri L and Blank, Marvin and Obreja, Aura}, -eprint = {1811.10625}, -keywords = {cosmology,formation-galaxies,kine-matics and dynamics-galaxies,numerical,structure-methods,theory-dark matter-galaxies}, -number = {November}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://arxiv.org/abs/1811.10625}, -volume = {000}, -year = {2018} -} -@article{Bower:2016aa, -abstract = {Galaxies fall into two clearly distinct types: `blue-sequence' galaxies that are rapidly forming young stars, and `red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than {\$}3\backslashtimes10{\^{}}{\{}10{\}} M{\_}\backslashodot{\$} follow the red-sequence while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's center. We develop a simple analytic model for this interaction. In galaxies less massive than {\$}3\backslashtimes10{\^{}}{\{}10{\}} M{\_}\backslashodot{\$}, young stars and supernovae drive a high entropy outflow that is more buoyant that any diffuse corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by a hot corona. We argue that above a halo mass of {\$}\backslashsim 10{\^{}}{\{}12{\}} M{\_}\backslashodot{\$}, the supernova-driven outflow is no longer buoyant and star formation is unable to prevent the build up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers. We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations, and demonstrate that, so long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice. The transition mass disappears entirely, however, if star formation driven outflows are absent.}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -month = {jul}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Ferrero2017, -abstract = {The Tully-Fisher relation (TFR) links the stellar mass of a disc galaxy, Mstr, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling (M ∝ V3) of dark matter haloes, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to deviate substantially from a single power law and to evolve rapidly with redshift. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of $\Lambda$ cold dark matter ($\Lambda$CDM) cosmological simulations. Matching both relations requires disc sizes to satisfy constraints given by the concentration of haloes and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. $\Lambda$CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1607.03100}, -author = {Ferrero, Ismael and Navarro, Julio F. and Abadi, Mario G. and Sales, Laura V. and Bower, Richard G. and Crain, Robert A. and Frenk, Carlos S. and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw2691}, -eprint = {1607.03100}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ferrero et al. - 2017 - Size matters Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {4}, -pages = {4736--4746}, -title = {{Size matters: Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE}}, -volume = {464}, -year = {2017} -} -@article{Schaller2015, -abstract = {We use the 'Evolution and assembly of galaxies and their environments' (EAGLE) cosmological simulation to investigate the effect of baryons on the density profiles of rich galaxy clusters. We focus on EAGLE clusters with M200 > 1014M⊙ of which we have six examples. The central brightest cluster galaxies (BCGs) in the simulation have steep stellar density profiles, $\rho$*(r)∝r-3. Stars dominate the mass density for r < 10 kpc, and, as a result, the total mass density profiles are steeper than the Navarro-Frenk-White (NFW) profile, in remarkable agreement with observations. The dark matter halo itself closely follows the NFW form at all resolved radii (r ≳ 3.0 kpc). The EAGLE BCGs have similar surface brightness and line-of-sight velocity dispersion profiles as the BCGs in the sample of Newman et al., which have the most detailed measurements currently available. After subtracting the contribution of the stars to the central density, Newman et al. infer significantly shallower slopes than the NFW value, in contradiction with the EAGLE results. We discuss possible reasons for this discrepancy, and conclude that an inconsistency between the kinematical model adopted by Newman et al. for their BCGs, which assumes isotropic stellar orbits, and the kinematical structure of the EAGLE BCGs, in which the orbital stellar anisotropy varies with radius and tends to be radially biased, could explain at least part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1409.8297}, -author = {Schaller, Matthieu and Frenk, Carlos S. and Bower, Richard G. and Theuns, Tom and Trayford, James and Crain, Robert A. and Furlong, Michelle and Schaye, Joop and Vecchia, Claudio Dalla and McCarthy, I. G.}, -doi = {10.1093/mnras/stv1341}, -eprint = {1409.8297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: clusters: general,Galaxies: haloes}, -month = {sep}, -number = {1}, -pages = {343--355}, -title = {{The effect of baryons on the inner density profiles of rich clusters}}, -url = {http://adsabs.harvard.edu/abs/2014arXiv1409.8297S}, -volume = {452}, -year = {2015} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/de Vaucouleurs - 2005 - Author Index.pdf:pdf}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287--a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{Pontzen2015a, -abstract = {Galaxies and the dark matter haloes that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealized calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter core-creation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are 'maximally stable', i.e. that do not evolve at first order when external potentials (which arise from baryons, large-scale tidal fields or infalling substructure) are applied. We show that a spherically symmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for near-isotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealized spherically symmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter haloes (formed in collisionless cosmological simulations) nearly attain our maximally stable limit, but their evolution freezes out before reaching it.}, -archivePrefix = {arXiv}, -arxivId = {1502.07356}, -author = {Pontzen, Andrew and Read, Justin I. and Teyssier, Romain and Governato, Fabio and Gualandris, Alessia and Roth, Nina and Devriendt, Julien}, -doi = {10.1093/mnras/stv1032}, -eprint = {1502.07356}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pontzen et al. - 2015 - Milking the spherical cow - on aspherical dynamics in spherical coordinates(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {1366--1379}, -title = {{Milking the spherical cow - on aspherical dynamics in spherical coordinates}}, -volume = {451}, -year = {2015} -} -@article{Newman2012a, -abstract = {The presence of extremely compact galaxies at z ∼ 2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 galaxies selected with 0.4 {\textless} z {\textless} 2.5 and stellar masses M* {\textgreater} 1010.7 M {\textperiodcentered}in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and the mean size of these systems at fixed stellar mass grows by a factor of 3.5 0.3 over this redshift interval. The data are sufficiently deep to identify companions to these hosts whose stellar masses are ten times smaller. By searching for these around 404 quiescent hosts within a physical annulus 10 h -1 kpc {\textless} R {\textless} 30 h -1 kpc, we estimate the minor merger rate over 0.4 {\textless} z {\textless} 2. We find that 13{\%}-18{\%} of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6{\%} ± 2{\%} per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers may explain most of the size evolution observed at z ≲ 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes. {\textcopyright}2012 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1110.1637}, -author = {Newman, Andrew B and Ellis, Richard S and Bundy, Kevin and Treu, Tommaso}, -doi = {10.1088/0004-637X/746/2/162}, -eprint = {1110.1637}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: structure}, -number = {2}, -title = {{Can minor merging account for the size growth of quiescent galaxies? New results from the CANDELS survey}}, -volume = {746}, -year = {2012} -} -@article{Schombert2013, -abstract = {Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the S{\'{e}}rsic r 1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the S{\'{e}}rsic r 1/n model produces good fits to the core regions of ellipticals (r{\textless}r half), but is an inadequate function for the entire profile of an elliptical from core to halo due to competing effects on the S{\'{e}}rsic n index and the fact that the interior shape of an elliptical is only weakly correlated with its halo shape. In addition, there are a wide range of S{\'{e}}rsic parameters that will equally describe the shape of the outer profile, degrading the S{\'{e}}rsic model's usefulness as a describer of the entire profile. Empirically determined parameters, such as half-light radius and total luminosity, have less scatter than fitting function variables. The scaling relations for ellipticals are often non-linear, but for ellipticals brighter than MJ {\textless}-23 the following structural relations are found: L ∞ r 0.8±0.1, L ∞ $\Sigma$-0.5±0.1, and $\Sigma$ ∞ r -1.5±0.1. {\textcopyright}2013 Astronomical Society of Australia.}, -archivePrefix = {arXiv}, -arxivId = {1303.4710}, -author = {Schombert, J M}, -doi = {10.1017/pas.2013.010}, -eprint = {1303.4710}, -issn = {13233580}, -journal = {Publications of the Astronomical Society of Australia}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: star formation,galaxies: structure}, -number = {1}, -title = {{The structure of galaxies: II. Fitting functions and scaling relations for ellipticals}}, -url = {http://arxiv.org/abs/1303.4710%7B%5C%25%7D0Ahttp://dx.doi.org/10.1017/pas.2013.010}, -volume = {30}, -year = {2013} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. with the particletagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of {\$\sim${}}1900 massive dark matter haloes (1012-1014M⊙) from the Millennium II $\lambda$ cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of MilkyWay-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a S{\`{e}}rsic profile, the radial scale and amplitude of which vary systematically with halo mass (M200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M* and M200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z ≈ 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S and White, Simon D M}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Sales2012, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {jun}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Wilson1995, -abstract = {The recent development of unified theories of active galactic nuclei (AGNs) has indicated that there are two physically distinct classes of these objects--radio-loud and radio-quiet. Despite differences, the (probable) thermal emissions from the AGNs (continua and lines from X-ray to infrared wavelengths) are quite similar to the two classes of object. We argue that this last result suggests that the black hole masses and mass accretion rates in the two classes are not greatly different, and that the difference between the classes is associated with the spin of the black hole. We assume that the normal process of accretion through a disk does not lead to rapidly spinning holes and propose that galaxies (e.g., spirals) which have not suffered a recent major merger event contain nonrotating or only slowly rotating black holes. When two such galaxies merge, the two black holes are known to form a binary and we assume that they eventually coalesce. The ratio of the number of radio-loud to radio-quiet AGNs at a given thermal (e.g., optical) luminosity is determined by the galaxy merger rate. Comparisons between the predicted and observed radio luminosity functions constrain the efficiencies with which jet power is extracted from the spinning hole and radio emission is produced by the jet.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9408005}, -author = {Wilson, A S and Colbert, E J M}, -doi = {10.1086/175054}, -eprint = {9408005}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Active Galactic Nuclei,Black Holes (Astronomy),Cosmology,Interacting Galaxies,Luminosity,Quasars,Radio Astronomy,Radio Jets (Astronomy)}, -month = {jan}, -pages = {62}, -primaryClass = {astro-ph}, -title = {{The difference between radio-loud and radio-quiet active galaxies}}, -url = {http://adsabs.harvard.edu/doi/10.1086/175054}, -volume = {438}, -year = {2002} -} -@article{Martizzi2013, -abstract = {In a recent study, we used cosmological simulations to show that active galactic nuclei (AGN) feedback on the gas distribution in clusters of galaxies can be important in determining the spatial distribution of stars and dark matter in the central regions of these systems. The hierarchical assembly of dark matter, baryons and black holes obscures the physical mechanism behind the restructuring process. Here, we use idealized simulations to follow the response of a massive dark matter halo as we feed the central black hole with a controlled supply of cold gas. This removes most of the complexity taking place in the cosmological simulations that may have biased our previous study.We confirm our previous results: gas heated and expelled from the central regions of the halo by AGN feedback can return after cooling; repeated cycles generate gravitational potential fluctuations responsible for irreversible modifications of the dark matter mass profile. The main result is the expulsion of large amounts of baryons and dark matter from the central regions of the halo. According to the work presented here, outflowinduced fluctuations represent the only mechanism able to efficiently create dark matter cores in clusters of galaxies. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1211.2648}, -author = {Martizzi, Davide and Teyssier, Romain and Moore, Ben}, -doi = {10.1093/mnras/stt297}, -eprint = {1211.2648}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cosmology: theory,Galaxies: clusters: general,Galaxies: formation,Large-scale structure of universe,Methods: numerical}, -month = {jul}, -number = {3}, -pages = {1947--1954}, -title = {{Cusp-core transformations induced by AGN feedback in the progenitors of cluster galaxies}}, -volume = {432}, -year = {2013} -} -@article{Despali2022, -abstract = {This paper aims to quantify how the lowest halo mass that can be detected with galaxy-galaxy strong gravitational lensing depends on the quality of the observations and the characteristics of the observed lens systems. Using simulated data, we measure the lowest detectable NFW mass at each location of the lens plane, in the form of detailed sensitivity maps. In summary, we find that: (i) the lowest detectable mass Mlow decreases linearly as the signal-to-noise ratio (SNR) increases and the sensitive area is larger when we decrease the noise; (ii) a moderate increase in angular resolution (0.07′′ versus 0.09′′) and pixel scale (0.01′′ versus 0.04′′) improves the sensitivity by on average 0.25 dex in halo mass, with more significant improvement around the most sensitive regions; (iii) the sensitivity to low-mass objects is largest for bright and complex lensed galaxies located inside the caustic curves and lensed into larger Einstein rings (i.e rE ≥ 1.0′′). We find that for the sensitive mock images considered in this work, the minimum mass that we can detect at the redshift of the lens lies between 1.5 × 108 and 3 × 109 M☉. We derive analytic relations between Mlow, the SNR and resolution and discuss the impact of the lensing configuration and source structure. Our results start to fill the gap between approximate predictions and real data and demonstrate the challenging nature of calculating precise forecasts for gravitational imaging. In light of our findings, we discuss possible strategies for designing strong lensing surveys and the prospects for HST, Keck, ALMA, Euclid and other future observations.}, -archivePrefix = {arXiv}, -arxivId = {2111.08718}, -author = {Despali, Giulia and Vegetti, Simona and White, Simon D.M. and Powell, Devon M. and Stacey, Hannah R. and Fassnacht, Christopher D. and Rizzo, Francesca and Enzi, Wolfgang}, -doi = {10.1093/mnras/stab3537}, -eprint = {2111.08718}, -file = {:C\:/Users/Jammy/Documents/Papers/Substructure/Despali2021Senstitoty.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmology: Observations,Dark matter,Galaxies: High-redshift,Gravitational lensing: Strong,Methods: Data analysis}, -number = {2}, -pages = {2480--2494}, -title = {{Detecting low-mass haloes with strong gravitational lensing I: the effect of data quality and lensing configuration}}, -volume = {510}, -year = {2022} -} -@article{Minka2009, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture models is not well captured by factor graphs unless the entire mixture is represented by one factor, because the message equations have a containment structure. Gates capture this containment structure graphically, allowing both the independences and the message-passing equations for a model to be readily visualized. Different variational approximations for mixture models can be understood as different ways of drawing the gates in a model. We present general equations for expectation propagation and variational message passing in the presence of gates.}, -author = {Minka, Tom and Winn, John}, -doi = {10.5790/hongkong/9789888083091.003.0088}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Minka, Winn - 2009 - Gates.pdf:pdf}, -isbn = {9781605609492}, -issn = {0018702X}, -journal = {Advances in Neural Information Processing Systems 21 - Proceedings of the 2008 Conference}, -pages = {1073--1080}, -title = {{Gates}}, -year = {2009} -} -@article{Pontzen2014, -abstract = {A principal discovery in modern cosmology is that standard model particles comprise only 5 per cent of the mass-energy budget of the Universe. In the $\Lambda$CDM paradigm, the remaining 95 per cent consists of dark energy ($\Lambda$) and cold dark matter. $\Lambda$CDM is being challenged by its apparent inability to explain the low-density 'cores' of dark matter measured at the centre of galaxies, where centrally concentrated high-density 'cusps' were predicted. But before drawing conclusions, it is necessary to include the effect of gas and stars, historically seen as passive components of galaxies. We now understand that these can inject heat energy into the cold dark matter through a coupling based on rapid gravitational potential fluctuations, explaining the observed low central densities. {\textcopyright} 2014 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1402.1764}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1038/nature12953}, -eprint = {1402.1764}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pontzen, Governato - 2014 - Cold dark matter heats up.pdf:pdf}, -isbn = {1476-4687 (Electronic)$\$r0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -number = {7487}, -pages = {171--178}, -pmid = {24522596}, -title = {{Cold dark matter heats up}}, -volume = {506}, -year = {2014} -} -@article{Wertz2018, -abstract = {Modern time-delay cosmography aims to infer the cosmological parameters with a competitive precision from observing a multiply imaged quasar. The success of this technique relies upon a robust modeling of the lens mass distribution. Unfortunately strong degeneracies between density profiles that lead to almost the same lensing observables may bias precise estimates of the Hubble constant. The source position transformation (SPT), which covers the well-known mass-sheet transformation (MST) as a special case, defines a new framework to investigate these degeneracies. In this paper, we present pySPT, a python package dedicated to the SPT. We describe how it can be used to evaluate the impact of the SPT on lensing observables. We review most of its capabilities and elaborate on key features that we used in a companion paper regarding SPT and time delays. The pySPT program also comes with a subpackage dedicated to simple lens modeling. This can be used to generate lensing related quantities for a wide variety of lens models independent of any SPT analysis. As a first practical application, we present a correction to the first estimate of the impact on time delays of the SPT, which has been experimentally found in a previous work between a softened power law and composite (baryons + dark matter) lenses. We find that the large deviations previously predicted have been overestimated because of a minor bug in the public lens modeling code lensmodel (v1.99), which is now fixed. We conclude that the predictions for the Hubble constant deviate by ∼7%, first and foremost as a consequence of an MST. The latest version of pySPT is available on Github, a software development platform, along with some tutorials to describe in detail how making the best use of pySPT.}, -archivePrefix = {arXiv}, -arxivId = {1801.04151}, -author = {Wertz, Olivier and Orthen, Bastian}, -doi = {10.1051/0004-6361/201732242}, -eprint = {1801.04151}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wertz, Orthen - 2018 - A dedicated source-position transformation package PySPT(2).pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Cosmological parameters,Gravitational lensing: Strong}, -pages = {1--9}, -title = {{A dedicated source-position transformation package: PySPT}}, -url = {http://arxiv.org/abs/1801.04151%0Ahttp://dx.doi.org/10.1051/0004-6361/201732242}, -volume = {619}, -year = {2018} -} -@article{Suyu2016, -abstract = {Strong gravitational lens systems with time delays between the multiple images allow measurements of time-delay distances, which are primarily sensitive to the Hubble constant that is key to probing dark energy, neutrino physics and the spatial curvature of the Universe, as well as discovering new physics. We present H0LiCOW (H0 Lenses in COSMOGRAIL's Wellspring), a program that aims to measure H0 with < 3.5 per cent uncertainty from five lens systems (B1608+656, RXJ1131-1231, HE 0435-1223, WFI2033-4723 and HE 1104-1805). We have been acquiring (1) time delays through COSMOGRAIL and Very Large Array monitoring, (2) high-resolution Hubble Space Telescope imaging for the lens mass modelling, (3) wide-field imaging and spectroscopy to characterize the lens environment and (4) moderate-resolution spectroscopy to obtain the stellar velocity dispersion of the lenses for mass modelling. In cosmological models with one-parameter extension to flat $\Lambda$ cold dark matter, we expect to measure H0 to < 3.5 per cent in most models, spatial curvature $\Omega$k to 0.004, w to 0.14 and the effective number of neutrino species to 0.2 (1$\sigma$ uncertainties) when combined with current cosmic microwave background (CMB) experiments. These are, respectively, a factor of $\sim$15, $\sim$2 and $\sim$1.5 tighter than CMB alone. Our data set will further enable us to study the stellar initial mass function of the lens galaxies, and the co-evolution of supermassive black holes and their host galaxies. This program will provide a foundation for extracting cosmological distances from the hundreds of time-delay lenses that are expected to be discovered in current and future surveys.}, -archivePrefix = {arXiv}, -arxivId = {1607.00017}, -author = {Suyu, S. H. and Bonvin, V. and Courbin, F. and Fassnacht, C. D. and Rusu, C. E. and Sluse, D. and Treu, T. and Wong, K. C. and Auger, M. W. and Ding, X. and Hilbert, S. and Marshall, P. J. and Rumbaugh, N. and Sonnenfeld, A. and Tewes, M. and Tihhonova, O. and Agnello, A. and Blandford, R. D. and Chen, G. C.F. and Collett, T. and Koopmans, L. V.E. and Liao, K. and Meylan, G. and Spiniello, C.}, -doi = {10.1093/mnras/stx483}, -eprint = {1607.00017}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Suyu et al. - 2017 - H0LiCOW - I. H0 Lenses in COSMOGRAIL's Wellspring Program overview(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Distance scale,Galaxies: structure,Gravitational lensing: strong,HE 0435-1223,HE 1104-1805,Quasars: individual:B1608+656,RXJ1131-1231,WFI2033-4723}, -number = {3}, -pages = {2590--2604}, -title = {{H0LiCOW - I. H0 Lenses in COSMOGRAIL's Wellspring: Program overview}}, -url = {http://arxiv.org/abs/1607.00017%0Ahttp://dx.doi.org/10.1093/mnras/stx483}, -volume = {468}, -year = {2017} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) "CMASS" sample at {\$}z\backslashbackslashsim0.5{\$}. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogs which include selection effects, reproduce the overall SMF, the projected two-point correlation function {\$}w{\_}{\{}\backslashbackslashrm p{\}}{\$}, the CMASS {\$}dn/dz{\$}, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of "age matching" and show that these effects are markedly different compared to the ones explored by Hearin et al. (2013) at lower stellar masses. We construct two models, one in which galaxy color is stochastic ("AbM" model) as well as a model which contains assembly bias effects ("AgM" model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colors are not a stochastic process in high-mass halos. Our results suggest that the colors of galaxies in high-mass halos are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P and Bundy, Kevin and Zentner, Andrew R and Behroozi, Peter S and Reid, Beth A and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L and White, Martin and Schneider, Donald P}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Wertz2018, -abstract = {The modern time-delay cosmography aims to infer the cosmological parameters with a competitive precision from observing a multiply imaged quasar. The success of this technique relies upon a robust modeling of the lens mass distribution. Unfortunately strong degeneracies between density profiles that lead to almost the same lensing observables may bias precise estimate for the Hubble constant. The source position transformation (SPT), which covers the well-known mass sheet transformation (MST) as a special case, defines a new framework to investigate these degeneracies. In this paper, we present pySPT, a Python package dedicated to the SPT. We describe how it can be used to evaluate the impact of the SPT on lensing observables. We review most of its capabilities and elaborate on key features that we used in a companion paper regarding SPT and time delays. pySPT also comes with a sub-package dedicated to simple lens modeling. It can be used to generate lensing related quantities for a wide variety of lens models, independently from any SPT analysis. As a first practical application, we present a correction to the first estimate of the impact on time delays of the SPT, which has been experimentally found in Schneider and Sluse (2013) between a softened power-law and a composite (baryons + dark matter) lenses. We find that the large deviations predicted in Schneider and Sluse (2014) have been overestimated due to a minor bug (now fixed) in the public lens modeling code lensmodel (v1.99). We conclude that the predictions for the Hubble constant deviate by {\$}\backslashbackslashsim 7{\$}{\$}\backslash{\$}{\%}, first and foremost caused by an MST. The latest version of pySPT is available at https://github.com/owertz/pySPT. We also provide tutorials to describe in detail how making the best use of pySPT at https://github.com/owertz/pySPT{\_}tutorials.}, -archivePrefix = {arXiv}, -arxivId = {1801.04151}, -author = {Wertz, Olivier and Orthen, Bastian}, -eprint = {1801.04151}, -keywords = {cosmological parameters,gravitational lensing,strong}, -pages = {1--9}, -title = {{pySPT: a package dedicated to the source position transformation}}, -url = {http://arxiv.org/abs/1801.04151}, -year = {2018} -} -@article{Morganti2013, -abstract = {NGC 4494 is one of several intermediate-luminosity elliptical galaxies inferred to have an unusually diffuse dark matter halo. We use the chi{\^{}}2-made-to-measure particle code NMAGIC to construct axisymmetric models of NGC 4494 from photometric and various kinematic data. The extended kinematics include light spectra in multiple slitlets out to 3.5 R{\_}e, and hundreds of planetary nebulae velocities out to {\$\sim${}}7 R{\_}e, thus allowing us to probe the dark matter content and orbital structure in the halo. We use Monte Carlo simulations to estimate confidence boundaries for the halo parameters, given our data and modelling set-up. We find that the true potential of the dark matter halo is recovered within Delta G (merit function){\textless}26 (Delta chi{\^{}}2{\textless}59) at 70{\%} confidence level (C.L.), and within Delta G{\textless}32 (Delta chi{\^{}}2{\textless}70) at 90{\%} C.L.. These numbers are much larger than the usually assumed Delta chi{\^{}}2=2.3 (4.6) for 70{\%} (90{\%}) C.L. for two free parameters, perhaps case-dependent, but calling into question the general validity of the standard assumptions used for halo and black hole mass determinations. The best-fitting models for NGC 4494 have a dark matter fraction of about 0.6$\backslash$pm0.1 at 5R{\_}e (70{\%} C.L.), and are embedded in a dark matter halo with circular velocity {\$\sim${}}200 km/s. The total circular velocity curve (CVC) is approximately flat at v{\_}c=220 km/s outside {\$\sim${}}0.5R{\_}e. The orbital anisotropy of the stars is moderately radial. These results are independent of the assumed inclination of the galaxy, and edge-on models are preferred. Comparing with the halos of NGC 3379 and NGC 4697, whose velocity dispersion profiles also decrease rapidly from the center outwards, the outer CVCs and dark matter halos are quite similar. NGC 4494 shows a particularly high dark matter fraction inside {\$\sim${}}3R{\_}e, and a strong concentration of baryons in the center.}, -archivePrefix = {arXiv}, -arxivId = {1303.2688}, -author = {Morganti, Lucia and Gerhard, Ortwin and Coccato, Lodovico and Martinez-valpuesta, Inma and Arnaboldi, Magda}, -doi = {10.1093/mnras/stt442}, -eprint = {1303.2688}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: individual: NGC 4494,Galaxies: kinematics and dynamics,Methods: numerical,cD}, -number = {4}, -pages = {3570--3588}, -title = {{Elliptical galaxies with rapidly decreasing velocity dispersion profiles: Nmagic models and dark halo parameter estimates for NGC 4494}}, -volume = {431}, -year = {2013} -} -@article{Roy:2018aa, -abstract = {We have obtained structural parameters of about 340 000 galaxies from the Kilo-Degree Survey (KiDS) in 153 deg2 of data release 1, 2, and 3.We have performed a seeing convolved 2D single S{\'{e}}rsic fit to the galaxy images in the four photometric bands (u, g, r, i) observed by KiDS, by selecting high signal-to-noise ratio (S/N > 50) systems in every bands. We have classified galaxies as spheroids and disc-dominated by combining their spectral energy distribution properties and their S{\'{e}}rsic index. Using photometric redshifts derived from a machine learning technique, we have determined the evolution of the effective radius, Re and stellar mass, M*, versus redshift, for both mass complete samples of spheroids and discdominated galaxies up to z$\sim$0.6. Our results show a significant evolution of the structural quantities at intermediate redshift for the massive spheroids (logM*/M⊙ > 11, Chabrier IMF), while almost no evolution has found for less massive ones (logM*/M⊙ < 11). On the other hand, disc dominated systems show a milder evolution in the less massive systems (logM*/M⊙ < 11) and possibly no evolution of the more massive systems. These trends are generally consistent with predictions from hydrodynamical simulations and independent datasets out to redshift z $\sim$ 0.6, although in some cases the scatter of the data is large to drive final conclusions. These results, based on 1/10 of the expected KiDS area, reinforce precedent finding based on smaller statistical samples and show the route towards more accurate results, expected with the the next survey releases.}, -archivePrefix = {arXiv}, -arxivId = {1807.06085}, -author = {Roy, N. and Napolitano, N. R. and {La Barbera}, F. and Tortora, C. and Getman, F. and Radovich, M. and Capaccioli, M. and Brescia, M. and Cavuoti, S. and Longo, G. and Raj, M. A. and Puddu, E. and Covone, G. and Amaro, V. and Vellucci, C. and Grado, A. and Kuijken, K. and {Verdoes Kleijn}, G. and Valentijn, E.}, -doi = {10.1093/mnras/sty1917}, -eprint = {1807.06085}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Roy et al. - 2018 - Evolution of galaxy size-stellar mass relation from the Kilo-Degree Survey(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution}, -month = {oct}, -number = {1}, -pages = {1057--1080}, -title = {{Evolution of galaxy size-stellar mass relation from the Kilo-Degree Survey}}, -volume = {480}, -year = {2018} -} -@article{Blanton2003, -abstract = {Using photometry and spectroscopy of 144,609 galaxies from the Sloan Digital Sky Survey, we present bivariate distributions of pairs of seven galaxy properties: four optical colors, surface brightness, radial profile shape as measured by the Sersic index, and absolute magnitude. In addition, we present the dependence of local galaxy density (smoothed on 8 h{\^{}}{\{}-1{\}} Mpc scales) on all of these properties. Several classic, well-known relations among galaxy properties are evident at extremely high signal-to-noise ratio: the color-color relations of galaxies, the color-magnitude relations, the magnitude-surface brightness relation, and the dependence of density on color and absolute magnitude. We show that most of the i-band luminosity density in the universe is in the absolute magnitude and surface brightness ranges used. Some of the relationships between parameters, in particular the color--magnitude relations, show stronger correlations for exponential galaxies and concentrated galaxies taken separately than for all galaxies taken together. We provide a simple set of fits of the dependence of galaxy properties on luminosity for these two sets of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0209479}, -author = {Blanton, M R and Hogg, D W and Bahcall, N A and Baldry, I K and Brinkmann, J and Csabai, I and Eisenstein, D J and Fukugita, M and Gunn, J E and Ivezic, Z and Lamb, D Q and Lupton, R H and Loveday, J and Munn, J A and Nichol, R C and Okamura, S and Schlegel, D J and Shimasaku, K and Strauss, M A and Vogeley, M S and Weinberg, D H}, -doi = {10.1086/375528}, -eprint = {0209479}, -isbn = {0004-6256}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Fundamental Parameters,Galaxies: Photometry,Galaxies: Statistics}, -month = {sep}, -number = {1}, -pages = {186--207}, -pmid = {19408790}, -primaryClass = {astro-ph}, -title = {{The Broad-band Optical Properties of Galaxies with Redshifts 0.0 {\textless} z {\textless} 0.2}}, -url = {http://arxiv.org/abs/astro-ph/0209479%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/375528}, -volume = {594}, -year = {2002} -} -@article{Kotilainen2018, -archivePrefix = {arXiv}, -arxivId = {arXiv:1409.1948v1}, -author = {Kotilainen, J K and Falomo, R and Decarli, R and Karhunen, K and Uslenghi, M}, -eprint = {arXiv:1409.1948v1}, -keywords = {active,bulges,galaxies,general,nuclei,quasars,supermassive black holes}, -number = {October}, -pages = {1--9}, -title = {{The black hole - host galaxy relation for very low-mass quasars.}}, -volume = {9}, -year = {2018} -} -@article{Schombert2013, -abstract = {Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the S{\'{e}}rsic r 1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the S{\'{e}}rsic r 1/n model produces good fits to the core regions of ellipticals (r 108 M☉}, -archivePrefix = {arXiv}, -arxivId = {2211.15679}, -author = {O'Riordan, Conor M. and Despali, Giulia and Vegetti, Simona and Lovell, Mark R. and Molin{\'{e}}, {\'{A}}ngeles}, -doi = {10.1093/mnras/stad650}, -eprint = {2211.15679}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/ORiodan2023Euclid.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {dark matter,gravitational lensing: strong}, -number = {2}, -pages = {2342--2356}, -title = {{Sensitivity of strong lensing observations to dark matter substructure: a case study with Euclid}}, -volume = {521}, -year = {2023} -} -@article{Holl2012, -abstract = {Gaia, the next astrometric mission of the European Space Agency, will use a camera composed of 106 CCDs to collect multiple observations for one billion stars. The astrometric core solution of Gaia will use the estimated location of the stellar images on the CCDs to derive the astrometric parameters (position, parallax and proper motion) of the stars. The Gaia CCDs will suffer from charge transfer inefficiency (CTI) mainly caused by radiation damage. CTI is expected to significantly degrade the quality of the collected images which ultimately affects the astrometric accuracy of Gaia. This paper is the second and last in a study aiming at characterizing and quantifying the impact of CCD radiation damage on Gaia astrometry. Here we focus on the effect of the image location errors induced by CTI on the astrometric solution. We apply the Gaia Astrometric Global Iterative Solution (AGIS) to simulated Gaia-like observations for 1 million stars including CTI-induced errors as described in the first paper. We show that a magnitude-dependent image location bias is propagated in the astrometric solution, biasing the estimation of the astrometric parameters as well as decreasing its precision. We demonstrate how the Gaia scanning law dictates this propagation and the ultimate sky distribution of the CTI-induced errors. The possibility of using the residuals of the astrometric solution to improve the calibration of the CTI effects is investigated. We also estimate the astrometric errors caused by (faint) disturbing stars preceding the stellar measurements on the CCDs. Finally, we show that, for single stars, the overall astrometric accuracy of Gaia can be preserved to within 10per cent of the CTI-free case for all magnitudes by appropriate modelling at the image location estimation level and using the solution residuals. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.1547}, -author = {Holl, B and Prod'homme, T and Lindegren, L and Brown, A G A}, -doi = {10.1111/j.1365-2966.2012.20429.x}, -eprint = {1110.1547}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: numerical,Space vehicles}, -number = {4}, -pages = {2786--2807}, -title = {{The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solution}}, -volume = {422}, -year = {2012} -} -@article{Perlmutter1997, -abstract = {We have developed a technique to systematically discover and study high-redshift supernovae that can be used to measure the cosmological parameters. We report here results based on the initial seven of >28 supernovae discovered to date in the high-redshift supernova search of the Supernova Cosmology Project. We find a dispersion in peak magnitudes of sigma_{M_B} = 0.27 this dispersion narrows to sigma_{M_B,corr} = 0.19 after "correcting" the magnitudes using the light-curve "width-luminosity" relation found for nearby (z <= 0.1) type Ia supernovae from the Calan/Tololo survey (Hamuy et al. 1996). Comparing lightcurve-width-corrected magnitudes as a function of redshift of our distant (z = 0.35-0.46) supernovae to those of nearby type Ia supernovae yields a global measurement of the mass density, Omega_M = 0.88^{+0.69}_{-0.60} for a Lambda = 0 cosmology. For a spatially flat universe (i.e., Omega_M +Omega_Lambda = 1), we find Omega_M = 0.94 ^{+0.34}_{-0.28} or, equivalently, a measurement of the cosmological constant, Omega_Lambda = 0.06 ^{+0.28}_{-0.34} (<0.51 at the 95% confidence level). For the more general Friedmann-Lemaitre cosmologies with independent Omega_M and Omega_Lambda, the results are presented as a confidence region on the Omega_M-Omega_Lambda plane. This region does not correspond to a unique value of the deceleration parameter q_0. We present analyses and checks for statistical and systematic errors, and also show that our results do not depend on the specifics of the width-luminosity correction. The results for Omega_Lambda-versus-Omega_M are inconsistent with Lambda-dominated, low density, flat cosmologies that have been proposed to reconcile the ages of globular cluster stars with higher Hubble constant values.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9608192}, -author = {Perlmutter, S. and Gabi, S. and Goldhaber, G. and Goobar, A. and Groom, D. E. and Hook, I. M. and Kim, A. G. and Kim, M. Y. and Lee, J. C. and Pain, R. and Pennypacker, C. R. and Small, I. A. and Ellis, R. S. and McMahon, R. G. and Boyle, B. J. and Bunclark, P. S. and Carter, D. and Irwin, M. J. and Glazebrook, K. and Newberg, H. J. M. and Filippenko, A. V. and Matheson, T. and Dopita, M. and Couch, W. J.}, -doi = {10.1086/304265}, -eprint = {9608192}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {3-Pronto,Cosmology,Dark Energy}, -month = {jul}, -number = {2}, -pages = {565--581}, -primaryClass = {astro-ph}, -title = {{ Measurements of the Cosmological Parameters $\Omega$ and $\Lambda$ from the First Seven Supernovae at z ≥ 0.35 }}, -url = {http://stacks.iop.org/0004-637X/483/i=2/a=565}, -volume = {483}, -year = {1997} -} -@article{Hubble1926, -abstract = {This contribution gives the results of a statistical investigation of 400 extragalactic nebulae for which Holetschek has determined total visual magnitudes. The list is complete for the brighter nebulae in the northern sky and is representative to 12.5 mag. or fainter. The classification employed is based on the forms of the photographic images. About 3 per cent are irregular, but the remaining nebulae fall into a sequence of type forms characterized by rotational symmetry about dominating nuclei. The sequence is composed of two sections, the elliptical nebulae and the spirals, which merge into each other. Luminosity relations. - The distribution of magnitudes appears to be uniform throughout the sequence. For each type or stage in the sequence, the total magnitudes are related to the logarithms of the maximum diameters by the formula, mT = C - 5 log d, where C varies progressively from type to type, indicating a variation in diameter for a given magnitude or vice versa. By applying corrections to C, the nebulae can be reduced to a standard type and then a single formula expresses the relation for all nebulae from the Magellanic Clouds to the faintest that can be classified. When the minor diameter is used, the value of C is approximately constant throughout the entire sequence. The coefficient of log d corresponds with the inverse-square law, which suggests that the nebulae are all of the same order of absolute luminosity and that apparent magnitudes are measures of distance. This hypothesis is supported by similar results for the nuclear magnitudes and the magnitudes of the brightest stars involved, and by the small range in luminosities among nebulae whose distances are already known. Distances and absolute dimensions. - The mean absolute visual magnitude, as derived from the nebulae whose distances are known, is -15.2. The statistical expression for the distance in parsecs is then log D = 4.04 + 0.2 mT. where mT is the total apparent magnitude. This leads to mean values for absolute dimensions at various stages in the sequence of types. Masses appear to be of the order of 2.6x108 Msun. Distribution and density of space. - To apparent magnitude about 16.7, corresponding to an exposure of one hour on fast plates with the 60-inch reflector, the numbers of nebulae to various limits of total magnitude vary directly with the volumes of space represented by the limits. This indicates an approximately uniform density of space, of the order of one nebula per 1017 cubic parsecs or 1.5x10-31 in C.G.S. units. The corresponding radius of curvature of the finite universe of general relativity is of the order of 2.7x1010 parsecs, or about 600 times the distance at which normal nebulae can be detected with the 100-inch reflector.}, -author = {Hubble, E. P.}, -doi = {10.1086/143018}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {dec}, -pages = {321}, -title = {{Extragalactic nebulae.}}, -url = {http://adsabs.harvard.edu/doi/10.1086/143018}, -volume = {64}, -year = {1926} -} -@article{Chen2017a, -abstract = {Different types of sentences express sentiment in very different ways. Traditional sentence-level sentiment classification research focuses on one-technique-fits-all solution or only centers on one special type of sentences. In this paper, we propose a divide-and-conquer approach which first classifies sentences into different types, then performs sentiment analysis separately on sentences from each type. Specifically, we find that sentences tend to be more complex if they contain more sentiment targets. Thus, we propose to first apply a neural network based sequence model to classify opinionated sentences into three types according to the number of targets appeared in a sentence. Each group of sentences is then fed into a one-dimensional convolutional neural network separately for sentiment classification. Our approach has been evaluated on four sentiment classification datasets and compared with a wide range of baselines. Experimental results show that: (1) sentence type classification can improve the performance of sentence-level sentiment analysis; (2) the proposed approach achieves state-of-the-art results on several benchmarking datasets.}, -archivePrefix = {arXiv}, -arxivId = {1404.7828}, -author = {Chen, Tao and Xu, Ruifeng and He, Yulan and Wang, Xuan}, -doi = {10.1016/j.eswa.2016.10.065}, -eprint = {1404.7828}, -isbn = {0925-2312}, -issn = {09574174}, -journal = {Expert Systems with Applications}, -keywords = {Deep neural network,Natural language processing,Sentiment analysis}, -pages = {221--230}, -pmid = {19932002}, -title = {{Improving sentiment analysis via sentence type classification using BiLSTM-CRF and CNN}}, -volume = {72}, -year = {2017} -} -@article{Bouwens2015, -abstract = {The remarkable Hubble Space Telescope (HST) data sets from the CANDELS, HUDF09, HUDF12, ERS, and BoRG/HIPPIES programs have allowed us to map the evolution of the rest-frame UV luminosity function (LF) from z ∼ 10 to z ∼ 4. We develop new color criteria that more optimally utilize the full wavelength coverage from the optical, near-IR, and mid-IR observations over our search fields, while simultaneously minimizing the incompleteness and eliminating redshift gaps. We have identified 5859, 3001, 857, 481, 217, and 6 galaxy candidates at z ∼ 4, z ∼ 5, z ∼ 6, z ∼ 7, z ∼ 8, and z ∼ 10, respectively, from the ∼1000 arcmin2 area covered by these data sets. This sample of >10,000 galaxy candidates at z ≥ 4 is by far the largest assembled to date with HST. The selection of z ∼ 4-8 candidates over the five CANDELS fields allows us to assess the cosmic variance; the largest variations are at z ≥ 7. Our new LF determinations at z ∼ 4 and z ∼ 5 span a 6 mag baseline and reach to -16 AB mag. These determinations agree well with previous estimates, but the larger samples and volumes probed here result in a more reliable sampling of >L∗ galaxies and allow us to reassess the form of the UV LFs. Our new LF results strengthen our earlier findings to 3.4$\sigma$ significance for a steeper faint-end slope of the UV LF at z ∼ 4, with $\alpha$ evolving from $\alpha$ = -2.06 ∓ 0.13 at to z ∼ 7 (and $\alpha$ = -2.02 ∓ 0.23 at z ∼ 8), consistent with that expected from the evolution of the halo mass function. We find less evolution in the characteristic magnitude M∗ from z ∼ 7 to z ∼ 4; the observed evolution in the LF is now largely represented by changes ∅∗ in . No evidence for a non-Schechter-like form to the z ∼ 4-8 LFs is found. A simple conditional LF model based on halo growth and evolution in the M/L ratio(∝(1+ ∼)-1.5 of halos provides a good representation of the observed evolution.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1403.4295v4}, -author = {Bouwens, R. J. and Illingworth, G. D. and Oesch, P. A. and Trenti, M. and Labb{\'{e}}, I. and Bradley, L. and Carollo, M. and {Van Dokkum}, P. G. and Gonzalez, V. and Holwerda, B. and Franx, M. and Spitler, L. and Smit, R. and Magee, D.}, -doi = {10.1088/0004-637X/803/1/34}, -eprint = {arXiv:1403.4295v4}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bouwens et al. - 2015 - UV luminosity functions at redshifts z ∼ 4 to z ∼ 10 10,000 galaxies from HST legacy fields.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {Galaxies: evolution,Glaxies: high-redshift}, -number = {1}, -pages = {1--49}, -title = {{UV luminosity functions at redshifts z ∼ 4 to z ∼ 10: 10,000 galaxies from HST legacy fields}}, -volume = {803}, -year = {2015} -} -@article{Young2022, -archivePrefix = {arXiv}, -arxivId = {arXiv:2202.13921v2}, -author = {Young, A J and Keeton, C R and Baker, A J}, -eprint = {arXiv:2202.13921v2}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Young2022ColorReg.pdf:pdf}, -keywords = {galaxies,gravitational lensing,high-redshift,kinematics and dynamics}, -title = {{A New Method for the Reconstruction of Strongly Lensed Galaxies with Resolved Kinematics}}, -year = {2022} -} -@article{Pontzen2014, -abstract = {A principal discovery in modern cosmology is that standard model particles comprise only 5 per cent of the mass-energy budget of the Universe. In the $\Lambda$CDM paradigm, the remaining 95 per cent consists of dark energy ($\Lambda$) and cold dark matter. $\Lambda$CDM is being challenged by its apparent inability to explain the low-density 'cores' of dark matter measured at the centre of galaxies, where centrally concentrated high-density 'cusps' were predicted. But before drawing conclusions, it is necessary to include the effect of gas and stars, historically seen as passive components of galaxies. We now understand that these can inject heat energy into the cold dark matter through a coupling based on rapid gravitational potential fluctuations, explaining the observed low central densities. {\textcopyright} 2014 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1402.1764}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1038/nature12953}, -eprint = {1402.1764}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pontzen, Governato - 2014 - Cold dark matter heats up.pdf:pdf}, -isbn = {1476-4687 (Electronic)\r0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -number = {7487}, -pages = {171--178}, -pmid = {24522596}, -title = {{Cold dark matter heats up}}, -volume = {506}, -year = {2014} -} -@article{LeFloch2005, -abstract = {We analyze a sample of {\$\sim${}}2600 MIPS/Spitzer 24mic sources brighter than {\$\sim${}}80muJy and located in the Chandra Deep Field South to characterize the evolution of the comoving infrared (IR) energy density of the Universe up to z{\$\sim${}}1. Using published ancillary optical data we first obtain a nearly complete redshift determination for the 24mic objects associated with R{\textless}24 counterparts at z{\textless}1. We find that the 24mic population at 0.5{\textless}z{\textless}1 is dominated by ``Luminous Infrared Galaxies'' (i.e., 10{\^{}}11 L{\_}sol {\textless} L{\_}IR {\textless} 10{\^{}}12 L{\_}sol), the counterparts of which appear to be also luminous at optical wavelengths and tend to be more massive than the majority of optically-selected galaxies. We finally derive 15mic and total IR luminosity functions (LFs) up to z{\$\sim${}}1. In agreement with the previous results from ISO and SCUBA and as expected from the MIPS source number counts, we find very strong evolution of the contribution of the IR-selected population with lookback time. Pure evolution in density is firmly excluded by the data, but we find considerable degeneracy between strict evolution in luminosity and a combination of increases in both density and luminosity (L*{\_}IR prop. to (1+z){\^{}}{\{}3.2{\_}{\{}-0.2{\}}{\^{}}{\{}+0.7{\}}{\}}, Phi*{\_}IR prop. to (1+z){\^{}}{\{}0.7{\_}{\{}-0.6{\}}{\^{}}{\{}+0.2{\}}{\}}). Our results imply that the comoving IR energy density of the Universe evolves as (1+z){\^{}}(3.9+/-0.4) up to z{\$\sim${}}1 and that galaxies luminous in the infrared (i.e., L{\_}IR {\textgreater} 10{\^{}}11 L{\_}IR) are responsible for 70+/-15{\%} of this energy density at z{\$\sim${}}1. Taking into account the contribution of the UV luminosity evolving as (1+z){\^{}}{\$\sim${}}2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z{\$\sim${}}0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24mic fluxes into luminosities.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506462}, -author = {{Le Floc'h}, Emeric and Papovich, Casey and Dole, Herve and Bell, Eric F and Lagache, Guilaine and Rieke, George H and Egami, Eiichi and Perez‐Gonzalez, Pablo G and Alonso‐Herrero, Almudena and Rieke, Marcia J and Blaylock, Myra and Engelbracht, Charles W and Gordon, Karl D and Hines, Dean C and Misselt, Karl A and Morrison, Jane E and Mould, Jeremy}, -doi = {10.1086/432789}, -eprint = {0506462}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Observations,Galaxies: Evolution,Galaxies: High-Redshift,Infrared: Galaxies}, -month = {oct}, -number = {1}, -pages = {169--190}, -primaryClass = {astro-ph}, -title = {{ Infrared Luminosity Functions from the Chandra Deep Field–South: The Spitzer View on the History of Dusty Star Formation at 0 ≲ z ≲ 1 }}, -url = {http://arxiv.org/abs/astro-ph/0506462%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/432789}, -volume = {632}, -year = {2005} -} -@article{Schaye2015, -abstract = {We introduce the Virgo Consortium's EAGLE project, a suite of hydrodynamical simulations that follow the formation of galaxies and black holes in representative volumes. We discuss the limitations of such simulations in light of their finite resolution and poorly constrained subgrid physics, and how these affect their predictive power. One major improvement is our treatment of feedback from massive stars and AGN in which thermal energy is injected into the gas without the need to turn off cooling or hydrodynamical forces, allowing winds to develop without predetermined speed or mass loading factors. Because the feedback efficiencies cannot be predicted from first principles, we calibrate them to the z$\sim$0 galaxy stellar mass function and the amplitude of the galaxy-central black hole mass relation, also taking galaxy sizes into account. The observed galaxy mass function is reproduced to $\lesssim 0.2$ dex over the full mass range, $10^8 < M_*/M_\odot \lesssim 10^{11}$, a level of agreement close to that attained by semi-analytic models, and unprecedented for hydrodynamical simulations. We compare our results to a representative set of low-redshift observables not considered in the calibration, and find good agreement with the observed galaxy specific star formation rates, passive fractions, Tully-Fisher relation, total stellar luminosities of galaxy clusters, and column density distributions of intergalactic CIV and OVI. While the mass-metallicity relations for gas and stars are consistent with observations for $M_* \gtrsim 10^9 M_\odot$, they are insufficiently steep at lower masses. The gas fractions and temperatures are too high for clusters of galaxies, but for groups these discrepancies can be resolved by adopting a higher heating temperature in the subgrid prescription for AGN feedback. EAGLE constitutes a valuable new resource for studies of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1407.7040}, -author = {Schaye, Joop and Crain, Robert A. and Bower, Richard G. and Furlong, Michelle and Schaller, Matthieu and Theuns, Tom and {Dalla Vecchia}, Claudio and Frenk, Carlos S. and Mccarthy, I. G. and Helly, John C. and Jenkins, Adrian and Rosas-Guevara, Y. M. and White, Simon D M and Baes, Maarten and Booth, C. M. and Camps, Peter and Navarro, Julio F. and Qu, Yan and Rahmati, Alireza and Sawala, Till and Thomas, Peter A. and Trayford, James}, -doi = {10.1093/mnras/stu2058}, -eprint = {1407.7040}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {jan}, -number = {1}, -pages = {521--554}, -title = {{The EAGLE project: Simulating the evolution and assembly of galaxies and their environments}}, -volume = {446}, -year = {2015} -} -@article{Keeton1997, -abstract = {Galaxies modeled as singular isothermal ellipsoids with an axis ratio distribution similar to the observed axis ratio distribution of E and S0 galaxies are statistically consistent with both the observed numbers of two-image and four-image lenses and the inferred ellipticities of individual lenses. However, no four-image lens is well fit by the model (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 20{\$}), the axis ratio of the model can be significantly different from that of the observed lens galaxy, and the major axes of the model and the galaxy may be slightly misaligned. We found that models with a second, independent, external shear axis could fit the data well (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 1{\$}), while adding the same number of extra parameters to the radial mass distribution does not produce such a dramatic improvement in the fit. An independent shear axis can be produced by misalignments between the luminous galaxy and its dark matter halo, or by external shear perturbations due to galaxies and clusters correlated with the primary lens or along the line of sight. We estimate that the external shear perturbations have no significant effect on the expected numbers of two-image and four-image lenses, but that they can be important perturbations in individual lens models. However, the amplitudes of the external shears required to produce the good fits are larger than our estimates for typical external shear perturbations (10-15{\%} shear instead of 1-3{\%} shear) suggesting that the origin of the extra angular structure must be intrinsic to the primary lens galaxy in most cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610163}, -author = {Keeton, C R and Kochanek, C S and Seljak, U}, -doi = {10.1086/304172}, -eprint = {9610163}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Elliptical and Lenticular,cD,cosmology: theory}, -number = {2}, -pages = {604--620}, -primaryClass = {astro-ph}, -title = {{Shear and Ellipticity in Gravitational Lenses}}, -url = {http://arxiv.org/abs/astro-ph/9610163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/304172}, -volume = {482}, -year = {1996} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@inproceedings{Grogin2010b, -author = {Grogin, N A and Lim, P L and Maybhate, A and Hook, R N and Loose, M}, -booktitle = {2010 HST Calibration Workshop}, -month = {jul}, -pages = {1--12}, -series = {Bulletin of the American Astronomical Society}, -title = {{Post-SM4 ACS / WFC Bias Striping : Characterization And Mitigation}}, -volume = {42}, -year = {2010} -} -@article{Brooks2015a, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disk galaxies. Under this bulge-formation model, though, the high rates of mergers in Cold Dark Matter galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disk galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Maio2014, -abstract = {We present results of cosmological N-body hydrodynamic chemistry simulations of primordial structure growth and evolution in a scenario with warm dark matter (WDM) having a mass of 3 keV (thermal relic) and compare with a model consisting of standard cold dark matter (CDM).We focus on the high-redshift universe (z > 6), where the structure formation process should better reflect the primordial (linear) differences in terms of matter power spectrum. We find that early epochs can be exceptional probes of the dark matter nature. Non-linear WDM power spectra and mass functions are up to 2 dex lower than in CDM and show spreads of factor of a few persisting in the whole first Gyr. Runaway molecular cooling in WDM haloes results severely inhibited because of the damping of power at large k modes and hence cosmic (Populations III and II-I) star formation rate (SFR) is usually suppressed with respect to CDM predictions. Luminous objects formed in a WDM background are very rare at z > 10, due to the sparser and retarded evolution of early WDM minihaloes during the dark ages and their lack can be fitted with a simple analytical formula depending only on magnitude and redshift. Future high-z observations of faint galaxies have the potential to discriminate between CDM and WDM scenarios by means of cosmic stellar mass density and specific SFR, as well. When compared to the effects of alternative cosmologies (e.g. non-Gaussian or dark energy models) or of high-order corrections at large z (e.g. primordial streaming motions or changes in the pristine initial mass function) the ones caused by WDM are definitely more dramatic.}, -archivePrefix = {arXiv}, -arxivId = {1409.6718}, -author = {Maio, Umberto and Viel, Matteo}, -doi = {10.1093/mnras/stu2304}, -eprint = {1409.6718}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Early Universe}, -number = {3}, -pages = {2760--2775}, -title = {{The first billion years of a warm dark matter universe}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.446.2760M%5Cnhttp://mnras.oxfordjournals.org/cgi/doi/10.1093/mnras/stu2304}, -volume = {446}, -year = {2015} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Distribution of Satellite Galaxies in a Lambda-CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2005} -} -@article{Yang2019a, -abstract = {We use the Illustris simulation to study the distributions of ellipticities and kinematic misalignments of galactic projections, as well as the intrinsic shapes and rotation of the simulated galaxies. Our results for the projections of galaxies display clear trends of an overall increase of kinematic misalignment and a slight decrease of ellipticity for fast rotators with increasing masses, while revealing no clear distinction between slow rotators of different mass. It is also found that the number of very slow rotators with large ellipticities is much larger than found in observations. The intrinsic properties of the galaxies are then analysed. The results for the intrinsic shapes of the galaxies are mostly consistent with previous results inferred from observational data. The distributions of intrinsic misalignment of the galaxies suggest that some of the galaxies produced by Illustris have significant rotation around their medium axes. Further analysis reveals that most of these galaxies display signs of non-equilibrium. We then study the evolution of the intrinsic misalignments and shapes of three specific Illustris galaxies, which we consider as typical ones, along the main progenitor line of their merger trees, revealing how mergers influence the intrinsic shapes and kinematics: the spin axis in general stays close to the shortest axis, and tends to quickly relax to such an equilibrium state within a few dynamical times of the galaxy after major perturbations; triaxiality and intrinsic flatness in general decrease with time, however, sometimes increases occur that are clearly seen to correlate with major merger events.}, -archivePrefix = {arXiv}, -arxivId = {1908.01102}, -author = {Yang, Lisiyuan and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hongyu}, -doi = {10.1093/mnras/stz2156}, -eprint = {1908.01102}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {evolution,fundamental,galaxies,kinematics and dynamics,parameters,photometry,stellar content,structure}, -number = {1}, -pages = {534--547}, -title = {{Photometric and kinematic misalignments and their evolution among fast and slow rotators in the illustris simulation}}, -volume = {489}, -year = {2019} -} -@article{Pontzen2014, -abstract = {A principal discovery in modern cosmology is that standard model particles comprise only 5 per cent of the mass-energy budget of the Universe. In the $\Lambda$CDM paradigm, the remaining 95 per cent consists of dark energy ($\Lambda$) and cold dark matter. $\Lambda$CDM is being challenged by its apparent inability to explain the low-density 'cores' of dark matter measured at the centre of galaxies, where centrally concentrated high-density 'cusps' were predicted. But before drawing conclusions, it is necessary to include the effect of gas and stars, historically seen as passive components of galaxies. We now understand that these can inject heat energy into the cold dark matter through a coupling based on rapid gravitational potential fluctuations, explaining the observed low central densities. {\textcopyright}2014 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1402.1764}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1038/nature12953}, -eprint = {1402.1764}, -isbn = {1476-4687 (Electronic){\$}\backslash{\$}r0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -number = {7487}, -pages = {171--178}, -pmid = {24522596}, -title = {{Cold dark matter heats up}}, -volume = {506}, -year = {2014} -} -@article{Weijmans2014, -abstract = {We use the ATLAS3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation $\sigma$q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and $\sigma$q = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrizations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P. T. and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F. and Davies, Roger L. and Davis, Timothy A. and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M.}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Weijmans et al. - 2014 - The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular, cD- galaxies,Galaxies,Structure}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Cappellari2013, -abstract = {In the companion Paper XV of this series, we derive accurate total mass-to-light ratios (M/L)JAM ≈ (M/L)(r = Re) within a sphere of radius r = Re centred on the galaxy, as well as stellar (M/L)stars (with the dark matter removed) for the volume-limited and nearly massselected (stellarmassM* ≲ 6 × 109M⊙)ATLAS3D sample of 260 early-type galaxies (ETGs, ellipticals Es and lenticulars S0s). Here, we use those parameters to study the two orthogonal projections (MJAM, $\sigma$e) and (MJAM,R maje ) of the thin Mass Plane (MP) (MJAM, $\sigma$e,Rmaje ) which describes the distribution of the galaxy population, where MJAM = L × (M/L)JAM ≈ M*. The distribution of galaxy properties on both projections of the MP is characterized by: (i) the same zone of exclusion (ZOE), which can be transformed from one projection to the other using the scalar virial equation. The ZOE is roughly described by two power laws, joined by a break at a characteristic mass MJAM ≈ 3 × 1010M⊙, which corresponds to the minimum Re and maximum stellar density. This results in a break in the meanMJAM-$\sigma$e relation with trends MJAM $\alpha$ $\sigma$2.3e and MJAM $\alpha$ $\sigma$4.7e at small and large $\sigma$e, respectively; (ii) a characteristic mass MJAM ≈ 2 × 1011M⊙ which separates a population dominated by flat fast rotator with discs and spiral galaxies at lower masses, from one dominated by quite round slow rotators at larger masses; (iii) below that mass the distribution of ETGs' properties on the two projections of the MP tends to be constant along lines of roughly constant se, or equivalently along lines with Rmaje $\alpha$ MJAM, respectively (or even better parallel to the ZOE: Rmaje $\alpha$ M0.75JAM); (iv) it forms a continuous and parallel sequence with the distribution of spiral galaxies; (v) at even lower masses, the distribution of fast-rotator ETGs and late spirals naturally extends to that of dwarf ETGs (Sph) and dwarf irregulars (Im), respectively. We use dynamical models to analyse our kinematic maps. We show that $\sigma$e traces the bulge fraction, which appears to be the main driver for the observed trends in the dynamical (M/L)JAM and in indicators of the (M/L)pop of the stellar population like H$\beta$ and colour, as well as in the molecular gas fraction. A similar variation along contours of $\sigma$e is also observed for the mass normalization of the stellar initial mass function (IMF), which was recently shown to vary systematically within the ETGs' population. Our preferred relation has the form log10[(M/L)stars/(M/L)Salp] = a + b × log10($\sigma$e/130 km s-1) with a=-0.12 ± 0.01 and b = 0.35 ± 0.06. Unless there are major flaws in all stellar population models, this trend implies a transition of the mean IMF from Kroupa to Salpeter in the interval log10($\sigma$e/km s-1) ≈ 1.9-2.5 (or $\sigma$e ≈ 90-290 km s-1), with a smooth variation in between, consistently with what was shown in Cappellari et al. The observed distribution of galaxy properties on the MP provides a clean and novel view for a number of previously reported trends, which constitute special two-dimensional projections of the more general four-dimensional parameters trends on the MP. We interpret it as due to a combination of two main effects: (i) an increase of the bulge fraction, which increases $\sigma$e, decreases Re, and greatly enhance the likelihood for a galaxy to have its star formation quenched, and (ii) dry merging, increasing galaxy mass and Re by moving galaxies along lines of roughly constant $\sigma$e (or steeper), while leaving the population nearly unchanged. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1208.3523}, -author = {Cappellari, Michele and McDermid, Richard M. and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Crocker, Alison F. and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Emsellem, Eric and Khochfar, Sadegh and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1093/mnras/stt644}, -eprint = {1208.3523}, -isbn = {0769518745}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -month = {jul}, -number = {3}, -pages = {1862--1893}, -title = {{The ATLAS3D project-XX. Mass-size and mass-$\sigma$ distributions of early-type galaxies: Bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function}}, -volume = {432}, -year = {2013} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified {\$\sim${}}17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M {\textless}10{\^{}}9 M*), low-metallicity (Z{\$\sim${}}1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He $\backslash$ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A and Erb, Dawn K and Auger, Matthew W and Pettini, Max and Brammer, Gabriel B}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {164}, -title = {{ A Window on the Earliest Star Formation: Extreme Photoionization Conditions of a High-ionization, Low-metallicity Lensed Galaxy at z ∼ 2* }}, -url = {http://arxiv.org/abs/1803.02340}, -volume = {859}, -year = {2018} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance $\Lambda$ cold dark matter cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for 'radio' feedback from those active galactic nuclei that lie at the centre of a quasi-static X-ray-emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models that might explain the accretion rate scalings required for our phenomenological 'radio mode' model to be successful. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J and Springel, Volker and White, Simon D M and {De Lucia}, G and Frenk, C S and Gao, L and Jenkins, A and Kauffmann, G and Navarro, J F and Yoshida, N}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, $\sigma$(R), for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude MK {\textless} -25.3mag, or stellar mass M* ≳ 4 × 1011M⊙, within 108 Mpc. Our wide-field 107 arcsec × 107 arcsec IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes $\gamma$ inner and $\gamma$ outer of s(R). While $\gamma$ inner is mostly negative, of the 56 galaxies with sufficient radial coverage to determine $\gamma$ outer we find 36 per cent to have rising outer dispersion profiles, 30 per cent to be flat within the uncertainties and 34 per cent to be falling. The fraction of galaxies with rising outer profiles increases with M* and in denser galaxy environment, with 10 of the 11 most massive galaxies in our sample having flat or rising dispersion profiles. The strongest environmental correlations are with local density and halo mass, but a weaker correlation with large-scale density also exists. The average $\gamma$ outer is similar for brightest group galaxies, satellites and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis h4. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the $\Lambda$CDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no significant detection of a stellar halo, as in the case of M101, NGC 3351 and NGC 1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies in the range M200 = 8 × 1011-2 × 1012 M⊙ with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction fSH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming, and assemble their dark matter halos earlier than galaxies with similar masses. They have also accreted more low-mass satellites at earlier infall times than centrals with high fSH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretiondominated r {\$\sim${}} 45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers at higher redshifts and evolved unperturbed in the last {\$\sim${}}10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M and Sales, Laura V and Creasey, Peter and Cooper, Michael C and Bullock, James S and {Michael Rich}, R and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Li2018a, -abstract = {We investigate the discrepancy between the two-dimensional projected lensing mass and the dynam- ical mass for an ensemble of 97 strong gravitational lensing systems discovered by the Sloan Lens ACS (SLACS) Survey, the BOSS Emission-Line Lens Survey (BELLS), and the BELLS for GALaxy-Ly{\{}$\backslash$alpha{\}} EmitteR sYs- tems (BELLS GALLERY) Survey. We fit the lensing data to obtain the Einstein mass, and use the velocity dispersion of the lensing galaxies provided by the Sloan Digital Sky Survey (SDSS) to get the projected dynamical mass within the Einstein radius by assuming the power-law mass approximation. The discrepancy is found to be obvious and quantified by Bayesian analysis. For the singular isothermal sphere (SIS) mass model, we obtain that the Einstein mass is 20.7{\%} more than the dynamical mass, and the discrepancy increases with the redshift of the lensing galaxies. For more general power-law mass model, the discrepancy still exists within 1{\{}$\backslash$sigma{\}} credible region. The main reason of the the discrepancy could be mass contamination, including all invisible masses along the line of sight. In addition, the measurement errors and the approximation of the mass models could lead to part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1803.00819}, -author = {Li, Rui and Wang, Jiancheng and Shu, Yiping and Xu, Zhaoyi}, -doi = {10.3847/1538-4357/aaab50}, -eprint = {1803.00819}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {64}, -title = {{The Discrepancy between Einstein Mass and Dynamical Mass for SIS and Power-law Mass Models}}, -url = {http://arxiv.org/abs/1803.00819%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaab50}, -volume = {855}, -year = {2018} -} -@article{Morganti2013, -abstract = {NGC 4494 is one of several intermediate-luminosity elliptical galaxies inferred to have an unusually diffuse dark matter halo. We use the $\chi$2-made-to-measure particle code nmagic to construct axisymmetric models of NGC 4494 from photometric and various kinematic data. The extended kinematics include light spectra in multiple slitlets out to 3.5Re, and hundreds of planetary nebula velocities out to ≃7Re, thus allowing us to probe the dark matter content and orbital structure in the halo. We use Monte Carlo simulations to estimate confidence boundaries for the halo parameters, given our data and modelling set-up. We find that the true potential of the dark matter halo is recovered within $\Delta$G (merit function) ≲ 26 ($\Delta$$\chi$2 ≲ 59) at the 70 per cent confidence level (CL), and within $\Delta$G ≲ 32 ($\Delta$$\chi$2 ≲ 70) at the 90 per cent CL. These numbers are much larger than the usually assumed $\Delta$$\chi$2 2.3 (4.6) for the 70 per cent (90 per cent) CL for two free parameters, perhaps case dependent, but calling into question the general validity of the standard assumptions used for halo and black hole mass determinations. The best-fitting models for NGC 4494 have a dark matter fraction of about 0.6 ± 0.1 at 5Re (70 per cent CL) and are embedded in a dark matter halo with circular velocity ∼200 km s-1. The total circular velocity curve (CVC) is approximately flat at vc 220 km s-1 outside ∼0.5Re. The orbital anisotropy of the stars is moderately radial. These results are independent of the assumed inclination of the galaxy, and edge-on models are preferred. Comparing with the haloes of NGC 3379 and NGC 4697, whose velocity dispersion profiles also decrease rapidly from the centre outwards, the outer CVCs and dark matter haloes are quite similar. NGC 4494 shows a particularly high dark matter fraction inside ∼ 3Re, and a strong concentration of baryons in the centre. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.2688}, -author = {Morganti, Lucia and Gerhard, Ortwin and Coccato, Lodovico and Martinez-valpuesta, Inma and Arnaboldi, Magda}, -doi = {10.1093/mnras/stt442}, -eprint = {1303.2688}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: individual: NGC 4494,Galaxies: kinematics and dynamics,Methods: numerical,cD}, -number = {4}, -pages = {3570--3588}, -title = {{Elliptical galaxies with rapidly decreasing velocity dispersion profiles: Nmagic models and dark halo parameter estimates for NGC 4494}}, -volume = {431}, -year = {2013} -} -@article{Brainerd2005, -abstract = {The distribution of satellite galaxies relative to isolated host galaxies in the Sloan Digital Sky Survey (SDSS) is investigated. Host-satellite systems are selected using three different methods, yielding samples of {\$\sim${}}3300, {\$\sim${}}1600, and {\$\sim${}}950 satellites. In the plane of the sky, the distributions of all three samples show highly significant deviations from circular symmetry ({\textgreater}99.99{\%}, {\textgreater}99.99{\%}, and 99.79{\%} confidence levels, respectively), and the degree of anisotropy is a strong function of the projected radius, r p , at which the satellites are found. For r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 100 kpc, the SDSS satellites are aligned preferentially with the major axes of the hosts. This is in stark contrast to the Holmberg effect, in which satellites are aligned with the minor axes of host galaxies. The degree of anisotropy in the distribution of the SDSS satellites decreases with r p and is consistent with an isotropic distribution at of order the 1 {\$}\sigma{\$}level for 250 kpc {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 500 kpc.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408559}, -author = {Brainerd, Tereasa G}, -doi = {10.1086/432713}, -eprint = {0408559}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L101--------L104}, -primaryClass = {astro-ph}, -title = {{Anisotropic Distribution of SDSS Satellite Galaxies: Planar (Not Polar) Alignment}}, -url = {http://stacks.iop.org/1538-4357/628/i=2/a=L101}, -volume = {628}, -year = {2005} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Dekel2006, -abstract = {We address the origin of the robust bimodality observed in galaxy properties about a characteristic stellar mass ∼3 × 1010 M⊙. Less massive galaxies tend to be ungrouped blue star forming discs, while more massive galaxies are typically grouped red old-star spheroids. Colour-magnitude data show a gap between the red and blue sequences, extremely red luminous galaxies already at z ∼ 1, a truncation of today's blue sequence above L*, and massive starbursts at z ∼ 2-4. We propose that these features are driven by the thermal properties of the inflowing gas and their interplay with the clustering and feedback processes, all functions of the dark matter halo mass and associated with a similar characteristic scale. In haloes below a critical shock-heating mass MShOCk ≲ 10 12 M⊙, discs are built by cold streams, not heated by a virial shock, yielding efficient early star formation. It is regulated by supernova feedback into a long sequence of bursts in blue galaxies constrained to a 'fundamental line'. Cold streams penetrating through hot media in M ≥ MShock haloes preferentially at z ≥ 2 lead to massive starbursts in L > L* galaxies. At z < 2, in M > Mshock haloes hosting groups, the gas is heated by a virial shock, and being dilute it becomes vulnerable to feedback from energetic sources such as active galactic nuclei. This shuts off gas supply and prevents further star formation, leading by passive evolution to 'red-and-dead' massive spheroids starting at z ∼ 1. A minimum in feedback efficiency near Mshock explains the observed minimum in M/L and the qualitative features of the star formation history. The cold flows provide a hint for solving the angular momentum problem. When these processes are incorporated in simulations they recover the main bimodality features and solve other open puzzles. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0412300}, -author = {Dekel, Avishai and Birnboim, Yuval}, -doi = {10.1111/j.1365-2966.2006.10145.x}, -eprint = {0412300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Dark matter,Galaxies: evolution,Galaxies: formation,Galaxies: haloes,Shock waves}, -month = {may}, -number = {1}, -pages = {2--20}, -pmid = {24653860}, -primaryClass = {astro-ph}, -title = {{Galaxy bimodality due to cold flows and shock heating}}, -volume = {368}, -year = {2006} -} -@article{MinkaT.2008, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture}, -author = {Zarocostas, John}, -doi = {10.1136/bmj.d706}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Zarocostas - 2011 - Gates and Cameron pledge new money to eradicate polio.pdf:pdf}, -issn = {14685833}, -journal = {BMJ (Clinical research ed.)}, -pages = {16}, -pmid = {21285225}, -title = {{Gates and Cameron pledge new money to eradicate polio.}}, -volume = {342}, -year = {2011} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M{\_}*/M{\_}sun) {\textgreater} 11.5 (M{\_}K {\textless} -25.3 mag) and distance D {\textless} 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38$\backslash$pm6{\%} down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80$\backslash$pm10{\%} and 28$\backslash$pm6{\%}, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R{\_}e), and the gas morphologies are diverse, with 17/28 = 61$\backslash$pm9{\%} being centrally concentrated, 8/28 = 29$\backslash$pm9{\%} exhibiting clear rotation out to several kpc, and 3/28 = 11$\backslash$pm6{\%} being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly {\$\sim${}}10{\^{}}5M{\_}sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A and Blakeslee, John P and Goulding, Andy D and McConnell, Nicholas J and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{Smith2017, -abstract = {We analyse the stellar kinematics of the z = 0.169 brightest cluster galaxy in Abell 1201, using integral field observations acquired with the Multi-Unit Spectroscopic Explorer on the Very Large Telescope. This galaxy has a gravitationally lensed arc located at unusually small radius ($\sim$5 kpc), allowing us to constrain the mass distribution using lensing and stellar dynamical information over the same radial range. We measure a velocity dispersion profile which is nearly flat at s ≈ 285 km s-1 in the inner $\sim$5 kpc, and then rises steadily to $\sigma$ ≈ 360 km s-1 at $\sim$30 kpc. We analyse the kinematics using axisymmetric Jeans models, finding that the data require both a significant dark matter halo (to fit the rising outer profile) and a compact central component, with mass Mcen ≈ 2.5 × 1010 M⊙ (to fit the flat s in the inner regions). The latter component could represent a supermassive black hole, in which case it would be among the largest known to date. Alternatively Mcen could describe excess mass associated with a gradient in the stellar mass-to-light ratio. Imposing a standard Navarro-Frenk-White (NFW) dark matter density profile, we recover a stellar mass-to-light ratio $\gamma$, which is consistent with a Milky Way-like initial mass function (IMF). By anchoring the models using the lensing mass constraint, we break the degeneracy between $\gamma$ and the inner slope $\gamma$ of the dark matter profile, finding $\gamma$ = 1.0 ± 0.1, consistent with the NFW form. We show that our results are quite sensitive to the treatment of the central mass in the models. Neglecting Mcen biases the results towards both a heavier-than-Salpeter IMF and a shallower-than-NFW dark matter slope ($\gamma$ ≈ 0.5).}, -archivePrefix = {arXiv}, -arxivId = {1706.07055}, -author = {Smith, Russell J. and Lucey, John R. and Edge, Alastair C.}, -doi = {10.1093/MNRAS/STX1573}, -eprint = {1706.07055}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Smith, Lucey, Edge - 2017 - Stellar dynamics in the strong-lensing central galaxy of Abell 1201 A low stellar mass-to-light ratio, a lar.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {CD- galaxies: kinematics and dynamics,Galaxies: clusters: individual: Abell 1201,Galaxies: elliptical and lenticular,Gravitational lensing: strong}, -number = {1}, -pages = {383--393}, -title = {{Stellar dynamics in the strong-lensing central galaxy of Abell 1201: A low stellar mass-to-light ratio, a large central compact mass and a standard dark matter halo}}, -url = {http://arxiv.org/abs/1706.07055%0Ahttp://dx.doi.org/10.1093/mnras/stx1573}, -volume = {471}, -year = {2017} -} -@article{Brooks2015a, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by a global driving force and a local positive feedback mechanism, which creates regular geometric and/or temporal patterns, and decreases the entropy locally, in contrast to random processes. Here we investigate for the first time a comprehensive number of (17) self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous “order out of randomness”, during the evolution from an initially disordered system to an ordered quasi-stationary system, mostly by quasi-periodic limit-cycle dynamics, but also by harmonic (mechanical or gyromagnetic) resonances. The global driving force can be due to gravity, electromagnetic forces, mechanical forces (e.g., rotation or differential rotation), thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational (Balbus-Hawley) instability, the convective (Rayleigh-B{\'{e}}nard) instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or a loss-cone instability. Physical models of astrophysical self-organization processes require hydrodynamic, magneto-hydrodynamic (MHD), plasma, or N-body simulations. Analytical formulations of self-organizing systems generally involve coupled differential equations with limit-cycle solutions of the Lotka-Volterra or Hopf-bifurcation type.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J. and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C.M. and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G. and Scargle, Jeffrey D. and Melatos, Andrew and Wagoner, Robert V. and Trimble, Virginia and Green, William H.}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Aschwanden et al. - 2018 - Order out of Randomness Self-Organization Processes in Astrophysics.pdf:pdf}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Handley2015, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W. J. and Hobson, M. P. and Lasenby, A. N.}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Handley, Hobson, Lasenby - 2015 - POLYCHORD Next-generation nested sampling(3).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Robertson2019, -abstract = {We present BAHAMAS-SIDM, the first large-volume, (400 h−1 Mpc)3, cosmological simulations including both self-interacting dark matter (SIDM) and baryonic physics. These simulations are important for two primary reasons: (1) they include the effects of baryons on the dark matter distribution and (2) the baryon particles can be used to make mock observables that can be compared directly with observations. As is well known, SIDM haloes are systematically less dense in their centres, and rounder, than CDM haloes. Here, we find that that these changes are not reflected in the distribution of gas or stars within galaxy clusters, or in their X-ray luminosities. However, gravitational lensing observables can discriminate between DM models, and we present a menu of tests that future surveys could use to measure the SIDM interaction strength. We ray-trace our simulated galaxy clusters to produce strong lensing maps. Including baryons boosts the lensing strength of clusters that produce no critical curves in SIDM-only simulations. Comparing the Einstein radii of our simulated clusters with those observed in the CLASH survey, we find that at velocities around 1000 km s−1 an SIDM cross-section of $\sigma$/m ≳ 1 cm2 g−1 is likely incompatible with observed cluster lensing.}, -archivePrefix = {arXiv}, -arxivId = {1810.05649}, -author = {Robertson, Andrew and Harvey, David and Massey, Richard and Eke, Vincent and McCarthy, Ian G. and Jauzac, Mathilde and Li, Baojiu and Schaye, Joop}, -doi = {10.1093/mnras/stz1815}, -eprint = {1810.05649}, -file = {:C\:/Users/Jammy/Documents/Papers/DarkMatterModels/Robertson2018SIDMsimulation.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Astroparticle physics,Cosmology: theory,Dark matter,Galaxies: clusters: general}, -number = {3}, -pages = {3646--3662}, -title = {{Observable tests of self-interacting dark matter in galaxy clusters: Cosmological simulations with SIDM and baryons}}, -volume = {488}, -year = {2019} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned {\$}r{\$} and {\$}g{\$} band images from a sample of 45508 galaxies from SDSS DR9 in the redshift range {\$}0.06\backslash,\backslashbackslashle\backslash,z\backslash,\backslashbackslashle\backslash,0.1{\$} and in the mass range {\$}10{\^{}}{\{}10.0{\}} M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}} {\textless}M{\_}{\{}*{\}} {\textless}10{\^{}}{\{}11.4{\}} M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$}r. We derive surface brightness profiles to a depth of almost {\$}\backslashbackslashmu{\{}\backslash{\_}{\}}r \backslashbackslashsim 32 \backslash,\backslashbackslashmathrm{\{}\backslash{\{}{\}}mag\backslashbackslash,arcsec{\{}\backslash{\}}{\}}{\^{}}{\{}-2{\}}{\$}. We find that the ellipticity of the stellar halo is a function of galaxy stellar mass and that the haloes of high concentration ({\$}C {\textgreater}2.6{\$}) galaxies are more elliptical than those of low concentration ({\$}C {\textless}2.6{\$}) galaxies. The {\$}g{\$}-{\$}r{\$} colour profile of high concentration galaxies reveals that the {\$}g{\$}-{\$}r{\$} colour of the stellar population in the stellar halo is bluer than in the main galaxy, and the colour of the stellar halo is redder for higher mass galaxies. We further demonstrate that the full two-dimensional surface intensity distribution of our galaxy stacks can only be fit through multi-component S{\$}\backslash{\$}'{\{}e{\}}rsic models. Using the fraction of light in the outer component of the models as a proxy for the fraction of accreted stellar light, we show that this fraction is a function of stellar mass and galaxy type. For high concentration galaxies, the fraction of accreted stellar light rises from {\$}30\backslashbackslash{\{}\backslash{\%}{\}}{\$} to {\$}70\backslashbackslash{\{}\backslash{\%}{\}}{\$} for galaxies in the stellar mass range from {\$}10{\^{}}{\{}10.0{\}} M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} to {\$}10{\^{}}{\{}11.4{\}} M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$}. The fraction of accreted light is much smaller in low concentration systems, increasing from {\$}2\backslashbackslash{\{}\backslash{\%}{\}}{\$} to {\$}25\backslashbackslash{\{}\backslash{\%}{\}}{\$} over the same mass range. This work provides important constraints for the theoretical understanding of the formation of stellar haloes of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1404.2123}, -author = {D'Souza, Richard and Kauffman, Guinevere and Wang, Jing and Vegetti, Simona}, -doi = {10.1093/mnras/stu1194}, -eprint = {1404.2123}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: halo,Galaxy: structure}, -number = {2}, -pages = {1433--1450}, -title = {{Parametrizing the stellar haloes of galaxies}}, -volume = {443}, -year = {2014} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Ding2018a, -abstract = {Strong gravitational lenses with measured time delay are a powerful tool to measure cosmological parameters, especially the Hubble constant ({\$}H{\_}0{\$}). Recent studies show by combining just three multiply-imaged AGN systems, one can determine {\$}H{\_}0{\$} to 3.8{\%} precision. Furthermore, the number of time-delay lens is growing rapidly, enabling the determination of {\$}H{\_}0{\$} to 1{\%} precision in the near future. However, it is important to ensure that systematic errors and biases remain subdominant. For this purpose, challenges with simulated datasets are a key component. Following the experience of the past challenge on time delay, where it was shown that time delays can be measured precisely and accurately at the sub-percent level, we now present the "Time Delay Lens Modeling Challenge" (TDLMC). The goal of TDLMC is to assess the present capabilities of lens modeling codes and assumptions and test the level of accuracy of inferred cosmological parameters given realistic mock datasets. We invite scientists to model a set of simulated HST observations of 50 mock lens systems. The systems are organized in rungs, with the complexity and realism increasing going up the ladder. The goal of the challenge is to infer {\$}H{\_}0{\$} for each rung, given the HST images, the time delay, and a stellar velocity dispersion of the deflector, for a fixed background cosmology. The TDLMC challenge will start with the mock data release on 2018 January 8th. The deadline for blind submission is different for each rung. The deadline for Rung0-1 is 2018 September 8; the deadline for Rung2 is 2019 January 8 and the one for Rung3 is 2019 May 8. This first paper gives an overview of the challenge including the data design, and a set of metrics to quantify the modeling performance and challenge details. After the deadline, the results of the challenge will be presented in a companion paper with all challenge participants as co-authors.}, -archivePrefix = {arXiv}, -arxivId = {1801.01506}, -author = {Ding, Xuheng and Treu, Tommaso and Shajib, Anowar J and Xu, Dandan and Chen, Geoff C -F. and More, Anupreeta and Despali, Giulia and Frigo, Matteo and Fassnacht, Christopher D and Gilman, Daniel and Hilbert, Stefan and Marshall, Philip J and Sluse, Dominique and Vegetti, Simona}, -eprint = {1801.01506}, -title = {{Time Delay Lens Modeling Challenge: I. Experimental Design}}, -url = {http://arxiv.org/abs/1801.01506}, -year = {2018} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ {\textgreater} 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright}2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{Leauthaud2017, -abstract = {We present high signal-to-noise galaxy-galaxy lensing measurements of the Baryon Oscillation Spectroscopic Survey constant mass (CMASS) sample using 250 deg2 of weak-lensing data from Canada-France-Hawaii Telescope Lensing Survey and Canada-France-Hawaii Telescope Stripe 82 Survey. We compare this signal with predictions from mock catalogues trained to match observables including the stellar mass function and the projected and twodimensional clustering of CMASS. We show that the clustering of CMASS, together with standard models of the galaxy-halo connection, robustly predicts a lensing signal that is 20-40 per cent larger than observed. Detailed tests show that our results are robust to a variety of systematic effects. Lowering the value of S8 = $\sigma$8 √ $\Omega$m/0.3 compared to Planck Collaboration XIII reconciles the lensing with clustering. However, given the scale of our measurement (r {\textless} 10 h-1 Mpc), other effects may also be at play and need to be taken into consideration. We explore the impact of baryon physics, assembly bias, massive neutrinos and modifications to general relativity on $\Delta$$\Sigma$ and show that several of these effects may be non-negligible given the precision of our measurement. Disentangling cosmological effects from the details of the galaxy-halo connection, the effect of baryons, and massive neutrinos, is the next challenge facing joint lensing and clustering analyses. This is especially true in the context of large galaxy samples from Baryon Acoustic Oscillation surveys with precise measurements but complex selection functions.}, -archivePrefix = {arXiv}, -arxivId = {1611.08606}, -author = {Leauthaud, Alexie and Saito, Shun and Hilbert, Stefan and Barreira, Alexandre and More, Surhud and White, Martin and Alam, Shadab and Behroozi, Peter and Bundy, Kevin and Coupon, Jean and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Mandelbaum, Rachel and Miller, Lance and Moraes, Bruno and Pereira, Maria E S and Rodr{\'{i}}guez-Torres, Sergio A and Schmidt, Fabian and Shan, Huan Yuan and Viel, Matteo and Villaescusa-Navarro, Francisco}, -doi = {10.1093/mnras/stx258}, -eprint = {1611.08606}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {3}, -pages = {3024--3047}, -title = {{Lensing is low: Cosmology, galaxy formation or new physics?}}, -volume = {467}, -year = {2017} -} -@article{Hsueh2016, -abstract = {Gravitational lens flux-ratio anomalies provide a powerful technique for measuring dark matter substructure in distant galaxies. However, before using these flux-ratio anomalies to test galaxy formation models, it is imperative to ascertain that the given anomalies are indeed due to the presence of dark matter substructure and not due to some other component of the lensing galaxy halo or to propagation effects. Here we present the case of CLASS B1555+375, which has a strong radio-wavelength flux-ratio anomaly. Our high-resolution near-infrared Keck II adaptive optics imaging and archival Hubble Space Telescope data reveal the lensing galaxy in this system to have a clear edge-on disc component that crosses directly over the pair of images that exhibit the flux-ratio anomaly. We find that simple models that include the disc can reproduce the cm-wavelength flux-ratio anomaly without requiring additional dark matter substructure. Although further studies are required, our results suggest the assumption that all flux-ratio anomalies are due to a population of dark matter sub-haloes may be incorrect, and analyses that do not account for the full complexity of the lens macro-model may overestimate the substructure mass fraction in massive lensing galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1601.01671}, -author = {Hsueh, J. W. and Fassnacht, C. D. and Vegetti, S. and McKean, J. P. and Spingola, C. and Auger, M. W. and Koopmans, L. V.E. and Lagattuta, D. J.}, -doi = {10.1093/mnrasl/slw146}, -eprint = {1601.01671}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hsueh et al. - 2016 - SHARP - II. Mass structure in strong lenses is not necessarily dark matter substructure A flux ratio anomaly from.pdf:pdf}, -issn = {17453933}, -journal = {MNRAS Letters}, -keywords = {Galaxies: structure,Quasars: individual: CLASS B1555+375}, -number = {1}, -pages = {L51--L55}, -title = {{SHARP - II. Mass structure in strong lenses is not necessarily dark matter substructure: A flux ratio anomaly from an edge-on disc in B1555+375}}, -volume = {463}, -year = {2016} -} -@article{Gomer2018, -abstract = {The positions of multiple images in galaxy lenses are related to the galaxy mass distribution. Smooth elliptical mass profiles were previously shown to be inadequate in reproducing the quad population. In this paper, we explore the deviations from such smooth elliptical mass distributions. Unlike most other work, we use a model-free approach based on the relative polar image angles of quads, and their position in 3D space with respect to the fundamental surface of quads (FSQ). The FSQ is defined by quads produced by elliptical lenses. We have generated thousands of quads from synthetic populations of lenses with substructure consistent with Lambda cold dark matter ($\Lambda$CDM) simulations, and found that such perturbations are not sufficient to match the observed distribution of quads relative to the FSQ. The result is unchanged even when subhalo masses are increased by a factor of 10, and the most optimistic lensing selection bias is applied. We then produce quads from galaxies created using two components, representing baryons and dark matter. The transition from the mass being dominated by baryons in inner radii to being dominated by dark matter in outer radii can carry with it asymmetries, which would affect relative image angles. We run preliminary experiments using lenses with two elliptical mass components with non-identical axial ratios and position angles, perturbations from ellipticity in the form of non-zero Fourier coefficients a4 and a6, and artificially offset ellipse centres as a proxy for asymmetry at image radii. We show that combination of these effects is a promising way of accounting for quad population properties. We conclude that the quad population provides a unique and sensitive tool for constraining detailed mass distribution in the centres of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1712.07665}, -author = {Gomer, Matthew R and Williams, Liliya L R}, -doi = {10.1093/mnras/stx3294}, -eprint = {1712.07665}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1987--2002}, -title = {{The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses}}, -volume = {475}, -year = {2018} -} -@article{Schombert2013, -abstract = {Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the S{\'{e}}rsic r 1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the S{\'{e}}rsic r 1/n model produces good fits to the core regions of ellipticals (r{\textless}r half), but is an inadequate function for the entire profile of an elliptical from core to halo due to competing effects on the S{\'{e}}rsic n index and the fact that the interior shape of an elliptical is only weakly correlated with its halo shape. In addition, there are a wide range of S{\'{e}}rsic parameters that will equally describe the shape of the outer profile, degrading the S{\'{e}}rsic model's usefulness as a describer of the entire profile. Empirically determined parameters, such as half-light radius and total luminosity, have less scatter than fitting function variables. The scaling relations for ellipticals are often non-linear, but for ellipticals brighter than MJ {\textless}-23 the following structural relations are found: L ∞ r 0.8±0.1, L ∞ $\Sigma$-0.5±0.1, and $\Sigma$ ∞ r -1.5±0.1. {\textcopyright}2013 Astronomical Society of Australia.}, -archivePrefix = {arXiv}, -arxivId = {1303.4710}, -author = {Schombert, J M}, -doi = {10.1017/pas.2013.010}, -eprint = {1303.4710}, -issn = {13233580}, -journal = {Publications of the Astronomical Society of Australia}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: star formation,galaxies: structure}, -number = {1}, -title = {{The structure of galaxies: II. Fitting functions and scaling relations for ellipticals}}, -url = {http://arxiv.org/abs/1303.4710%7B%5C%25%7D0Ahttp://dx.doi.org/10.1017/pas.2013.010}, -volume = {30}, -year = {2013} -} -@article{Sales2012, -abstract = {In the simplest scenario, disk galaxies form predominantly in halos with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly-rotating remnants of repeated merging events. We explore these assumptions using one hundred systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations GIMIC. At z=0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disk galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: disks form in halos with high and low net spin, and mergers play a negligible role in the formation of spheroid stars, most of which form in-situ. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly-accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Disks, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier-accreted material. Gas accretion from a hot corona thus favours disk formation, whereas gas that flows "cold", often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, most spheroids consist of superpositions of stellar components with distinct kinematics, age, and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology is imprinted early by the interplay of the tidal field and the shape of the material destined to form the galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {jun}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Minor2021, -abstract = {The presence of an invisible substructure has previously been detected in the gravitational lens galaxy SDSSJ0946+1006 through its perturbation of the lensed images. Using flexible models for the main halo and the subhalo perturbation, we demonstrate that the subhalo has an extraordinarily high central density and steep density slope. We robustly infer the subhalo's projected mass within 1 kpc to be ∼2-3.7 × 109 M⊙ at >95 per cent CL for all our lens models, while the average log-slope of the subhalo's projected density profile over the radial range 0.75-1.25 kpc is constrained to be steeper than isothermal ($\gamma$2D ≲ -1). By modeling the subhalo light, we infer a conservative upper bound on its luminosity LV < 1.2 × 108L⊙ at 95 per cent CL that shows that the perturber is dark matter dominated. We analyse lensing galaxy analogues in the Illustris TNG100-1 simulation over many lines of sight, and find hundreds of subhalos that achieve a mass within 1 kpc ≳ 2 × 109M⊙. However, less than 1 per cent of the mock observations yield a log-slope steep enough to be consistent with our lensing models, and they all have stellar masses exceeding that allowed by observations by an order of magnitude or more. We conclude that the presence of such a dark highly concentrated subhalo is unexpected in a Lambda cold dark matter universe. While it remains to be determined whether this tension can be reduced by adding more complexity to the primary lens model, it is not significantly alleviated if the perturber is assumed to be a LOS structure, rather than a subhalo.}, -archivePrefix = {arXiv}, -arxivId = {2011.10627}, -author = {Minor, Quinn and Gad-Nasr, Sophia and Kaplinghat, Manoj and Vegetti, Simona}, -doi = {10.1093/mnras/stab2247}, -eprint = {2011.10627}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Minor2020DMConcentration0946.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {dark matter,galaxies: dwarf,gravitational lensing: strong}, -number = {2}, -pages = {1662--1683}, -title = {{An unexpected high concentration for the dark substructure in the gravitational lens SDSSJ0946+1006}}, -volume = {507}, -year = {2021} -} -@article{Bullock:2005aa, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {dec}, -number = {2}, -pages = {931--949}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Daddi2005, -abstract = {1. publ.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503102}, -author = {Cloud, Preston E.}, -doi = {10.1126/science.144.3625.1428}, -eprint = {0503102}, -issn = {00368075}, -journal = {Science}, -keywords = {Cosmology: Observations,Galaxies: Evolution,Galaxies: Formation,Galaxies: High-Redshift}, -month = {jun}, -number = {3625}, -pages = {1428--1431}, -primaryClass = {astro-ph}, -title = {{Earth science today}}, -url = {http://stacks.iop.org/0004-637X/626/i=2/a=680}, -volume = {144}, -year = {1964} -} -@article{Geometryeq, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and $\backslash$nspectroscopic ESA cornerstone mission, currently scheduled for launch in$\backslash$nlate 2011. Its primary science drivers are the composition, formation$\backslash$nand evolution of the Galaxy. Gaia will not achieve its scientific$\backslash$nrequirements without detailed calibration and correction for radiation$\backslash$ndamage. Microscopic models of Gaia's CCDs are being developed to$\backslash$nsimulate the effect of radiation damage, charge trapping, which causes$\backslash$ncharge transfer inefficiency. The key to calculating the probability of$\backslash$na photoelectron being captured by a trap is the 3D electron density$\backslash$nwithin each CCD pixel. However, this has not been physically modelled$\backslash$nfor Gaia CCD pixels. In this paper, the first of a series, we motivate$\backslash$nthe need for such specialised 3D device modelling and outline how its$\backslash$nfuture results will fit into Gaia's overall radiation calibration$\backslash$nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -isbn = {9780819472311}, -issn = {0277-786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy III}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Hartigan1979, -abstract = {The K-means clustering algorithm is described indetail by Hartigan(1975). An efficient version of the algorithm is presented here.\nThe aim of the K-means algorithm is to divide M points in N dimensions into K clusters so that the within-cluster sum of squares is minimized. It is not practical to require that the solution has minimal sum of squares against all partitions except when M,N are small and K = 2. We seek instead "local" optima, solution such that no movement of a point from one cluster to another will reduce the within cluster sum of squares.}, -author = {Hartigan, J. A. and Wong, M. A.}, -doi = {10.2307/2346830}, -isbn = {00359254}, -issn = {00359254}, -journal = {Applied Statistics}, -keywords = {k-means clustering algorithm,transfer algorithm}, -number = {1}, -pages = {100}, -pmid = {8705250}, -title = {{Algorithm AS 136: A K-Means Clustering Algorithm}}, -url = {http://www.jstor.org/stable/10.2307/2346830?origin=crossref}, -volume = {28}, -year = {1979} -} -@article{Algorry2016, -abstract = {We examine the properties of barred disc galaxies in a $\Lambda$CDM cosmological hydrodynamical simulation from the EAGLE project. Our study follows the formation of 269 discs identified at z = 0 in the stellar mass range 10.6 {\textless} logM∗/M⊙ {\textless} 11. These discs show a wide range of bar strengths, from unbarred discs (≈60 per cent) to weak bars (≈20 per cent) and to strongly barred systems (≈20 per cent). Bars in these systems develop after redshift ≈1.3, on timescales that depend sensitively on the strength of the pattern. Strong bars develop relatively quickly (in a few Gyr, or roughly∼10 disc rotation periods) in systems that are disc dominated, gas poor, and have declining rotation curves.Weak bars develop more slowly in systems where the disc is less gravitationally important, and are still growing at z = 0. Unbarred galaxies are comparatively gas-rich discs whose rotation speeds do not exceed the maximum circular velocity of the haloes they inhabit. Bar lengths compare favourably with observations, ranging from 0.2 to 0.8 times the radius containing 90 per cent of the stars. Bars slow down remarkably quickly as they grow, causing the inner regions of the surrounding dark halo to expand. At z = 0 strong bars in simulated galaxies have corotation radii roughly 10 times the bar length. Such slow bars are inconsistent with the few cases where pattern speeds have been measured or inferred observationally, a discrepancy that, if confirmed, might prove a challenge for disc galaxy formation in $\Lambda$CDM.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1609.05909}, -author = {Algorry, David G and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Vecchia, Claudio Dalla and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx1008}, -eprint = {1609.05909}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Kinematics and dynamics,Galaxy: Disc,Galaxy: Formation,Galaxy: Structure}, -number = {1}, -pages = {1054--1064}, -title = {{Barred galaxies in the EAGLE cosmological hydrodynamical simulation}}, -url = {http://arxiv.org/abs/1609.05909%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1008}, -volume = {469}, -year = {2017} -} -@article{Stinson2013, -abstract = {We introduce the Making Galaxies In a Cosmological Context (MAGICC) programme of smoothed particle hydrodynamics simulations. We describe a parameter study of galaxy formation simulations of an L* galaxy that uses early stellar feedback combined with supernova feedback to match the stellar mass-halo mass relationship. While supernova feedback alone can reduce star formation enough to match the stellar mass-halo mass relationship, the galaxy forms too many stars before z = 2 to match the evolution seen using abundance matching. Our early stellar feedback is purely thermal and thus operates like an ultraviolet ionization source as well as providing some additional pressure from the radiation of massive, young stars. The early feedback heats gas to >106 K before cooling it to 104 K. The pressure from this hot gas creates a more extended disc and prevents more star formation prior to z = 1 than supernova feedback alone. The resulting disc galaxy has a flat rotation curve, an exponential surface brightness profile, and matches a wide range of disc scaling relationships. The disc forms from the inside-out with an increasing exponential scale length as the galaxy evolves. Overall, early stellar feedback helps to simulate galaxies that match observational results at low and high redshifts. {\textcopyright} 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1208.0002}, -author = {Stinson, G. S. and Brook, C. and Macci{\`{o}}, A. V. and Wadsley, J. and Quinn, T. R. and Couchman, H. M.P.}, -doi = {10.1093/mnras/sts028}, -eprint = {1208.0002}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Formation-galaxies,Hydrodynamics-galaxies,ISM}, -month = {jan}, -number = {1}, -pages = {129--140}, -title = {{Making galaxies in a cosmological context: The need for early stellar feedback}}, -volume = {428}, -year = {2013} -} -@article{Sanderson2009, -abstract = {We study the distribution of projected offsets between the cluster X-ray centroid and the brightest cluster galaxy (BCG) for 65 X-ray-selected clusters from the Local Cluster Substructure Survey, with a median redshift of z = 0.23. We find a clear correlation between X-ray/BCG projected offset and the logarithmic slope of the cluster gas density profile at 0.04r 500($\alpha$), implying that more dynamically disturbed clusters have weaker cool cores. Furthermore, there is a close correspondence between the activity of the BCG, in terms of detected H$\alpha$ and radio emission, and the X-ray/BCG offset, with the line-emitting galaxies all residing in clusters with X-ray/BCG offsets of ≤15 kpc. Of the BCGs with $\alpha$ {\textless} -0.85 and an offset {\textless}0.02r500, 96 per cent (23/24) have optical emission and 88 per cent (21/24) are radio active, while none has optical emission outside these criteria. We also study the cluster gas fraction (fgas) within r500 and find a significant correlation with X-ray/BCG projected offset. The mean fgas of the 'small offset' clusters ({\textless}0.02r 500) is 0.106 ± 0.005 ($\sigma$ = 0.03) compared to 0.145 ± 0.009 ($\sigma$ = 0.04) for those with an offset {\textgreater}0.02r 500, indicating that the total mass may be systematically underestimated in clusters with larger X-ray/BCG offsets. Our results imply a link between cool core strength and cluster dynamical state consistent with the view that cluster mergers can significantly perturb cool cores, and set new constraints on models of the evolution of the intracluster medium. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0906.1808}, -author = {Sanderson, Alastair J R and Edge, Alastair C and Smith, Graham P}, -doi = {10.1111/j.1365-2966.2009.15214.x}, -eprint = {0906.1808}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: Clusters: general,Galaxies: Elliptical and lenticular,Galaxies: Evolution,X-rays: Galaxies: Clusters,cD}, -number = {4}, -pages = {1698--1705}, -title = {{LoCuSS: The connection between brightest cluster galaxy activity, gas cooling and dynamical disturbance of X-ray cluster cores}}, -volume = {398}, -year = {2009} -} -@article{Yang2006, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Fergus2014, -abstract = {High dynamic-range imagers aim to block out or null light from a very bright primary star to make it possible to detect and measure far fainter companions; in real systems a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronograph. The model uses Principal Components Analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of order a percent of the brightness of the speckles, or up to {\$}10{\^{}}{\{}-7{\}}{\$} times the brightness of the primary star. This outperforms existing methods by a factor of 2-3 and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Schaller2015, -abstract = {We use the 'Evolution and assembly of galaxies and their environments' (EAGLE) cosmological simulation to investigate the effect of baryons on the density profiles of rich galaxy clusters. We focus on EAGLE clusters with M200 > 1014M⊙ of which we have six examples. The central brightest cluster galaxies (BCGs) in the simulation have steep stellar density profiles, $\rho$*(r)∝r-3. Stars dominate the mass density for r < 10 kpc, and, as a result, the total mass density profiles are steeper than the Navarro-Frenk-White (NFW) profile, in remarkable agreement with observations. The dark matter halo itself closely follows the NFW form at all resolved radii (r ≳ 3.0 kpc). The EAGLE BCGs have similar surface brightness and line-of-sight velocity dispersion profiles as the BCGs in the sample of Newman et al., which have the most detailed measurements currently available. After subtracting the contribution of the stars to the central density, Newman et al. infer significantly shallower slopes than the NFW value, in contradiction with the EAGLE results. We discuss possible reasons for this discrepancy, and conclude that an inconsistency between the kinematical model adopted by Newman et al. for their BCGs, which assumes isotropic stellar orbits, and the kinematical structure of the EAGLE BCGs, in which the orbital stellar anisotropy varies with radius and tends to be radially biased, could explain at least part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1409.8297}, -author = {Schaller, Matthieu and Frenk, Carlos S. and Bower, Richard G. and Theuns, Tom and Trayford, James and Crain, Robert A. and Furlong, Michelle and Schaye, Joop and Vecchia, Claudio Dalla and McCarthy, I. G.}, -doi = {10.1093/mnras/stv1341}, -eprint = {1409.8297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: clusters: general,Galaxies: haloes}, -number = {1}, -pages = {343--355}, -title = {{The effect of baryons on the inner density profiles of rich clusters}}, -url = {http://adsabs.harvard.edu/abs/2014arXiv1409.8297S}, -volume = {452}, -year = {2015} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -month = {aug}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -volume = {370}, -year = {2006} -} -@article{Kennedy2015, -abstract = {With a large sample of bright, low-redshift galaxies with optical-near-IR imaging from the GAMA survey we use bulge-disc decompositions to understand the wavelength-dependent behaviour of single-S{\'{e}}rsic structural measurements. We denote the variation in single-S{\'{e}}rsic index with wavelength as N{script}, likewise for effective radius we use ℛ. We find that most galaxies with a substantial disc, even those with no discernable bulge, display a high value of N{script}. The increase in S{\'{e}}rsic index to longer wavelengths is therefore intrinsic to discs, apparently resulting from radial variations in stellar population and/or dust reddening. Similarly, low values of ℛ (< 1) are found to be ubiquitous, implying an element of universality in galaxy colour gradients. We also study how bulge and disc colour distributions vary with galaxy type. We find that, rather than all bulges being red and all discs being blue in absolute terms, both components become redder for galaxies with redder total colours. We even observe that bulges in bluer galaxies are typically bluer than discs in red galaxies, and that bulges and discs are closer in colour for fainter galaxies. Trends in total colour are therefore not solely due to the colour or flux dominance of the bulge or disc.}, -archivePrefix = {arXiv}, -arxivId = {1605.04720}, -author = {Kennedy, Rebecca and Bamford, Steven P. and H{\"{a}}u{\ss}ler, Boris and Baldry, Ivan and Bremer, Malcolm and Brough, Sarah and Brown, Michael J.I. and Driver, Simon and Duncan, Kenneth and Graham, Alister W. and Holwerda, Benne W. and Hopkins, Andrew M. and Kelvin, Lee S. and Lange, Rebecca and Phillipps, Steven and Vika, Marina and Vulcani, Benedetta}, -doi = {10.1093/mnras/stw1176}, -eprint = {1605.04720}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxies: fundamental parameters,Galaxies: general,Galaxies: structure}, -month = {nov}, -number = {4}, -pages = {3458--3471}, -pmid = {8596459}, -title = {{Galaxy And Mass Assembly (GAMA): Understanding the wavelength dependence of galaxy structure with bulge-disc decompositions}}, -volume = {460}, -year = {2016} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies, in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the SDSS in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on the UV-optical colour {\$}NUV-r{\$}. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings that green valley galaxies have intermediate morphologies, moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of green valley galaxies, we find that they tend to be more massive in the field than in denser environments. On average, green valley galaxies account for {\$}\backslashbackslashsim 20\backslashbackslash{\{}\backslash{\%}{\}}{\$} of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming low mass galaxies. Green valley galaxies have average star formation histories intermediate between passive and star forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time, and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Kochanek2004a, -abstract = {A review of strong gravitational lensing and its astrophysical uses.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407232}, -author = {Kochanek, C. S.}, -eprint = {0407232}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kochanek - 2004 - The Saas Fee Lectures on Strong Gravitational Lensing.pdf:pdf}, -journal = {Saas-Fee Advanced Course 33: Gravitational Lensing: Strong, Weak and Micro}, -pages = {1--183}, -primaryClass = {astro-ph}, -title = {{The Saas Fee Lectures on Strong Gravitational Lensing}}, -url = {http://arxiv.org/abs/astro-ph/0407232}, -volume = {arXiv:astr}, -year = {2004} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past {\$\sim${}}12 Gyr. We model this process using a hybrid semianalytic plus N-body approach that distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our accreted stellar halos have density profiles that typically drop off with radius faster than the dark matter and follow power laws at r{\textgreater}{\$\sim${}}30 kpc with {\$}\rho{\$}{\$\sim${}}r-{\$}\alpha{\$}, {\$}\alpha{\$}{\$\sim${}}=3-4. They are well fit by Hernquist profiles over the full radial range. We find that stellar halos are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the {\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase-space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print){\$}\backslash{\$}r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://stacks.iop.org/0004-637X/635/i=2/a=931}, -volume = {635}, -year = {2005} -} -@article{Gebhardt2000, -abstract = {We describe a correlation between the mass M_BH of a galaxy's central black hole and the luminosity-weighted line-of-sight velocity dispersion sigma_e within the half-light radius. The result is based on a sample of 26 galaxies, including 13 galaxies with new determinations of black hole masses from Hubble Space Telescope measurements of stellar kinematics. The best-fit correlation is M_BH = 1.2 (+-0.2) x 10^8 M_sun (sigma_e/200 km/s)^(3.75 (+-0.3))over almost three orders of magnitude in M_BH; the scatter in M_BH at fixed sigma_e is only 0.30 dex and most of this is due to observational errors. The M_BH-sigma_e relation is of interest not only for its strong predictive power but also because it implies that central black hole mass is constrained by and closely related to properties of the host galaxy's bulge.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0006289}, -author = {Gebhardt, Karl and Bender, Ralf and Bower, Gary and Dressler, Alan and Faber, S. M. and Filippenko, Alexei V. and Green, Richard and Grillmair, Carl and Ho, Luis C. and Kormendy, John and Lauer, Tod R. and Magorrian, John and Pinkney, Jason and Richstone, Douglas and Tremaine, Scott}, -doi = {10.1086/312840}, -eprint = {0006289}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Gebhardt2000SMBHVelDisp.pdf:pdf}, -issn = {0004637X}, -journal = {ApJ}, -number = {1}, -pages = {L13--L16}, -primaryClass = {astro-ph}, -title = {{A Relationship between Nuclear Black Hole Mass and Galaxy Velocity Dispersion}}, -volume = {539}, -year = {2000} -} -@article{Aguero2016, -abstract = {We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75{\%} of the hosts), with a bar (44{\%} weak, 37{\%} strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem not to be important for the appearance of CNRs, which appear to be more related to intrinsic properties of the host galaxies or to minor merger processes; 2) the proportion of weak bars in galaxies with a CNR is higher than expected; 3) the incidence of Seyfert (Sy) activity coeval with CNRs is significantly larger than the rate expected from the morphological distribution of the host galaxies; 4) the rate of Sy 2 to Sy 1 type galaxies with CNRs is about three times larger than the expected ratio for galaxies without CNRs and is opposite to that predicted by the geometric paradigm of the classical unified model for AGNs, although it does support the hypothesis that Sy 2 activity is linked to circumnuclear star formation. The possible selection effects of the sample are discussed, and we conclude that the detected trends are strong enough to justify high quality observations of as large as possible set of galaxies with circumnuclear rings and their matched control samples.}, -author = {Ag{\"{u}}ero, Mar{\'{i}}a P and D{\'{i}}az, Rub{\'{e}}n J and Dottori, Horacio}, -doi = {10.4236/ijaa.2016.63018}, -issn = {2161-4717}, -journal = {International Journal of Astronomy and Astrophysics}, -keywords = {active,dynamics,galaxies,nuclei,spiral,structure}, -number = {03}, -pages = {219--235}, -title = {{Nuclear Activity in Circumnuclear Ring Galaxies}}, -url = {http://www.scirp.org/journal/doi.aspx?DOI=10.4236/ijaa.2016.63018}, -volume = {06}, -year = {2016} -} -@article{Morishita2018a, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {evolution,formation,galaxies,star formation}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Lilly2016, -abstract = {There are very strong observed correlations between the specific star-formation rates (sSFR) of galaxies and their mean surface mass densities, {\{}$\backslash$Sigma{\}}, as well as other aspects of their internal structure. These strong correlations have often been taken to indicate that the internal structure of a galaxy must play a major physical role, directly or indirectly, in the control of star-formation. In this paper we show by means of a very simple toy model that these correlations can arise naturally without any such physical role once the observed evolution of the size-mass relation for star-forming galaxies is taken into account. In particular, the model reproduces the sharp threshold in {\{}$\backslash$Sigma{\}} between galaxies that are star-forming and those that are quenched, and the evolution of this threshold with redshift. Similarly, it produces iso-quenched-fraction contours in the {\$}{\{}f{\_}Q(m,R{\_}e){\}}{\$} plane that are almost exactly parallel to lines of constant {\{}$\backslash$Sigma{\}} for centrals and shallower for satellites. It does so without any dependence on quenching on size or {\{}$\backslash$Sigma{\}}, and without invoking any differences between centrals and satellites, beyond the different mass-dependences of their quenching laws. The toy-model also reproduces several other observations, including the sSFR gradients within galaxies and the appearance of inside-out build-up of passive galaxies. Finally, it is shown that curvature in the Main Sequence sSFR-mass relation can produce curvature in the apparent B/T ratios with mass. Our analysis therefore suggests that many of the strong correlations that are observed between galaxy structure and sSFR may well be a consequence of things unrelated to quenching and should not be taken as evidence of the physical processes that drive quenching.}, -archivePrefix = {arXiv}, -arxivId = {1604.06459}, -author = {Lilly, Simon J and Carollo, C Marcella}, -doi = {10.3847/0004-637x/833/1/1}, -eprint = {1604.06459}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {1}, -pmid = {15540530}, -title = {{Surface Density Effects in Quenching: Cause or Effect?}}, -url = {http://arxiv.org/abs/1604.06459%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/833/1/1}, -volume = {833}, -year = {2016} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287----a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{2001ey, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M * = 1010.2 to 1012.0 M . We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority (≳75{\%}) of elliptical galaxies is not well described by a single S{\'{e}}rsic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (Re ∼ 1 kpc) inner component with luminosity fraction f 0.1-0.15; an intermediate-scale (Re 2.5 kpc) middle component with f 0.2-0.25; and a dominant (f = 0.6), extended (Re 10 kpc) outer envelope. All subcomponents have average S{\'{e}}rsic indices n 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies. {\textcopyright}2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C and Peng, Chien Y and Li, Zhao Yu and Barth, Aaron J}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{DeNicola2019, -abstract = {We study the correlations between Supermassive Black Holes (BH) and their host galaxies, using a sample of 83 BH masses collected from the most recent and reliable spatially resolved estimates available from the literature. We confirm the mono- and bivariate correlations between SMBHs and the bulges of their host galaxies, confirming that the correlation with the effective velocity dispersion is not significantly improved by higher dimensionality. Instead, pseudobulges do not seem to correlate with their SMBHs, probably because their secular evolution is often unable to trigger accretion onto the central BH. We then present a novel approach aimed at finding the fundamental relation between SMBHs and their host galaxies. For the first time, we analytically combine BH masses with the Fundamental Plane (FP), showing that MBH-$\sigma$e appears to be the fundamental relation rather than a putative “BH Fundamental Plane” of the kind MBH-$\sigma$e-Re. These results can be explained by a picture which sees the MBH$\sigma$e relation as a natural outcome of the change in AGN feedback from momentum- to energy-driven. The other scaling relations are then established through the FP.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0006053}, -author = {de Nicola, Stefano and Marconi, Alessandro and Longo, Giuseppe}, -doi = {10.1086/312838}, -eprint = {0006053}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Ferrarese2000VeloDisp.pdf:pdf}, -issn = {23318422}, -journal = {arXiv}, -keywords = {Galaxies: fundamental parameters,Galaxies: supermassive black holes}, -pages = {1995--1998}, -primaryClass = {astro-ph}, -title = {{The Fundamental Relation between Supermassive Black Holes and Their Host Galaxies}}, -year = {2019} -} -@article{Shi2015, -abstract = {We study how halo intrinsic dynamical properties are linked to their formation processes for halos in two mass ranges, 1012-1012.5 h-1M⊙ and ≥1013 h-1M⊙, and how both are correlated with the large-scale tidal field within which the halos reside at present. We identify infall halos that are about to merge with their hosts. We find that the tangential infall velocity increases significantly with the strength of the tidal field, but no strong correlation is found for the radial component. These results can be used to explain the environmental dependence of internal velocity anisotropy and spin of halos. The position vectors and velocities of infall halos are aligned with the principal axes of the tidal field, and the alignment depends on the strength of the tidal field. Opposite accretion patterns are found in weak and strong tidal fields, showing that in a weak field the accretion flow is dominated by radial motion within the local structure, while a large tangential component is present in a strong field. These findings can be used to understand the strong alignments we find between the principal axes of the internal velocity ellipsoids of halos and the tidal field, and their dependence on the strength of the tidal field. We further find that only in weak tidal fields does the spin-tidal field alignment follow the prediction of the tidal torque theory. We discuss how our results may be used to understand the spins of disk galaxies and velocity structures of elliptical galaxies and their correlations with large-scale structure.}, -archivePrefix = {arXiv}, -arxivId = {1501.07764}, -author = {Shi, Jingjing and Wang, Huiyuan and Mo, H. J.}, -doi = {10.1088/0004-637X/807/1/37}, -eprint = {1501.07764}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shi, Wang, Mo - 2015 - Flow Patterns Around Dark Matter Halos the Link Between Halo Dynamical Properties and Large-Scale Tidal Field(2).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: halos,large-scale structure of universe,methods: statistical}, -number = {1}, -title = {{Flow Patterns Around Dark Matter Halos: the Link Between Halo Dynamical Properties and Large-Scale Tidal Field}}, -volume = {807}, -year = {2015} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and discs are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disc components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to Calar Alto Integral Field Area integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux, they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P. and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tabor et al. - 2017 - Untangling galaxy components Full spectral bulge-disc decomposition.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Dynamics,Galaxies: elliptical and lenticular,Galaxies: kinematics}, -number = {2}, -pages = {2024--2033}, -title = {{Untangling galaxy components: Full spectral bulge-disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {466}, -year = {2017} -} -@article{Bonaca2019, -abstract = {We present a model for the interaction of the GD-1 stellar stream with a massive perturber that naturally explains many of the observed stream features, including a gap and an off-stream spur of stars. The model involves an impulse by a fast encounter, after which the stream grows a loop of stars at different orbital energies. At specific viewing angles, this loop appears offset from the stream track. A quantitative comparison of the spur and gap features prefers models where the perturber is in the mass range of $10^6\,\rm M_\odot$ to $10^8\,\rm M_\odot$. Orbit integrations back in time show that the stream encounter could not have been caused by any known globular cluster or dwarf galaxy with a determined orbit, and mass, size and impact-parameter arguments show that it could not have been caused by a molecular cloud in the Milky Way disk. The most plausible explanation for the gap-and-spur structure is an encounter with a dark-matter substructure, like those predicted to populate galactic halos in LCDM cosmology. However, the expected densities of LCDM subhalos in this mass range and in this part of the Milky Way are $2-3\,\sigma$ lower than the inferred density of the GD-1 perturber. This observation opens up the possibility that detailed observations of streams could measure the mass spectrum of dark-matter substructures and even identify individual substructures and their orbits in the Galactic halo.}, -archivePrefix = {arXiv}, -arxivId = {1811.03631}, -author = {Bonaca, Ana and Hogg, David W. and Price-Whelan, Adrian M. and Conroy, Charlie}, -doi = {10.3847/1538-4357/ab2873}, -eprint = {1811.03631}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bonaca et al. - 2019 - The Spur and the Gap in GD-1 Dynamical Evidence for a Dark Substructure in the Milky Way Halo.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cosmology,dark matter,galaxy,gravitation,halo,kinematics and dynamics,observations,stars}, -number = {1}, -pages = {38}, -title = {{The Spur and the Gap in GD-1: Dynamical Evidence for a Dark Substructure in the Milky Way Halo}}, -volume = {880}, -year = {2019} -} -@article{VanDeVyvere2022b, -abstract = {Massive elliptical galaxies can display structures that deviate from a pure elliptical shape, such as a twist of the principal axis or variations in the axis ratio with galactocentric distance. Although satisfactory lens modeling is generally achieved without accounting for these azimuthal structures, the question about their impact on inferred lens parameters remains, in particular, on time delays as they are used in time-delay cosmography. This paper aims at characterizing these effects and quantifying their impact considering realistic amplitudes of the variations. We achieved this goal by creating mock lensing galaxies with morphologies based on two data sets: observational data of local elliptical galaxies, and hydrodynamical simulations of elliptical galaxies at a typical lens redshift. We then simulated images of the lensing systems with space-based data quality and modeled them in a standard way to assess the impact of a lack of azimuthal freedom in the lens model. We find that twists in lensing galaxies are easily absorbed in homoeidal lens models by a change in orientation of the lens up to 10 • with respect to the reference orientation at the Einstein radius, and of the shear by up to 20 • with respect to the input shear orientation. The ellipticity gradients, on the other hand, can introduce a substantial amount of shear that may impact the radial mass model and consequently bias H 0 , up to 10 km s −1 Mpc −1. However, we find that light is a good tracer of azimuthal structures, meaning that direct imaging should be capable of diagnosing their presence. This in turn implies that such a large bias is unlikely to be unaccounted for in standard modeling practices. Furthermore, the overall impact of twists and ellipticity gradients averages out at a population level. For the galaxy populations we considered, the cosmological inference remains unbiased.}, -archivePrefix = {arXiv}, -arxivId = {2206.00022v1}, -author = {{Van De Vyvere}, Lyne and Sluse, Dominique and Gomer, Matthew R and Mukherjee, Sampath}, -eprint = {2206.00022v1}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/vandevyree2022Azimuthal.pdf:pdf}, -journal = {A\&A}, -keywords = {19c B-4000 Li{\`{e}}ge,Belgium Received DD-MM-YYYY,Cosmological parameters,Galaxies: elliptical and lenticular,Methods: numerical,Quartier Agora-All{\'{e}}e du six Ao{\^{u}}t,STAR Institute,accepted DD-MM-YYYY Key words Gravitational lensin,cD}, -pages = {1--19}, -title = {{Consequences of the lack of azimuthal freedom in the modeling of lensing galaxies}}, -url = {https://github.com/sibirrer/lenstronomy}, -volume = {179}, -year = {2022} -} -@article{Trujillo2006, -abstract = {We present the evolution of the luminosity-size and stellar mass-size relations of luminous (L V ≳ 3.4 × 10 10 h 70 -2 L⊙) and massive (M* ≳ 3 × 10 10 h 70 -2 M⊙) galaxies in the last ∼11 Gyr. We use very deep near-infrared images of the Hubble Deep Field-South and the MS 1054-03 field in the J s , H, and K s bands from FIRES to retrieve the sizes in the optical rest frame for galaxies with z > 1. We combine our results with those from GEMS at 0.2 < z > 1 and SDSS at z ∼ 0.1 to achieve a comprehensive picture of the optical rest-frame size evolution from z = 0 to 3. Galaxies are differentiated according to their light concentration using the S{\'{e}}rsic index n. For less concentrated objects, the galaxies at a given luminosity were typically ∼3 ± 0.5 (±2 $\sigma$) times smaller at z ∼ 2.5 than those we see today. The stellar mass-size relation has evolved less: the mean size at a given stellar mass was ∼2 ± 0.5 times smaller at z ∼ 2.5, evolving proportionally to (1 + Z) -0.40±0.06 . Simple scaling relations between dark matter halos and baryons in a hierarchical cosmogony predict a stronger (although consistent within the error bars) than observed evolution of the stellar mass-size relation. The observed luminosity-size evolution out to z ∼ 2.5 matches well recent infall model predictions for Milky Way-type objects. For low-n galaxies, the evolution of the stellar mass-size relation would follow naturally if the individual galaxies grow inside out. For highly concentrated objects, the situation is as follows: at a given luminosity, these galaxies were ∼2.7 ± 1.1 times smaller at z ∼ 2.5 (or, put differently, were typically ∼2.2 ± 0.7 mag brighter at a given size than they are today), and at a given stellar mass the size has evolved proportionally to (1 + z) -0.45±0.10 . {\textcopyright} 2006. The American Astronomical Society. Ail rights reserved.}, -author = {Trujillo, Ignacio and {Forster Schreiber}, Natascha M. and Rudnick, Gregory and Barden, Marco and Franx, Marijn and Rix, Hans‐Walter and Caldwell, J. A. R. and McIntosh, Daniel H. and Toft, Sune and Haussler, Boris and Zirm, Andrew and van Dokkum, Pieter G. and Labbe, Ivo and Moorwood, Alan and Rottgering, Huub and van der Wel, Arjen and van der Werf, Paul and van Starkenburg, Lottie}, -doi = {10.1086/506464}, -issn = {0004-637X}, -journal = {ApJ}, -month = {oct}, -number = {1}, -pages = {18--41}, -title = {{The Size Evolution of Galaxies since z ∼3: Combining SDSS, GEMS, and FIRES}}, -url = {http://stacks.iop.org/0004-637X/650/i=1/a=18}, -volume = {650}, -year = {2006} -} -@article{Yan2016a, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R{\$\sim${}}2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is {\$\sim${}}73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R and Bershady, Matthew A and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R and Thomas, Daniel and Wake, David A and Weijmans, Anne-Marie and Westfall, Kyle B and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A and Blanton, Michael R and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T and Goddard, Daniel and Gunn, James E and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R and Oravetz, Daniel and Pan, Kaike and Parejko, John K and Sanchez, Sebastian F and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {6}, -pages = {197}, -title = {{SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY}}, -url = {http://arxiv.org/abs/1607.08613%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {152}, -year = {2016} -} -@article{Suyu2006, -abstract = {Strong gravitational lens systems with extended sources are of special interest because they provide additional constraints on the models of the lens systems. To use a gravitational lens system for measuring the Hubble constant, one would need to determine the lens potential and the source intensity distribution simultaneously. A linear inversion method to reconstruct a pixellated source brightness distribution of a given lens potential model was introduced by Warren & Dye. In the inversion process, regularization on the source intensity is often needed to ensure a successful inversion with a faithful resulting source. In this paper, we use Bayesian analysis to determine the optimal regularization constant (strength of regularization) of a given form of regularization and to objectively choose the optimal form of regularization given a selection of regularizations. We consider and compare quantitatively three different forms of regularization previously described in the literature for source inversions in gravitational lensing: zeroth-order, gradient and curvature. We use simulated data with the exact lens potential to demonstrate the method. We find that the preferred form of regularization depends on the nature of the source distribution. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601493}, -author = {Suyu, S. H. and Marshall, P. J. and Hobson, M. P. and Blandford, R. D.}, -doi = {10.1111/j.1365-2966.2006.10733.x}, -eprint = {0601493}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Gravitational lensing,Methods: data analysis}, -month = {sep}, -number = {2}, -pages = {983--998}, -primaryClass = {astro-ph}, -title = {{A Bayesian analysis of regularized source inversions in gravitational lensing}}, -volume = {371}, -year = {2006} -} -@article{Morganti2013, -abstract = {NGC 4494 is one of several intermediate-luminosity elliptical galaxies inferred to have an unusually diffuse dark matter halo. We use the $\chi$2-made-to-measure particle code nmagic to construct axisymmetric models of NGC 4494 from photometric and various kinematic data. The extended kinematics include light spectra in multiple slitlets out to 3.5Re, and hundreds of planetary nebula velocities out to ≃7Re, thus allowing us to probe the dark matter content and orbital structure in the halo. We use Monte Carlo simulations to estimate confidence boundaries for the halo parameters, given our data and modelling set-up. We find that the true potential of the dark matter halo is recovered within $\Delta$G (merit function) ≲ 26 ($\Delta$$\chi$2 ≲ 59) at the 70 per cent confidence level (CL), and within $\Delta$G ≲ 32 ($\Delta$$\chi$2 ≲ 70) at the 90 per cent CL. These numbers are much larger than the usually assumed $\Delta$$\chi$2  2.3 (4.6) for the 70 per cent (90 per cent) CL for two free parameters, perhaps case dependent, but calling into question the general validity of the standard assumptions used for halo and black hole mass determinations. The best-fitting models for NGC 4494 have a dark matter fraction of about 0.6 ± 0.1 at 5Re (70 per cent CL) and are embedded in a dark matter halo with circular velocity ∼200 km s-1. The total circular velocity curve (CVC) is approximately flat at vc  220 km s-1 outside ∼0.5Re. The orbital anisotropy of the stars is moderately radial. These results are independent of the assumed inclination of the galaxy, and edge-on models are preferred. Comparing with the haloes of NGC 3379 and NGC 4697, whose velocity dispersion profiles also decrease rapidly from the centre outwards, the outer CVCs and dark matter haloes are quite similar. NGC 4494 shows a particularly high dark matter fraction inside ∼ 3Re, and a strong concentration of baryons in the centre. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.2688}, -author = {Morganti, Lucia and Gerhard, Ortwin and Coccato, Lodovico and Martinez-valpuesta, Inma and Arnaboldi, Magda}, -doi = {10.1093/mnras/stt442}, -eprint = {1303.2688}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Morganti et al. - 2013 - Elliptical galaxies with rapidly decreasing velocity dispersion profiles Nmagic models and dark halo paramet(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular, cD,Galaxies: haloes,Galaxies: individual: NGC 4494,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3570--3588}, -title = {{Elliptical galaxies with rapidly decreasing velocity dispersion profiles: Nmagic models and dark halo parameter estimates for NGC 4494}}, -volume = {431}, -year = {2013} -} -@article{Amvrosiadis2024, -abstract = {The surface brightness distribution of massive early-type galaxies (ETGs) often deviates from a perfectly elliptical shape. To capture these deviations in their isophotes during an ellipse fitting analysis, Fourier modes of order $m = 3, 4$ are often used. In such analyses the centre of each ellipse is treated as a free parameter, which may result in offsets from the centre of light, particularly for ellipses in the outer regions. This complexity is not currently accounted for in the mass models used in either strong gravitational lensing or galactic dynamical studies. In this work, we adopt a different approach, using the $m=1$ Fourier mode to account for this complexity while keeping the centres of all perturbed ellipses fixed, showing that it fits the data equally well. We applied our method to the distribution of light emission to a sample of ETGs from the MASSIVE survey and found that the majority have low $m_1$ amplitudes, below 2 percent. Five out of the 30 galaxies we analysed have high $m_1$ amplitudes, ranging from 2 to 10 percent in the outer parts ($R \gtrsim 3$ kpc), all of which have a physically associated companion. Based on our findings, we advocate the use of the $m=1$ multipole in the mass models used in strong lensing and dynamical studies, particularly for galaxies with recent or ongoing interactions.}, -archivePrefix = {arXiv}, -arxivId = {2407.12983}, -author = {Amvrosiadis, Aristeidis and Nightingale, James W. and He, Qiuhan and Robertson, Andrew and Lange, Samuel C. and Frenk, Carlos S. and Cole, Shaun and Massey, Richard and Poci, Adriano}, -eprint = {2407.12983}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Amvrosiadis2025M1Multipole.pdf:pdf}, -keywords = {elliptical and lenticular,galaxies,gravitational lensing,strong,structure}, -number = {July}, -pages = {1--7}, -title = {{Lopsidedness in Early-Type Galaxies: the role of the $m=1$ multipole in Isophote Fitting and Strong Lens Modelling}}, -volume = {000}, -year = {2024} -} -@article{Oldham2018, -abstract = {We present models for the dark and luminous mass structure of 12 strong lensing early-typegalaxies. We combine pixel-based modelling of multiband Hubble Space Telescope imagingwith Jeans modelling of kinematics obtained from Keck/ESI spectra to disentangle the darkand luminous contributions to the mass. Assuming a generalised NFW (gNFW) profile for thedark matter halo and a spatially constant stellar-mass-to-light ratio $\gamma$ * for the baryonic mass, we infer distributions for $\gamma$* consistent with initial mass functions (IMFs) that are heavierthan the Milky Way's (with a global mean mismatch parameter relative to a Chabrier IMF$\mu$ac = 1.80 ± 0.14) and halo inner density slopes that span a large range but are generallycuspier than the dark-matter-only prediction ($\mu$? = 2.01+0.19-0.22).We investigate possible reasonsfor overestimating the halo slope, including the neglect of spatially varying stellar-mass-tolightratios and/or stellar orbital anisotropy, and find that a quarter of the systems prefer radiallydeclining stellar-mass-to-light ratio gradients, but that the overall effect on our inference onthe halo slope is small. We suggest a coherent explanation of these results in the context ofinside-out galaxy growth, and that the relative importance of different baryonic processes inshaping the dark halo may depend on halo environment.}, -archivePrefix = {arXiv}, -arxivId = {1801.01887}, -author = {Oldham, Lindsay J. and Auger, Matthew W.}, -doi = {10.1093/mnras/sty065}, -eprint = {1801.01887}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Oldham2018StellarAndDark.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {1}, -pages = {133--150}, -title = {{Dark matter contraction and stellar-mass-to-light ratio gradients in massive early-type galaxies}}, -volume = {476}, -year = {2018} -} -@article{Toomre1972, -abstract = {Abstract image available at: http://adsabs.harvard.edu/abs/1972ApJ...178..623T}, -author = {Toomre, Alar and Toomre, Juri}, -doi = {10.1086/151823}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {dec}, -pages = {623}, -pmid = {14680119}, -title = {{Galactic Bridges and Tails}}, -url = {http://adsabs.harvard.edu/doi/10.1086/151823}, -volume = {178}, -year = {2002} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ($M_{*}>10^{10} M_{\odot}$), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at $z\sim2$. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that $39.2^{+3.9}_{-3.6}$\% (65/166) of cSFGs at $1.460°), nonvariable, unidentified sources contained in this catalog, only one or two are compatible with the spectrum of a dark matter particle heavier than approximately 50-100 GeV. The majority of these nine sources, however, feature a spectrum that is compatible with that predicted from a lighter (∼5-40GeV) dark matter particle. This population is consistent with the number of observable subhalos predicted for a dark matter candidate in this mass range and with an annihilation cross section of a simple thermal relic ($\sigma$v∼3×10 -26cm3/s). Observations in the direction of these sources at other wavelengths will be necessary to either reveal their astrophysical nature (as blazars or other active galactic nuclei, for example), or to further support the possibility that they are dark matter subhalos by failing to detect any non-gamma-ray counterpart. {\textcopyright} 2012 American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {1111.2613}, -author = {Belikov, Alexander V. and Buckley, Matthew R. and Hooper, Dan}, -doi = {10.1103/PhysRevD.86.043504}, -eprint = {1111.2613}, -issn = {15507998}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -number = {4}, -title = {{Searching for dark matter subhalos in the Fermi-LAT second source catalog}}, -volume = {86}, -year = {2012} -} -@article{Zhao1996, -abstract = {I present a general family of dynamical models with simple analytical potential-density pairs suited to modelling galactic bulges and nuclei with double power-law radial density profiles and an optional central black hole. Analytical expressions for the potential and velocity dispersion of these models are given for the spherical case. Many previously known analytical spherical models, including the recent $\gamma$/$\eta$-models by Dehnen and Tremaine et al., are special cases of this family. The family also forms a complete set for constructing general galaxy models or solving Poisson's equation in the non-spherical case. In particular, a generalized Clutton- Brock and Hernquist-Ostriker orthogonal basis set is given.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9509122}, -author = {Zhao, Hongsheng}, -doi = {10.1093/mnras/278.2.488}, -eprint = {9509122}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Celestial mechanics,Galaxies: kinematics and dynamics,Galaxies: nuclei,Methods: analytical,stellar dynamics}, -month = {jan}, -number = {2}, -pages = {488--496}, -primaryClass = {astro-ph}, -title = {{Analytical models for galactic nuclei}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996MNRAS.278..488Z&link_type=ABSTRACT%5Cnpapers2://publication/uuid/29FD512A-5F46-488B-A191-2EFF3CBEA33C}, -volume = {278}, -year = {1996} -} -@article{Hopkins2006, -abstract = {We present an evolutionary model for starbursts, quasars, and spheroidal galaxies in which mergers between gas-rich galaxies drive nuclear inflows of gas, producing intense starbursts and feeding the buried growth of supermassive black holes (BHs) until feedback expels gas and renders a briefly visible optical quasar. The quasar lifetime and obscuring column density depend on both the instantaneous and peak luminosity of the quasar, and we determine this dependence using a large set of simulations of galaxy mergers varying host galaxy properties, orbital geometry, and gas physics. We use these fits to deconvolve observed quasar luminosity functions (LFs) and obtain the evolution of the formation rate of quasars with a certain peak luminosity, n(L_peak,z). Quasars spend extended periods of time at luminosities well below peak, and so n(L_peak) has a maximum corresponding to the 'break' in the observed LF, falling off at both brighter and fainter luminosities. From n(L_peak) and our simulation results, we obtain self-consistent fits to hard and soft X-ray and optical quasar LFs and predict many observables, including: column density distributions of optical and X-ray samples, the LF of broad-line quasars in X-ray samples and the broad-line fraction as a function of luminosity, active BH mass functions, the distribution of Eddington ratios at z$\sim$0-2, the z=0 mass function of relic BHs and total mass density of BHs, and the cosmic X-ray background. In every case, our predictions agree well with observed estimates, and unlike previous modeling attempts, we are able to reproduce them without invoking any ad hoc assumptions about source properties or distributions. We provide a library of Monte Carlo realizations of our models for comparison with observations. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506398}, -author = {Hopkins, Philip F. and Hernquist, Lars and Cox, Thomas J. and {Di Matteo}, Tiziana and Robertson, Brant and Springel, Volker}, -doi = {10.1086/499298}, -eprint = {0506398}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins et al. - 2006 - A Unified, Merger‐driven Model of the Origin of Starbursts, Quasars, the Cosmic X‐Ray Background, Supermassive B.pdf:pdf}, -isbn = {doi:10.1086/499298}, -issn = {0067-0049}, -journal = {The Astrophysical Journal Supplement Series}, -number = {1}, -pages = {1--49}, -primaryClass = {astro-ph}, -title = {{A Unified, Merger‐driven Model of the Origin of Starbursts, Quasars, the Cosmic X‐Ray Background, Supermassive Black Holes, and Galaxy Spheroids}}, -url = {http://arxiv.org/abs/astro-ph/0506398%0Ahttp://dx.doi.org/10.1086/499298}, -volume = {163}, -year = {2006} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58 arcsec in the i band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including an $\sim$10 per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally,we check the sensitivity of our shear calibration estimates to other cutsmade on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalogue are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E. and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Mandelbaum et al. - 2018 - Weak lensing shear calibration with simulations of the HSC survey(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{Hoekstra2004, -abstract = {We present the results of a study of weak lensing by galaxies based on 45.5 deg{\$}{\^{}}2{\$} of {\$}R{\_}C{\$} band imaging data from the Red-Sequence Cluster Survey (RCS). We present the first weak lensing detection of the flattening of galaxy dark matter halos. We use a simple model in which the ellipticity of the halo is {\$}f{\$} times the observed ellipticity of the lens. We find a best fit value of {\$}f=0.77{\^{}}{\{}+0.18{\}}{\_}{\{}-0.21{\}}{\$}, suggesting that the dark matter halos are somewhat rounder than the light distribution. The fact that we detect a significant flattening implies that the halos are well aligned with the light distribution. Given the average ellipticity of the lenses, this implies a halo ellipticity of {\$}{\textless}e{\_}{\{}\backslashrm halo{\}} {\textgreater}=0.33{\^{}}{\{}+0.07{\}}{\_}{\{}-0.09{\}}{\$}, in fair agreement with results from numerical simulations of CDM. This result provides strong support for the existence of dark matter, as an isotropic lensing signal is excluded with 99.5{\%} confidence. We also study the average mass profile around the lenses, using a maximum likelihood analysis. We consider two models for the halo mass profile: a truncated isothermal sphere (TIS) and an NFW profile. We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo. The best fit NFW model yields a mass {\$}M{\_}{\{}200{\}}=(8.4\backslashpm0.7\backslashpm0.4)\backslashtimes 10{\^{}}{\{}11{\}} h{\^{}}{\{}-1{\}} M{\_}\backslashodot{\$} and a scale radius {\$}r{\_}s=16.2{\^{}}{\{}+3.6{\}}{\_}{\{}-2.9{\}} h{\^{}}{\{}-1{\}}{\$} kpc. This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, H K C and Gladders, Michael D}, -doi = {10.1086/382726}, -eprint = {0306515}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of Galaxy Dark Matter Halos from Weak Lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2004} -} -@article{Weinberg2002, -abstract = {Simulations predict that the dark matter halos of galaxies should have central cusps, while those inferred from observed galaxies do not have cusps. We demonstrate, using both linear perturbation theory and n-body simulations, that a disk bar, which should be ubiquitous in forming galaxies, can produce cores in cuspy CDM dark matter profiles within five bar orbital times. Simulations of forming galaxies suggest that one of Milky Way size could have a 10 kpc primordial bar; this bar will remove the cusp out to approximately 5 kpc in approximately 1.5 gigayears, while the disk only loses approximately 8% of its original angular momentum. An inner Lindblad-like resonance couples the rotating bar to orbits at all radii through the cusp, transferring the bar pattern angular momentum to the dark matter cusp, rapidly flattening it. This resonance disappears for profiles with cores and is responsible for a qualitative difference in bar driven halo evolution with and without a cusp. This bar induced evolution will have a profound effect on the structure and evolution of almost all galaxies. Hence, both to understand galaxy formation and evolution and to make predictions from theory it is necessary to resolve these dynamical processes. Unfortunately, correctly resolving these important dynamical processes in ab initio calculations of galaxy formation is a daunting task, requiring at least 4,000,000 halo particles using our SCF code, and probably requiring many times more particles when using noisier tree, direct summation, or grid based techniques, the usual methods employed in such calculations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0110632}, -author = {Weinberg, Martin D. and Katz, Neal}, -doi = {10.1086/343847}, -eprint = {0110632}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {627--633}, -primaryClass = {astro-ph}, -title = {{Bar‐driven Dark Halo Evolution: A Resolution of the Cusp‐Core Controversy}}, -url = {http://arxiv.org/abs/astro-ph/0110632}, -volume = {580}, -year = {2002} -} -@article{Lin2018, -abstract = {A Python non-uniform fast Fourier transform (PyNUFFT) package has been developed to accelerate multidimensional non-Cartesian image reconstruction on heterogeneous platforms. Since scientific computing with Python encompasses a mature and integrated environment, the time efficiency of the NUFFT algorithm has been a major obstacle to real-time non-Cartesian image reconstruction with Python. The current PyNUFFT software enables multi-dimensional NUFFT accelerated on a heterogeneous platform, which yields an efficient solution to many non-Cartesian imaging problems. The PyNUFFT also provides several solvers, including the conjugate gradient method, 1 total variation regularized ordinary least square (L1TV-OLS), and 1 total variation regularized least absolute deviation (L1TV-LAD). Metaprogramming libraries have been employed to accelerate PyNUFFT. The PyNUFFT package has been tested on multi-core central processing units (CPUs) and graphic processing units (GPUs), with acceleration factors of 6.3–9.5× on a 32-thread CPU platform and 5.4–13× on a GPU.}, -author = {Lin, Jyh Miin}, -doi = {10.3390/jimaging4030051}, -issn = {2313433X}, -journal = {Journal of Imaging}, -keywords = {Graphic processing unit (GPU),Heterogeneous system architecture (HSA),Magnetic resonance imaging (MRI),Multi-core system,Total variation (TV)}, -number = {3}, -pages = {1--22}, -title = {{Python non-uniform fast fourier transform (PyNUFFT): An accelerated non-cartesian MRI package on a heterogeneous platform (CPU/GPU)}}, -volume = {4}, -year = {2018} -} -@article{Greco2017, -abstract = {We present our catalog of extended low-surface-brightness galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first {\$}{\{}\backslashbackslashsim{\{}\backslash{\}}{\}}{\$}200 deg{\$}{\^{}}2{\$} of the survey, we have uncovered a rich diversity of LSB phenomena, including red ({\$}g-i\backslashbackslashgeq0.64{\$}) and blue ({\$}g-i{\textless}0.64{\$}) LSBGs with a wide range of morphologies, tidal debris from galaxy interactions, and cirrus emission from Galactic dust. We publish a catalog of 781 LSBGs, which, because we focus on angularly extended galaxies ({\$}r{\_}\backslashbackslashmathrm{\{}\backslash{\{}{\}}eff{\{}\backslash{\}}{\}}=2.5{\$}-{\$}14{\^{}}{\{}\backslashbackslashprime\backslashbackslashprime{\{}\backslash{\}}{\}}{\$}), is likely dominated by low-redshift objects. We define LSBGs to have mean surface brightnesses {\$}\backslashbackslashbar{\{}\backslash{\{}{\}}\backslashbackslashmu{\{}\backslash{\}}{\}}{\_}\backslashbackslashmathrm{\{}\backslash{\{}{\}}eff{\{}\backslash{\}}{\}}(g){\textgreater}24.3{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, which allows nucleated galaxies into our sample. As a result, the central surface brightness distribution spans a wide range of {\$}\backslashbackslashmu{\{}\backslash{\_}{\}}0(g)=18{\$}-{\$}27.4{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, with 50{\%} and 95{\%} of galaxies fainter than 24.3 and 22 mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, respectively. Furthermore, the mean surface brightness distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well-characterized by single-component S{\$}\backslash{\$}'{\{}e{\}}rsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We crossmatch our sample with existing optical, HI, and ultraviolet catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, with galaxies ranging from dwarf spheroidals and ultra-diffuse galaxies in nearby groups to gas-rich (physically large) irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the galaxy population at low surface brightnesses.}, -archivePrefix = {arXiv}, -arxivId = {1709.04474}, -author = {Greco, Johnny P and Greene, Jenny E and Strauss, Michael A and MacArthur, Lauren A and Flowers, Xzavier and Goulding, Andy D and Huang, Song and Kim, Ji Hoon and Komiyama, Yutaka and Leauthaud, Alexie and Leisman, Lukas and Lupton, Robert H and Sif{\'{o}}n, Crist{\'{o}}bal and Wang, Shiang-Yu}, -doi = {10.3847/1538-4357/aab842}, -eprint = {1709.04474}, -issn = {15384357}, -keywords = {dwarf,galaxies,general,keywords}, -title = {{Illuminating Low-Surface-Brightness Galaxies with the Hyper Suprime-Cam Survey}}, -url = {http://arxiv.org/abs/1709.04474}, -year = {2017} -} -@article{Wang2017, -abstract = {Difference imaging or image subtraction is a method that measures differential photometry by matching the pointing and point-spread function (PSF) between image frames. It is used for the detection of time-variable phenomena. Here we present a new category of method---CPM Difference Imaging, in which differences are not measured between matched images but instead between image frames and a data-driven predictive model that has been designed only to predict the pointing, PSF, and detector effects but not astronomical variability. In CPM Difference Imaging each pixel is modelled by the Causal Pixel Model (CPM) originally built for modeling Kepler data, in which pixel values are predicted by a linear combination of other pixels at the same epoch but far enough away such that these pixels are causally disconnected, astrophysically. It does not require that the user have any explicit model or description of the pointing or point-spread function of any of the images. Its principal drawback is that---in its current form---it requires an imaging campaign with many epochs and fairly stable telescope pointing. The method is applied to simulated data and also the K2 Campaign 9 microlensing data. We show that CPM Difference Imaging can detect variable objects and produce precise differentiate photometry in a crowded field. CPM Difference Imaging is capable of producing image differences at nearly photon-noise precision.}, -archivePrefix = {arXiv}, -arxivId = {1710.02428}, -author = {Wang, Dun and Hogg, David W and Foreman-Mackey, Daniel and Sch{\"{o}}lkopf, Bernhard}, -eprint = {1710.02428}, -pages = {1--23}, -title = {{A pixel-level model for event discovery in time-domain imaging}}, -url = {http://arxiv.org/abs/1710.02428}, -year = {2017} -} -@article{Reines2015, -abstract = {Scaling relations between central black hole (BH) mass and host galaxy properties are of fundamental importance to studies of BH and galaxy evolution throughout cosmic time. Here we investigate the relationship between BH mass and host galaxy total stellar mass using a sample of 262 broad-line active galactic nuclei (AGNs) in the nearby universe (z {\textless} 0.055), as well as 79 galaxies with dynamical BH masses. The vast majority of our AGN sample is constructed using Sloan Digital Sky Survey spectroscopy and searching for Seyfert-like narrow-line ratios and broad H$\alpha$ emission. BH masses are estimated using standard virial techniques. We also include a small number of dwarf galaxies with total stellar masses Mstellar ≲ 109.5 Mo and a subsample of the reverberation-mapped AGNs. Total stellar masses of all 341 galaxies are calculated in the most consistent manner feasible using color-dependent mass-to-light ratios. We find a clear correlation between BH mass and total stellar mass for the AGN host galaxies, with MBH ∝ Mstellar, similar to that of early-type galaxies with dynamically detected BHs. However, the relation defined by the AGNs has a normalization that is lower by more than an order of magnitude, with a BH-to-total stellar mass fraction of MBH/Mstellar ∼ 0.025{\%} across the stellar mass range 108 ≤ Mstellar/Mo ≤ 1012. This result has significant implications for studies at high redshift and cosmological simulations in which stellar bulges cannot be resolved.}, -archivePrefix = {arXiv}, -arxivId = {1508.06274}, -author = {Reines, Amy E and Volonteri, Marta}, -doi = {10.1088/0004-637X/813/2/82}, -eprint = {1508.06274}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: Seyfert,galaxies: active,galaxies: evolution,galaxies: nuclei}, -number = {2}, -title = {{RELATIONS between CENTRAL BLACK HOLE MASS and TOTAL GALAXY STELLAR MASS in the LOCAL UNIVERSE}}, -volume = {813}, -year = {2015} -} -@article{Kormendy2013, -abstract = {Supermassive black holes (BHs) have been found in 85 galaxies by dynamical modeling of spatially resolved kinematics. The Hubble Space Telescope revolutionized BH research by advancing the subject from its proof-of-concept phase into quantitative studies of BH demographics. Most influential was the discovery of a tight correlation between BH mass and the velocity dispersion $\sigma$ of the bulge component of the host galaxy. Together with similar correlations with bulge luminosity and mass, this led to the widespread belief that BHs and bulges coevolve by regulating each other's growth. Conclusions based on one set of correlations from in brightest cluster ellipticals to in the smallest galaxies dominated BH work for more than a decade. New results are now replacing this simple story with a richer and more plausible picture in which BHs correlate differently with different galaxy components. A reasonable aim is to use this progress to refine our understanding of BH-galaxy coevolution. BHs with masses of 105-106Mȯ are found in many bulgeless galaxies. Therefore, classical (elliptical-galaxy-like) bulges are not necessary for BH formation. On the other hand, although they live in galaxy disks, BHs do not correlate with galaxy disks. Also, any correlations with the properties of disk-grown pseudobulges and dark matter halos are weak enough to imply no close coevolution. The above and other correlations of host-galaxy parameters with each other and with suggest that there are four regimes of BH feedback. (1) Local, secular, episodic, and stochastic feeding of small BHs in largely bulgeless galaxies involves too little energy to result in coevolution. (2) Global feeding in major, wet galaxy mergers rapidly grows giant BHs in short-duration, quasar-like events whose energy feedback does affect galaxy evolution. The resulting hosts are classical bulges and coreless-rotating-disky ellipticals. (3) After these AGN phases and at the highest galaxy masses, maintenance-mode BH feedback into X-ray-emitting gas has the primarily negative effect of helping to keep baryons locked up in hot gas and thereby keeping galaxy formation from going to completion. This happens in giant, core-nonrotating-boxy ellipticals. Their properties, including their tight correlations between and core parameters, support the conclusion that core ellipticals form by dissipationless major mergers. They inherit coevolution effects from smaller progenitor galaxies. Also, (4) independent of any feedback physics, in BH growth modes 2 and 3, the averaging that results from successive mergers plays a major role in decreasing the scatter in correlations from the large values observed in bulgeless and pseudobulge galaxies to the small values observed in giant elliptical galaxies.Copyright {\textcopyright}2013 by Annual Reviews. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1304.7762}, -author = {Kormendy, John and Ho, Luis C.}, -doi = {10.1146/annurev-astro-082708-101811}, -eprint = {1304.7762}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Kormandy2013CoEvoOrNot.pdf:pdf}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {Active galactic nuclei,Black holes,Galaxy dynamics,Galaxy evolution,Galaxy structure}, -number = {4}, -pages = {511--653}, -title = {{Coevolution (or not) of supermassive black holes and host galaxies}}, -volume = {51}, -year = {2013} -} -@article{Harvey2015, -abstract = {Collisions between galaxy clusters provide a test of the non-gravitational forces acting on dark matter. Dark matter's lack of deceleration in the `bullet cluster collision' constrained its self-interaction cross-section {\$}\backslash{\$}sigma{\_}DM/m {\textless}1.25cm2/g (68{\%} confidence limit) for long-ranged forces. Using the Chandra and Hubble Space Telescopes we have now observed 72 collisions, including both `major' and `minor' mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6{\$}\backslash{\$}sigma significance. The position of the dark mass has remained closely aligned within 5.8+/-8.2 kpc of associated stars: implying a self-interaction cross-section {\$}\backslash{\$}sigma{\_}DM/m {\textless}0.47 cm2/g (95{\%} CL) and disfavoring some proposed extensions to the standard model.}, -archivePrefix = {arXiv}, -arxivId = {1503.07675}, -author = {Harvey, David and Massey, Richard and Kitching, Thomas and Taylor, Andy and Tittley, Eric}, -doi = {10.1126/science.1261381}, -eprint = {1503.07675}, -issn = {10959203}, -journal = {Science}, -number = {6229}, -pages = {1462--1465}, -pmid = {25814581}, -title = {{The nongravitational interactions of dark matter in colliding galaxy clusters}}, -volume = {347}, -year = {2015} -} -@article{Cyr-Racine2019, -abstract = {Gravitational lensing has emerged as a powerful probe of the matter distribution on subgalactic scales, which itself may contain important clues about the fundamental origins and properties of dark matter. Broadly speaking, two different approaches have been taken in the literature to map the small-scale structure of the Universe using strong lensing, with one focused on measuring the position and mass of a small number of discrete massive subhalos appearing close in projection to lensed images, and the other focused on detecting the collective effect of all the small-scale structure between the lensed source and the observer. In this paper, we follow the latter approach and perform a detailed study of the sensitivity of galaxy-scale gravitational lenses to the ensemble properties of small-scale structure. As in some previous studies, we adopt the language of the substructure power spectrum to characterize the statistical properties of the small-scale density field. We present a comprehensive theory that treats lenses with extended sources as well as those with time-dependent compact sources (such as quasars) in a unified framework for the first time. Our approach uses mode functions to provide both computational advantages and insights about couplings between the lens and source. The goal of this paper is to develop the theory and gain the intuition necessary to understand how the sensitivity to the substructure power spectrum depends on the source and lens properties, with the eventual aim of identifying the most promising targets for such studies.}, -archivePrefix = {arXiv}, -arxivId = {1806.07897}, -author = {Cyr-Racine, Francis-Yan and Keeton, Charles R. and Moustakas, Leonidas A.}, -doi = {10.1103/physrevd.100.023013}, -eprint = {1806.07897}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cyr-Racine, Keeton, Moustakas - 2019 - Beyond subhalos Probing the collective effect of the Universe's small-scale structure with gravit.pdf:pdf}, -issn = {2470-0010}, -journal = {Physical Review D}, -number = {2}, -pages = {1--30}, -title = {{Beyond subhalos: Probing the collective effect of the Universe's small-scale structure with gravitational lensing}}, -volume = {100}, -year = {2019} -} -@article{Hsueh2017, -abstract = {Flux-ratio anomalies in quasar lenses can be attributed to dark matter substructure surrounding the lensing galaxy and thus used to constrain the substructure mass fraction. Previous applications of this approach infer a substructure abundance that is potentially in tension with the predictions of $\Lambda$ cold dark matter cosmology. However, the assumption that all flux-ratio anomalies are due to substructure is a strong one and alternative explanations have not been fully investigated. Here, we use new high-resolution near-IR Keck II adaptive optics imaging for the lens system CLASS B0712+472 to perform pixel-based lens modelling for this system and, in combination with the new Very Long Baseline Array radio observations, show that the inclusion of the disc in the lens model can explain the flux-ratio anomalies without the need for dark matter substructures. The projected disc mass comprises 16 per cent of the total lensing mass within the Einstein radius and the total disc mass is 1.79 × 1010M⊙. The case of B0712+472 adds to the evidence that not all flux-ratio anomalies are due to dark subhaloes and highlights the importance of taking the effects of baryonic structures more fully into account in order to obtain an accurate measure of the substructure mass fraction.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1701.06575}, -author = {Hsueh, J. W. and Oldham, L. and Spingola, C. and Vegetti, S. and Fassnacht, C. D. and Auger, M. W. and Koopmans, L. V.E. and McKean, J. P. and Lagattuta, D. J.}, -doi = {10.1093/mnras/stx1082}, -eprint = {1701.06575}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hsueh et al. - 2017 - SHARP - IV. An apparent flux-ratio anomaly resolved by the edge-on disc in B0712 472.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Gravitational lensing: strong,galaxies: structure,quasars: individual: CLASS B0712+472}, -number = {3}, -pages = {3713--3721}, -title = {{SHARP - IV. An apparent flux-ratio anomaly resolved by the edge-on disc in B0712 + 472}}, -url = {http://arxiv.org/abs/1701.06575%0Ahttp://dx.doi.org/10.1093/mnras/stx1082}, -volume = {469}, -year = {2017} -} -@article{Report2011, -abstract = {Modelling students' behaviour in relation to tuition fees is a complex task since students' 'talent' is not common knowledge. Students observe a private noisy signal of their abilities, while university receives noisy information based on the quantitative and qualitative data provided by university applicants. In this article, we add the heterogeneity of the population to this model: we assume that this heterogeneity means that the perception of skills among a part of the population is biased and underestimates the capabilities of its members to succeed in the higher education system. Our conclusions differ from those derived in the literature and show in particular that the optimal tuition fees for a given number of students are lower than those obtained for a homogeneous population. {\textcopyright} 2013 Copyright Taylor and Francis Group, LLC.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Flacher, Harari-Kermadec - 2013 - Tuition fees, self-esteem and social heterogeneity.pdf:pdf}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Gadotti2008a, -abstract = {We have performed 2D bulge/bar/disc decompositions using g, r and i-band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for the bulge-to-total ratio than the global S{\'{e}}rsic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour-magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between the bulge S{\'{e}}rsic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass-size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass-size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0810.1953}, -author = {Gadotti, Dimitri A.}, -doi = {10.1111/j.1365-2966.2008.14257.x}, -eprint = {0810.1953}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gadotti - 2009 - Structural properties of pseudo-bulges, classical bulges and elliptical galaxies A Sloan Digital Sky Survey perspect(2).pdf:pdf}, -isbn = {0372-9311 (Print)\r0372-9311 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {1531--1552}, -pmid = {20063786}, -title = {{Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: A Sloan Digital Sky Survey perspective}}, -url = {http://arxiv.org/abs/0810.1953%0Ahttp://dx.doi.org/10.1111/j.1365-2966.2008.14257.x}, -volume = {393}, -year = {2009} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58" in the {\$}i{\$}-band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including a {\$}\backslashbackslashsim 10{\$} per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally, we check the sensitivity of our shear calibration estimates to other cuts made on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalog are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{Shao2016, -abstract = {The spatial distribution of the satellite populations of the Milky Way and Andromeda are puzzling in that they are nearly perpendicular to the disks of their central galaxies. To understand the origin of such configurations we study the alignment of the central galaxy, satellite system and dark matter halo in the largest of the "Evolution and Assembly of GaLaxies and their Environments" (EAGLE) simulation. We find that centrals and their satellite systems tend to be well aligned with their haloes, with a median misalignment angle of {\$}33{\^{}}{\{}\backslashcirc{\}}{\$} in both cases. While the centrals are better aligned with the inner {\$}10{\$} kpc halo, the satellite systems are better aligned with the entire halo indicating that satellites preferentially trace the outer halo. The central - satellite alignment is weak (median misalignment angle of {\$}52{\^{}}{\{}\backslashcirc{\}}{\$}) and we find that around {\$}20\backslash{\%}{\$} of systems have a misalignment angle larger than {\$}78{\^{}}{\{}\backslashcirc{\}}{\$}, which is the value for the Milky Way. The central - satellite alignment is a consequence of the tendency of both components to align with the dark matter halo. As a consequence, when the central is parallel to the satellite system, it also tends to be parallel to the halo. In contrast, if the central is perpendicular to the satellite system, as in the case of the Milky Way and Andromeda, then the central - halo alignment is much weaker. Dispersion-dominated (spheroidal) centrals have a stronger alignment with both their halo and their satellites than rotation-dominated (disk) centrals. We also found that the halo, the central galaxy and the satellite system tend to be aligned with the surrounding large-scale distribution of matter, with the halo being the better aligned of the three.}, -archivePrefix = {arXiv}, -arxivId = {1605.01728}, -author = {Shao, Shi and Cautun, Marius and Frenk, Carlos S and Gao, Liang and Crain, Robert A and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw1247}, -eprint = {1605.01728}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3772--3783}, -title = {{Alignments between galaxies, satellite systems and haloes}}, -volume = {460}, -year = {2016} -} -@article{Peter2013, -abstract = {If dark matter has a large self-interaction scattering cross-section, then interactions among dark-matter particles will drive galaxy and cluster haloes to become spherical in their centres. Work in the past has used this effect to rule out velocity-independent, elastic cross-sections larger than $\sigma$/m ≃ 0.02 cm2 g-1 based on comparisons to the shapes of galaxy cluster lensing potentials and X-ray isophotes. In this paper, we use cosmological simulations to show that these constraints were off by more than an order of magnitude because (a) they did not properly account for the fact that the observed ellipticity gets contributions from the triaxial mass distribution outside the core set by scatterings, (b) the scatter in axis ratios is large and (c) the core region retains more of its triaxial nature than estimated before. Including these effects properly shows that the same observations now allow dark matter self-interaction cross-sections at least as large as $\sigma$/m = 0.1 cm2 g-1. We show that constraints on self-interacting dark matter from strong-lensing clusters are likely to improve significantly in the near future, but possibly more via central densities and core sizes than halo shapes. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1208.3026}, -author = {Peter, Annika H.G. and Rocha, Miguel and Bullock, James S. and Kaplinghat, Manoj}, -doi = {10.1093/mnras/sts535}, -eprint = {1208.3026}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Methods: numerical}, -number = {1}, -pages = {105--120}, -title = {{Cosmological simulations with self-interacting dark matter - II. Halo shapes versus observations}}, -volume = {430}, -year = {2013} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the $\Lambda$CDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no significant detection of a stellar halo, as in the case of M101, NGC 3351 and NGC 1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies in the range M200 = 8 × 1011-2 × 1012 M⊙ with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction fSH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming, and assemble their dark matter halos earlier than galaxies with similar masses. They have also accreted more low-mass satellites at earlier infall times than centrals with high fSH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretiondominated r {\$\sim${}} 45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers at higher redshifts and evolved unperturbed in the last {\$\sim${}}10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M and Sales, Laura V and Creasey, Peter and Cooper, Michael C and Bullock, James S and {Michael Rich}, R and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Greco2017, -abstract = {We present a catalog of extended low-surface-brightness galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first {\$}{\{}\backslashsim{\}}{\$}200 deg{\$}{\^{}}2{\$} of the survey, we have uncovered 781 LSBGs, spanning red ({\$}g-i\backslashgeq0.64{\$}) and blue ({\$}g-i{\textless}0.64{\$}) colors and a wide range of morphologies. Since we focus on extended galaxies ({\$}r{\_}\backslashmathrm{\{}eff{\}}=2.5{\$}-{\$}14{\^{}}{\{}\backslashprime\backslashprime{\}}{\$}), our sample is likely dominated by low-redshift objects. We define LSBGs to have mean surface brightnesses {\$}\backslashbar{\{}\backslashmu{\}}{\_}\backslashmathrm{\{}eff{\}}(g){\textgreater}24.3{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, which allows nucleated galaxies into our sample. As a result, the central surface brightness distribution spans a wide range of {\$}\backslashmu{\_}0(g)=18{\$}-{\$}27.4{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, with 50{\%} and 95{\%} of galaxies fainter than 24.3 and 22 mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, respectively. Furthermore, the surface brightness distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well-characterized by single-component S$\backslash$'{\{}e{\}}rsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We crossmatch our sample with existing optical, HI, and ultraviolet catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, ranging from dwarf spheroidals and ultra-diffuse galaxies in nearby groups to gas-rich irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the LSBG population.}, -archivePrefix = {arXiv}, -arxivId = {1709.04474}, -author = {Greco, Johnny P and Greene, Jenny E and Strauss, Michael A and Macarthur, Lauren A and Flowers, Xzavier and Goulding, Andy D and Huang, Song and Kim, Ji Hoon and Komiyama, Yutaka and Leauthaud, Alexie and Leisman, Lukas and Lupton, Robert H and Sif{\'{o}}n, Crist{\'{o}}bal and Wang, Shiang-Yu}, -doi = {10.3847/1538-4357/aab842}, -eprint = {1709.04474}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {dwarf,galaxies,general,keywords}, -number = {2}, -pages = {104}, -title = {{Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey}}, -url = {http://arxiv.org/abs/1709.04474%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aab842}, -volume = {857}, -year = {2018} -} -@article{Dominika2016, -abstract = {Spectral features introduced by instrumental chromaticity of radio interferometers have the potential to negatively impact the ability to perform Epoch of Reionisation (EoR) and Cosmic Dawn (CD) science using the redshifted neutral hydrogen emission line from the early Universe. We describe instrument calibration choices that influence the spectral characteristics of the science data, and assess their impact on EoR statistical and tomographic experiments. Principally, we consider the intrinsic spectral response of the receiving antennas, embedded within a complete frequency-dependent primary beam response, and frequency-dependent instrument sampling. We assess different options for bandpass calibration. The analysis is applied to the proposed SKA1-Low EoR/CD experiments. We provide tolerances on the smoothness of the SKA station primary beam bandpass, to meet the scientific goals of statistical and tomographic (imaging) EoR programs. Two calibration strategies are tested: (1) fitting of each fine channel independently, and (2) fitting of an nth-order polynomial for each {\$\sim${}}1{\$\sim${}}MHz coarse channel with (n+1)th-order residuals (n=2,3,4). Strategy (1) leads to uncorrelated power in the 2D power spectrum proportional to the thermal noise power, thereby reducing the overall array sensitivity. Strategy (2) leads to correlated residuals from the fitting, and residual signal power with (n+1)th-order curvature. For the residual power to be less than the thermal noise, the fractional amplitude of a fourth-order term in the bandpass across a single coarse channel must be {\textless}2.5{\%} (50{\$\sim${}}MHz), {\textless}0.5{\%} (150{\$\sim${}}MHz), {\textless}0.8{\%} (200{\$\sim${}}MHz). The tomographic experiment places stringent constraints on phase residuals in the bandpass. We find that the root-mean-square variability over all stations of the change in phase across any fine channel (4.578{\$\sim${}}kHz) should not exceed 0.2 degrees.}, -archivePrefix = {arXiv}, -arxivId = {1604.03273}, -author = {Trott, Cathryn M and Wayth, Randall B}, -doi = {10.1017/pas.2016.xxx}, -eprint = {1604.03273}, -issn = {14486083}, -journal = {arXiv preprint arXiv: {\ldots}}, -keywords = {aboriginal astronomy,ethnoastronomy,history of astronomy}, -number = {3}, -pages = {15}, -title = {{Australian Aboriginal Astronomy and Navigation arXiv:1607.02215v1}}, -url = {http://arxiv.org/abs/1604.03273}, -volume = {447}, -year = {2016} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and S{\'{e}}rsic index distributions obtained from two-dimensional structural fits to 40, 000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of S{\'{e}}rsic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. {\textcopyright}2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely, the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since {\$}z=1.0{\$}. We find that lower-mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher-mass or lower-redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys, we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -keywords = {cosmology,gravitational lensing,haloes - galaxies,strong - galaxies,structure -,theory - dark matter}, -number = {October}, -pages = {27}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {27}, -year = {2016} -} -@article{VanDerWel2012, -abstract = {We present global structural parameter measurements of 109,533 unique, H F160W-selected objects from the CANDELS multi-cycle treasury program. S{\'{e}}rsic model fits for these objects are produced with GALFIT in all available near-infrared filters (H F160W, J F125W and, for a subset, Y F105W). The parameters of the best-fitting S{\'{e}}rsic models (total magnitude, half-light radius, S{\'{e}}rsic index, axis ratio, and position angle) are made public, along with newly constructed point-spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties, we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements - to 10{\%} or better - of all structural parameters can typically be obtained for galaxies with H F160W {\textless} 23, with comparable fidelity for basic size and shape measurements for galaxies to H F160W ∼ 24.5. {\textcopyright}2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1211.6954}, -author = {{Van Der Wel}, A and Bell, E F and H{\"{a}}ussler, B and McGrath, E J and Chang, Yu Yen and Guo, Yicheng and McIntosh, D H and Rix, H W and Barden, M and Cheung, E and Faber, S M and Ferguson, H C and Galametz, A and Grogin, N A and Hartley, W and Kartaltepe, J S and Kocevski, D D and Koekemoer, A M and Lotz, J and Mozena, M and Peth, M A and Peng, Chien Y}, -doi = {10.1088/0067-0049/203/2/24}, -eprint = {1211.6954}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: high-redshift,galaxies: statistics,galaxies: structure surveys}, -number = {2}, -title = {{Structural parameters of galaxies in candels}}, -volume = {203}, -year = {2012} -} -@article{Hopkins2006, -abstract = {We present an evolutionary model for starbursts, quasars, and spheroidal galaxies in which mergers between gas-rich galaxies drive nuclear inflows of gas, producing intense starbursts and feeding the buried growth of supermassive black holes (BHs) until feedback expels gas and renders a briefly visible optical quasar. The quasar lifetime and obscuring column density depend on both the instantaneous and peak luminosity of the quasar, and we determine this dependence using a large set of simulations of galaxy mergers varying host galaxy properties, orbital geometry, and gas physics. We use these fits to deconvolve observed quasar luminosity functions (LFs) and obtain the evolution of the formation rate of quasars with a certain peak luminosity, n(L{\_}peak,z). Quasars spend extended periods of time at luminosities well below peak, and so n(L{\_}peak) has a maximum corresponding to the 'break' in the observed LF, falling off at both brighter and fainter luminosities. From n(L{\_}peak) and our simulation results, we obtain self-consistent fits to hard and soft X-ray and optical quasar LFs and predict many observables, including: column density distributions of optical and X-ray samples, the LF of broad-line quasars in X-ray samples and the broad-line fraction as a function of luminosity, active BH mass functions, the distribution of Eddington ratios at z{\$\sim${}}0-2, the z=0 mass function of relic BHs and total mass density of BHs, and the cosmic X-ray background. In every case, our predictions agree well with observed estimates, and unlike previous modeling attempts, we are able to reproduce them without invoking any ad hoc assumptions about source properties or distributions. We provide a library of Monte Carlo realizations of our models for comparison with observations. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506398}, -author = {Hopkins, Philip F and Hernquist, Lars and Cox, Thomas J and {Di Matteo}, Tiziana and Robertson, Brant and Springel, Volker}, -doi = {10.1086/499298}, -eprint = {0506398}, -isbn = {doi:10.1086/499298}, -issn = {0067-0049}, -journal = {The Astrophysical Journal Supplement Series}, -number = {1}, -pages = {1--49}, -primaryClass = {astro-ph}, -title = {{A Unified, Merger‐driven Model of the Origin of Starbursts, Quasars, the Cosmic X‐Ray Background, Supermassive Black Holes, and Galaxy Spheroids}}, -url = {http://arxiv.org/abs/astro-ph/0506398%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/499298}, -volume = {163}, -year = {2006} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disk and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al, we assume that galaxies form stars quiescently in a disk until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow disks again. Thus, an individual galaxy may pass through various phases of disk or spheroid dominance during its lifetime. To distinguish between disks and spheroids we add one additional free parameter to the semianalytic model of Cole et al. which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an Ω = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals and the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50{\%} of ellipticals, but only about 15{\%} of spirals, have undergone a major merger during the redshift interval 0.0 ≤ z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long timescale for galaxy mergers compared with the timescale for cluster assembly at high redshift. The assembly of low redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor halos. As a result z = 0 rich clusters become E/S0 dominated and we find a " Butcher-Oemler " effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1 and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between disks and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/9602085v1}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085v1}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {arXiv:astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{LaBarbera2019, -abstract = {Using new long-slit spectroscopy obtained with X-Shooter at ESO-VLT, we study, for the first time, radial gradients of optical and near-infrared initial mass function (IMF)-sensitive features in a representative sample of galaxies at the very high mass end of the galaxy population. The sample consists of seven early-type galaxies (ETGs) at z ∼ 0.05, with central velocity dispersion in the range 300 ≲ $\sigma$ ≲ 350 km s-1. Using state-of-the-art stellar population synthesis models, we fit a number of spectral indices, from different chemical species (including TiO and Na indices), to constrain the IMF slope (i.e. the fraction of lowmass stars), as a function of galactocentric distance, over a radial range out to ∼4 kpc. ETGs in our sample show a significant correlation of IMF slope and surface mass density. The bottom-heavy population (i.e. an excess of low-mass stars in the IMF) is confined to central galaxy regions with surface mass density above ∼ 1010M kpc-2, or, alternatively, within a characteristic radius of ∼2 kpc. Radial distance, in physical units, and surface mass density are the best correlators to IMF variations, with respect to other dynamical (e.g. velocity dispersion) and stellar population (e.g. metallicity) properties. Our results for the most massive galaxies suggest that there is no single parameter that fully explains variations in the stellar IMF, but IMF radial profiles at z ∼ 0 rather result from the complex formation and mass accretion history of galaxy inner and outer regions.}, -archivePrefix = {arXiv}, -arxivId = {1909.01382}, -author = {{La Barbera}, F. and Vazdekis, A. and Ferreras, I. and Pasquali, A. and Prieto, C. Allende and Mart{\'{i}}n-Navarro, I. and Aguado, D. S. and {De Carvalho}, R. R. and Rembold, S. and Falc{\'{o}}n-Barroso, J. and {Van De Ven}, G.}, -doi = {10.1093/mnras/stz2192}, -eprint = {1909.01382}, -file = {:C\:/Users/Jammy/Documents/Papers/Ellipticals/LaBerbera2019IMFVaryMostEll.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Fundamental parameters,Galaxies: Stellar content,cD- galaxies: Formation}, -number = {3}, -pages = {4090--4110}, -title = {{IMF radial gradients in most massive early-type galaxies}}, -volume = {489}, -year = {2019} -} -@article{Peirani2008, -abstract = {If there is one key element in the social psychology of behaviour that is still missing from Stern's ABC model, it is the role of habit. Stern (2000) acknowledges this and proposes that an integrated model of environmentally significant behaviour would consist of four factors: 1) attitudes; 2) contextual factors; 3) personal capabilities; and 4) habits. The general thrust of Stern's suggestion is very similar to an attempt made almost thirty years ago by social psychologist Harry Triandis to develop an integrated model of 'interpersonal' behaviour. Triandis recognised the key role played by both social factors and emotions in forming intentions. He also highlighted the importance of past behaviour on the present. On the basis of these observations, Triandis proposed a Theory of Interpersonal Behaviour (Figure 4) in which intentions – as in many of the other models – are immediate antecedents of behaviour. But crucially, habits also mediate behaviour. And both these influences are moderated by facilitating conditions. Behaviour in any situation is, according to Triandis, a function partly of the intention, partly of the habitual responses, and partly of the situational constraints and conditions. The intention is influenced by social and affective factors as well as by rational deliberations. One is neither fully deliberative, in Triandis' model, nor fully automatic. One is neither fully autonomous nor entirely social. Behaviour is influenced by moral beliefs, but the impact of these is moderated both by emotional drives and cognitive limitations. Social factors include norms, roles and self-concept. Norms are the social rules about what should and should not be done. Roles are 'sets of behaviours that are considered appropriate for persons holding particular positions in a group' (Triandis, 1977). Self-concept refers to the idea that a person has of his/herself, the goals that it is appropriate for the person to pursue or to eschew, and the behaviours that the person does or does not engage in. Emotional responses to a decision or to a decision situation are assumed distinct from rational-instrumental evaluations of consequences, and may include both positive and negative emotional responses of varying strengths. Affect has a more or less unconscious input to decision-making, and is governed by instinctive behavioural responses to particular situations. Figure 3 Triandis' Theory of Interpersonal Behaviour Triandis offers an explicit role for affective factors on behavioural intentions. In more recent writings, the attempt to incorporate emotional antecedents into a model of action has received a lot of support (Bagozzi et al., 2002, Steg et al., 2001). Triandis theory of interpersonal behaviour captures many of the criticisms levelled at rational choice theory in a way that is not done by some of the other models. It also can be, and has been, used as a framework for empirical analysis of the strengths and weaknesses of the component factors in different kinds of situations. It also can be, and has been, used as the framework for empirical analysis of the strengths and weaknesses of the component factors in different kinds of situations. Far less use has been made of Triandis work than was made of the Ajzen-Fishbein work. However, where it has been used, it appears to have additional explanatory value over Ajzen's model, in particular, by including role beliefs and habits. Affect}, -archivePrefix = {arXiv}, -arxivId = {arXiv:0803.1210v1}, -author = {Zanna, G Del}, -doi = {10.1051/0004-6361}, -eprint = {arXiv:0803.1210v1}, -isbn = {0902009192}, -issn = {01851101}, -journal = {Astronomy}, -keywords = {activity,corona,sun,uv radiation}, -month = {feb}, -number = {2}, -pages = {52--55}, -pmid = {9010224}, -title = {{Special feature Flows in active region loops observed by Hinode EIS}}, -volume = {52}, -year = {2008} -} -@article{Kennicutt, -abstract = {We review progress over the past decade in observations of large-scale star formation, with a focus on the interface between extragalactic and Galactic studies. Methods of measuring gas contents and star-formation rates are discussed, and updated prescriptions for calculating star-formation rates are provided. We review relations between star formation and gas on scales ranging from entire galaxies to individual molecular clouds. Copyright {\textcopyright}2012 by Annual Reviews.}, -archivePrefix = {arXiv}, -arxivId = {1204.3552}, -author = {Kennicutt, Robert C and Evans, Neal J}, -doi = {10.1146/annurev-astro-081811-125610}, -eprint = {1204.3552}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {clouds,evolution,interstellar medium (ISM),molecules}, -number = {1}, -pages = {531--608}, -title = {{Star formation in the milky way and nearby galaxies}}, -url = {http://arxiv.org/abs/1204.3552%7B%5C%25%7D0Ahttp://dx.doi.org/10.1146/annurev-astro-081811-125610}, -volume = {50}, -year = {2012} -} -@article{Xie:2015aa, -abstract = {Recent work has suggested that the amplitude of the size mass relation of massive early type galaxies evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive early type galaxies. We find this model is able to reproduce the amplitude of present day amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark halos at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than {\$}10{\^{}}{\{}11.4{\}}M{\_}{\{}\backslashodot{\}}{\$}. At lower masses, low mass ratio mergers play a more important role. In situ star formation contribute more to the size growth than it does to stellar mass growth. We also find that, for ETGs identified at {\$}z=2{\$}, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -month = {feb}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Emsellem2011, -abstract = {{We provide a census of the apparent stellar angular momentum within 1 Re of a volume-limited sample of 260 early-type galaxies (ETGs) in the nearby Universe, using integral-field spectroscopy obtained in the course of the ATLAS3D project. We exploit the LambdaR parameter to characterise the existence of two families of ETGs: Slow Rotators which exhibit complex stellar velocity fields and often include stellar kinematically Distinct Cores (KDCs), and Fast Rotators which have regular velocity fields. Our complete sample of 260 ETGs leads to a new criterion to disentangle Fast and Slow Rotators which now includes a dependency on the apparent ellipticity (Epsilon). It separates the two classes significantly better than the previous prescription, and than a criterion based on V/Sigma: Slow Rotators and Fast Rotators have LambdaR lower and larger than kFSxSQRT(Epsilon), respectively, where kFS=0.31 for measurements made within 1 Re. We show that the vast majority of early-type galaxies are Fast Rotators: these have regular stellar rotation, with aligned photometric and kinematic axes (Paper II, Krajnovic et al. 2011{\}}, include discs and often bars and represent 86{\%} (224/260) of all early-type galaxies in the volume-limited ATLAS3D sample. Fast Rotators span the full range of apparent ellipticities from 0 to 0.85, and we suggest that they cover intrinsic ellipticities from about 0.35 to 0.85, the most flattened having morphologies consistent with spiral galaxies. Only a small fraction of ETGs are Slow Rotators representing 14{\%} (36/260) of the ATLAS3D sample of ETGs. Of all Slow Rotators, 11{\%} (4/36) exhibit two counter-rotating stellar disc-like components and are rather low mass objects (Mdyn{\textless}10{\^{}}10.5 M{\_}Sun). All other Slow Rotators (32/36) appear relatively round on the sky (Epsilon{\_}e{\textless}0.4), tend to be massive (Mdyn{\textgreater}10{\^{}}10.5 M{\_}Sun), and often (17/32) exhibit KDCs.}, -archivePrefix = {arXiv}, -arxivId = {1102.4444}, -author = {Emsellem, Eric and Cappellari, Michele and Krajnovi{\'{c}}, Davor and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Davies, Roger L and Davis, Timothy A and de Zeeuw, P T and Khochfar, Sadegh and Kuntschner, Harald and Lablanche, Pierre Yves and Mcdermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and van de Ven, Glenn and Weijmans, Anne Marie and Young, Lisa M}, -doi = {10.1111/j.1365-2966.2011.18496.x}, -eprint = {1102.4444}, -isbn = {13844}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {2}, -pages = {888--912}, -pmid = {13736}, -title = {{The ATLAS 3D project - III. A census of the stellar angular momentum within the effective radius of early-type galaxies: Unveiling the distribution of fast and slow rotators}}, -volume = {414}, -year = {2011} -} -@article{Wang2013, -abstract = {We investigate the spatial distribution of galactic satellites in high-resolution simulations of structure formation in the $\Lambda$ cold dark matter ($\Lambda$CDM) model: the Aquarius dark matter simulations of individual haloes and the Millennium-II simulation of a large cosmological volume. To relate the simulations to observations of the Milky Way we use two alternative models to populate dark haloes with 'visible' galaxies: a semi-analytic model of galaxy formation and an abundance matching technique. We find that the radial density profile of massive satellites roughly follows that of the dark matter halo (unlike the distribution of dark matter subhaloes). Furthermore, our two galaxy formation models give resultsconsistent with the observed profile of the 11 classical satellites of the Milky Way. Our simulations predict that larger, fainter samples of satellites should still retain this profile at least up to samples of 100 satellites. The angular distribution of the classical satellites of the Milky Way is known to be highly anisotropic. Depending on the exact measure of flattening, 5-10 per cent of satellite systems in our simulations are as flat as the Milky Way's and this fraction does not change when we correct for possible obscuration of satellites by the Galactic disc. A moderate flattening ofsatellite systems is a general property of $\Lambda$CDM, best understood as the consequence of preferential accretion along filaments of the cosmic web. Accretion of a single rich group of satellites can enhance the flattening due to such anisotropic accretion. We verify that a typical Milky Way-mass cold dark matter halo does not acquire its 11 most massive satellites from a small number of rich groups. Single-group accretion becomes more likely for less massive satellites. Our model predictions should be testable with forthcoming studies of satellite systems in other galaxies and surveys of fainter satellites in the MilkyWay. {\textcopyright}2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1206.1340}, -author = {Wang, Jie and Frenk, Carlos S and Cooper, Andrew P}, -doi = {10.1093/mnras/sts442}, -eprint = {1206.1340}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxy: formation,Galaxy: structure,Methods: numerical}, -number = {2}, -pages = {1502--1513}, -title = {{The spatial distribution of galactic satellites in the $\Lambda$ cold dark matter cosmology}}, -volume = {429}, -year = {2013} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular it demands highly efficient machine learning and image analysis algorithms. But scalability is not the only challenge: Astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. We argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. In the following, we will present this exciting application area for data scientists. We will focus on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from $\sim$1011 to > 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above $\sim$1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K.}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/K{\"{u}}ng et al. - 2018 - Models of gravitational lens candidates from SpaceWarps CFHTLS(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Sales2012, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V. and Navarro, Julio F. and Theuns, Tom and Schaye, Joop and White, Simon D.M. and Frenk, Carlos S. and Crain, Robert A. and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sales et al. - 2012 - The origin of discs and spheroids in simulated galaxies(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {jun}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as 'notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude ({\textless}50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 {\textless} G {\textless} 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G M and Prod'homme, T and Murray, N J and Crowley, C and Hopkinson, G and Brown, A G A and Kohley, R and Holland, A}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Wang2018b, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}} \backslashbackslashleqslant M{\_}{\{}\backslashbackslashast{\{}\backslash{\}}{\}} \backslashbackslashleqslant 10{\^{}}{\{}11.9{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashbackslashlangle\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}\backslashbackslashrangle = 2.003 \backslashbackslashpm 0.008{\$} and a standard deviation of {\$}\backslashbackslashsigma{\{}\backslash{\_}{\}}{\{}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}mw{\{}\backslash{\}}{\}}{\}}{\^{}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}-f{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}DM{\{}\backslash{\}}{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -keywords = {cd,elliptical and lenticular,evolution,formation,galaxies,kine-,matics and dynamics,stellar content}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -year = {2018} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M* > 1011M⊙ galaxies at 1 < z < 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 < z < 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V. A. and Dunlop, J. S. and McLure, R. J. and Cirasuolo, M. and Buitrago, F. and Bowler, R. A.A. and Targett, T. A. and Bell, E. F. and McIntosh, D. H. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Hartley, W. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and McGrath, E. J.}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 < z < 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.5221}, -volume = {444}, -year = {2014} -} -@article{Feroz2013, -abstract = {Phlorotannins (PH) derived from brown algae have been shown to have biological effects. However, the application of PH in biomedical materials has not been investigated. Here, we investigated the effects of PH on normal human dermal fibroblast (NHDF) proliferation and fabricated a composite hydrogel consisting PH and poly (vinyl alcohol) (PVA) (PVA/PH) by a freezing-thawing method for wound healing applications. Cell proliferation was significantly higher in the PH-treated (0.01 and 0.02%) cells than in non-treated cells. Based on the mechanical properties, the PVA/PH hydrogel had a significantly increased swelling ratio and ultimate strain compared to the PVA hydrogel, but the ultimate tensile strength and tensile modulus were decreased. Additionally, cell attachment and proliferation on the composites were evaluated using NHDFs. The results showed that after 1 and 5 days, cell attachment and proliferation were significantly increased on the PVA/PH hydrogel compared with that on the PVA hydrogel. The findings from this study suggest that the PVA/PH hydrogel may be a candidate biomedical material for wound healing applications.}, -archivePrefix = {arXiv}, -arxivId = {1306.2144}, -author = {Park, Hyeon Ho and Ko, Seok Chun and Oh, Gun Woo and Heo, Soo Jin and Kang, Do Hyung and Bae, Sung Yong and Jung, Won Kyo}, -doi = {10.1080/09205063.2017.1374030}, -eprint = {1306.2144}, -isbn = {1306.2144}, -issn = {15685624}, -journal = {Journal of Biomaterials Science, Polymer Edition}, -keywords = {Hydrogel,biomedical materials,phlorotannins,poly vinyl alcohol,wound healing}, -month = {jun}, -number = {7-9}, -pages = {972--983}, -pmid = {28853319}, -title = {{Fabrication and characterization of phlorotannins/poly (vinyl alcohol) hydrogel for wound healing application}}, -url = {http://arxiv.org/abs/1306.2144}, -volume = {29}, -year = {2018} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a $\Lambda$CDM concordance cosmology. To that extent we use a large N-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as a function of halo mass and galaxy colour. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by ∼40° (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the colour of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the colour of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion. {\textcopyright}2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X and {Van Den Bosch}, Frank C and Yang, Xiaohu and Mao, Shude and Mo, H J and Li, Cheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@inproceedings{Blandford2001, -abstract = {In order to use a gravitational lens to measure the Hubble constant accurately, it is necessary to derive a reliable model of the lens surface potential. If the analysis is restricted to the locations and magnifications of point images, the derived Hubble constant depends upon the class of mass models used to fit the data. However, when there is extended emission from an Einstein ring, it may be possible to derive a potential from the observed surface brightness in a model-independent manner. This procedure is illustrated with reference to B1608+656. The multi-band images are de-reddened, de-convolved and de-contaminated so that the luminous matter and the surface brightness contours in the Einstein ring are both faithfully mapped. This intensity distribution can then be used to reconstruct the potential. Progress in implementing this program is reported. The observed incidence of multiple-imaged galaxies on the Hubble Deep Fields is an order of magnitude smaller than naively predicted on the basis of radio lens surveys, like CLASS, but consistent with the rate computed using surface photometry of candidate lens galaxies assuming standard mass to light ratios. In order to resolve this paradox, it is suggested that most galaxy lenses are located in compact groups.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0001496}, -author = {Blandford, Roger and Surpi, Gabriela and Kundic, Tomislav}, -booktitle = {Gravitational Lensing: Recent Progress and Future Goals}, -editor = {Brainerd, T.$\sim$G. and Kochanek, C.$\sim$S.}, -eprint = {0001496}, -month = {jan}, -pages = {65}, -primaryClass = {astro-ph}, -series = {Astronomical Society of the Pacific Conference Series}, -title = {{Modeling Galaxy Lenses}}, -url = {http://arxiv.org/abs/astro-ph/0001496}, -volume = {237}, -year = {2000} -} -@article{Ding2016, -abstract = {The empirical correlation between the mass of a supermassive black hole (MBH) and its host galaxy properties is widely considered to be an evidence of their co-evolution. A powerful way to test the co-evolution scenario and learn about the feedback processes linking galaxies and nuclear activity is to measure these correlations as a function of redshift. Unfortunately, currently MBH can only be estimated in active galaxies at cosmological distances. At these distances, bright active galactic nuclei (AGNs) can outshine the host galaxy, making it extremely difficult to measure the host's luminosity. Strongly lensed AGNs provide in principle a great opportunity to improve the sensitivity and accuracy of the host galaxy luminosity measurements as the host galaxy is magnified and more easily separated from the point source, provided the lens model is sufficiently accurate. In order to measure the MBH-L correlation with strong lensing, it is necessary to ensure that the lens modelling is accurate, and that the host galaxy luminosity can be recovered to at least a precision and accuracy better than that of the typical MBH measurement. We carry out extensive and realistic simulations of deep Hubble Space Telescope observations of lensed AGNs obtained by our collaboration. We show that the host galaxy luminosity can be recovered with better accuracy and precision than the typical uncertainty in MBH({\$\sim${}}0.5 dex) for hosts as faint as 2-4 mag dimmer than the AGN itself. Our simulations will be used to estimate bias and uncertainties in the actual measurements to be presented in a future paper.}, -archivePrefix = {arXiv}, -arxivId = {1610.08504}, -author = {Ding, Xuheng and Liao, Kai and Treu, Tommaso and Suyu, Sherry H and Chen, Geoff C F and Auger, Matthew W and Marshall, Philip J and Agnello, Adriano and Courbin, Frederic and Nierenberg, Anna M and Rusu, Cristian E and Sluse, Dominique and Sonnenfeld, Alessandro and Wong, Kenneth C}, -doi = {10.1093/mnras/stw3078}, -eprint = {1610.08504}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: evolution}, -number = {4}, -pages = {4634--4649}, -title = {{H0LiCOW. VI. Testing the fidelity of lensed quasar host galaxy reconstruction}}, -url = {http://arxiv.org/abs/1610.08504}, -volume = {465}, -year = {2017} -} -@article{Brooks2015a, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disk galaxies. Under this bulge-formation model, though, the high rates of mergers in Cold Dark Matter galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disk galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Deason2011, -abstract = {We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the gimic suite of simulations. gimic consists of resimulations of five cosmologically representative regions from the Millennium Simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r∼ 0.1r200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r∼r200). Misalignments of {\textgreater}45° are seen in ∼30 per cent of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20 per cent of the satellite systems with 10 bright galaxies within r200 exhibit a polar spatial alignment with respect to the galaxy - an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction (∼10 per cent) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z= 0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation - the memory of their accretion history can remain intact to z= 0. Understanding the phase-space distribution of the z= 0 satellite population is key for studies that estimate the host halo mass from the line-of-sight velocities and projected positions of satellite galaxies. We quantify the effects of such systematics in estimates of the host halo mass from the satellite population. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A J and Mccarthy, I G and Font, A S and Evans, N W and Frenk, C S and Belokurov, V and Libeskind, N I and Crain, R A and Theuns, T}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Jin2017, -abstract = {We report the results from a recent 133 ks XMM-Newton observation of a highly super- Eddington narrow-line Type-1 quasi-stellar object RX J0439.6-5311. This source has one of the steepest active galactic nuclei hard X-ray slopes, in addition to a prominent and smooth soft X-ray excess. Strong variations are found throughout the 0.3-10 keV energy range on all time-scales covered by the observation, with the soft excess mainly showing low-frequency (LF) variations below 0.1 mHz while the hard X-rays show stronger variability at higher frequencies. We perform a full set of spectral-timing analysis on the X-ray data, including a simultaneous modelling of the time-averaged spectra, frequency-dependent root-mean-square and covariance spectra, lag-frequency and lag-energy spectra. Especially, we find a significant time-lag signal in the LF band, which indicates that the soft X-rays lead the hard by $\sim$4 ks, with a broad continuum-like profile in the lag spectrum. Our analysis strongly supports the model where the soft X-ray excess is dominated by a separate low temperature, optically thick Comptonization component rather than relativistic reflection or a jet. This soft X-ray emitting region is several tens or hundreds of Rg away from the hot corona emitting hard X-rays, and is probably associated with a geometrically thick ('puffed-up') inner disc region.}, -archivePrefix = {arXiv}, -arxivId = {1703.07118}, -author = {Jin, Chichuan and Done, Chris and Ward, Martin}, -doi = {10.1093/mnras/stx718}, -eprint = {1703.07118}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Jin, Done, Ward - 2017 - Super-Eddington QSO RX J0439.6-5311 - I. Origin of the soft X-ray excess and structure of the inner accretion f.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Accretion,Accretion discs,Galaxies: active,Galaxies: nuclei}, -number = {3}, -pages = {3663--3681}, -title = {{Super-Eddington QSO RX J0439.6-5311 - I. Origin of the soft X-ray excess and structure of the inner accretion flow}}, -url = {http://arxiv.org/abs/1703.07118%0Ahttp://dx.doi.org/10.1093/mnras/stx718}, -volume = {468}, -year = {2017} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the foreground lenses and background sources are early-type galaxies. Using imaging from Hubble Space Telescope (HST)/Advanced Camera for Studies (ACS) andKeck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population ofmassive, compact galaxies at redshifts 0.4 ≲ z ≲ 0.7, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of highredshift red nuggets or their partly evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar populations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S{\'{e}}rsic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still compact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterized by red-to-blue colour gradients as a function of radius which are stronger at low redshift - indicative of ongoing accretion - but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are pre-dominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W and Fassnacht, Christopher D and Treu, Tommaso and Brewer, Brendon J and Koopmans, L V E and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Hainline2011, -abstract = {We present a new study of stellar mass in a sample of ∼70 submillimeter-selected galaxies (SMGs) with accurate spectroscopic redshifts. We fit combinations of stellar population synthesis models and power laws to the galaxies' observed-frame optical through mid-IR spectral energy distributions (SEDs) to separate stellar emission from non-stellar near-IR continuum. The availability of spectroscopic redshifts significantly enhances our ability to determine unambiguously not only the mass and luminosity of SMGs, but also the presence and contribution of non-stellar emission to their SEDs. By separating the stellar emission from the non-stellar near-IR continuum, we find that ∼50% of our sample have non-stellar contributions of less than ∼10% in rest-frame H band and 10% of our sample have non-stellar contributions greater than 50%. We find that the K-band luminosity of the non-stellar continuum emission is correlated with hard X-ray luminosity, indicating an active galactic nucleus (AGN) origin of the emission. Upon subtracting this AGN-contributed continuum component from all of the galaxies in our sample, we determine a lower median stellar mass for SMGs than previous studies, ∼7 × 10 10 M ⊙. We use constraints of the starburst timescale from molecular gas studies to estimate the amount of fading our sample would undergo if they passively evolve after the starburst terminates. The results suggest that typical SMGs, while among the most massive galaxies at z ∼ 2, are likely to produce descendants of similar mass and luminosity to L* galaxies in the local universe. {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1006.0238}, -author = {Hainline, Laura J. and Blain, A. W. and Smail, Ian and Alexander, D. M. and Armus, L. and Chapman, S. C. and Ivison, R. J.}, -doi = {10.1088/0004-637X/740/2/96}, -eprint = {1006.0238}, -isbn = {0269-249X}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: high-redshift,infrared: galaxies}, -number = {2}, -pages = {96}, -title = {{The stellar mass content of submillimeter-selected galaxies}}, -url = {http://iopscience.iop.org/0004-637X/740/2/96/article/}, -volume = {740}, -year = {2011} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and S{\'{e}}rsic index distributions obtained from two-dimensional structural fits to 40, 000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of S{\'{e}}rsic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. {\textcopyright} 2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G. and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Chevance et al. - 2012 - On the shapes and structures of high-redshift compact galaxies.pdf:pdf}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Cabanac2007, -abstract = {Aims. We present data from the CFHTLS Strong Lensing Legacy Survey (SL2S). Due to the unsurpassed combined depth, area and image quality of the Canada-France-Hawaii Legacy Survey it is becoming possible to uncover a large, statistically well-defined sample of strong gravitational lenses which spans the dark halo mass spectrum predicted by the concordance model from galaxy to cluster haloes. Methods. We describe the development of several automated procedures to find strong lenses of various mass regimes in CFHTLS images. Results. The preliminary sample of about 40 strong lensing candidates discovered in the CFHTLS T0002 release, covering an effective field of view of 28 deg 2 is presented. These strong lensing systems were discovered using an automated search and consist mainly of gravitational arc systems with splitting angles between 2 and 15 arcsec. This sample shows for the first time that it is possible to uncover a large population of strong lenses from galaxy groups with typical halo masses of about 1013 h-1 M⊙. We discuss the future evolution of the SL2S project and its main scientific aims for the next 3 years, in particular our observational strategy to extract the hundreds of gravitational rings also present in these fields. {\textcopyright} ESO 2007.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0610362}, -author = {Cabanac, R. A. and Alard, C. and Dantel-Fort, M. and Fort, B. and Gavazzi, R. and Gomez, P. and Kneib, J. P. and {Le F{\`{e}}vre}, O. and Mellier, Y. and Pello, R. and Soucail, G. and Sygnet, J. F. and Valls-Gabaud, D.}, -doi = {10.1051/0004-6361:20065810}, -eprint = {0610362}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {Cosmology: dark matter,Galaxies: clusters: general,Galaxies: fundamental parameters,Galaxies: halos,Gravitational lensing,Surveys}, -month = {jan}, -number = {3}, -pages = {813--821}, -primaryClass = {astro-ph}, -title = {{The CFHTLS strong lensing legacy survey I. Survey overview and T0002 release sample}}, -url = {http://arxiv.org/abs/astro-ph/0610362%0Ahttp://dx.doi.org/10.1051/0004-6361:20065810}, -volume = {461}, -year = {2007} -} -@article{Velliscig2015, -abstract = {We report the alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE (Evolution and Assembly of GaLaxies and their Environments) and cosmo-OWLS(Over- Whelmingly Large Simulations) simulations. The combination of these state-of-the-art hydrodynamical cosmological simulations enables us to span four orders of magnitude in halo mass (11 ≤ log10(M200/[h-1M⊙]) ≤ 15), a wide radial range (-2.3 ≤ log10(r/[h-1 Mpc]) ≤ 1.3) and redshifts 0 ≤ z ≤ 1. The shape parameters of the dark matter, stellar and hot gas distributions follow qualitatively similar trends: they become more aspherical (and triaxial) with increasing halo mass, radius, and redshift. We measure the misalignment of the baryonic components (hot gas and stars) of galaxies with their host halo as a function of halo mass, radius, redshift, and galaxy type (centrals versus satellites and early- versus late-type). Overall, galaxies align well with the local distribution of the total (mostly dark) matter. However, the stellar distributions on galactic scales exhibit a median misalignment of about 45-50 deg with respect to their host haloes. This misalignment is reduced to 25-30 deg in the most massive haloes (13 ≤ log10(M200/[h-1M⊙]) ≤ 15). Half of the disc galaxies in the EAGLE simulations have a misalignment angle with respect to their host haloes larger than 40 deg. We present fitting functions and tabulated values for the probability distribution of galaxy-halo misalignment to enable a straightforward inclusion of our results into models of galaxy formations based on purely collisionless N-body simulations.}, -archivePrefix = {arXiv}, -arxivId = {1504.04025}, -author = {Velliscig, Marco and Cacciato, Marcello and Schaye, Joop and Crain, Robert A. and Bower, Richard G. and {Van Daalen}, Marcel P. and Vecchia, Claudio Dalla and Frenk, Carlos S. and Furlong, Michelle and McCarthy, I. G. and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stv1690}, -eprint = {1504.04025}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: Theory,Galaxies: Formation,Galaxies: Haloes,Large-scale structure of Universe}, -month = {oct}, -number = {1}, -pages = {721--738}, -title = {{The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations}}, -volume = {453}, -year = {2015} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of Super-Massive Black Hole (SMBH) formation and evolution is used, as in Tremmel et al.(2015, 2016), allowing to explicitly follow SMBH dynamics at the center of galaxies. A high SIDM constant cross-section is chosen, {\$}\backslashsigma{\$}=10 {\$}\backslashrm cm{\^{}}2/gr{\$}, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in CDM, with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80{\$}\backslash{\%}{\$} of the SMBH population is off-centered in the SIDM case, as opposed to the CDM case in which {\$}\backslashsim{\$}90{\$}\backslash{\%}{\$} of SMBHs have reached their host's centre. SMBHs are found as far as {\$}\backslashsim{\$}9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction timescale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in 'core stalling'. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@article{Spavone2017, -abstract = {{\textcopyright}2017 ESO. Observations of diffuse starlight in the outskirts of galaxies are thought to be a fundamental source of constraint on the cosmological context of galaxy assembly in the {\$}\Lambda{\$}CDM model. Such observations are not trivial because of the extreme faintness of such regions. In this work, we investigated the photometric properties of six massive early-type galaxies (ETGs) in the VEGAS sample (NGC 1399, NGC 3923, NGC 4365, NGC 4472, NGC 5044, and NGC 5846) out to extremely low surface brightness levels with the goal of characterizing the global structure of their light profiles for comparison to state-of-the-art galaxy formation models. We carried out deep and detailed photometric mapping of our ETG sample taking advantage of deep imaging with VST/OmegaCAM in the g and i bands. By fitting the light profiles, and comparing the results to simulations of elliptical galaxy assembly, we have identified signatures of a transition between relaxed and unrelaxed accreted components and can constrain the balance between in situ and accreted stars. The very good agreement of our results with predictions from theoretical simulations demonstrates that the full VEGAS sample of {\$\sim${}}100 ETGs will allow us to use the distribution of diffuse light as a robust statistical probe of the hierarchical assembly of massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1703.10835}, -author = {Spavone, Marilena and Capaccioli, Massimo and Napolitano, Nicola R and Iodice, Enrichetta and Grado, Aniello and Limatola, Luca and Cooper, Andrew P and Cantiello, Michele and Forbes, Duncan A and Paolillo, Maurizio and Schipani, Pietro}, -doi = {10.1051/0004-6361/201629111}, -eprint = {1703.10835}, -issn = {0004-6361}, -journal = {Astronomy {\&} Astrophysics}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: halos,Techniques: image processing,cD}, -number = {3}, -pages = {A38}, -title = {{VEGAS: A VST Early-type GAlaxy Survey}}, -url = {http://www.aanda.org/10.1051/0004-6361/201629111}, -volume = {603}, -year = {2017} -} -@article{James2018, -abstract = {We present the first spatially resolved rest-frame ultraviolet (UV) study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z = 2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each $\sim$4-8 kpc2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with C III] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. Themapped C III] emission shows distinct kinematical structure, with velocity offsets of $\sim$±50 km s-1 between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionization parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing in the range -200 ≲ v (km s-1) ≲ -50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star formation rates remain relatively constant ($\sim$8-16M⊙ yr-1), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced.We measure electron densities with a range of log (Ne)= 3.92-4.36 cm-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large-scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially resolved rest-frame UV studies expected with future observatories, such as James Webb Space Telescope.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L. and Auger, Matt and Pettini, Max and Stark, Daniel P. and Belokurov, V. and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies, in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the SDSS in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on the UV-optical colour {\$}NUV-r{\$}. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings that green valley galaxies have intermediate morphologies, moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of green valley galaxies, we find that they tend to be more massive in the field than in denser environments. On average, green valley galaxies account for {\$}\backslashsim 20\backslash{\%}{\$} of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming low mass galaxies. Green valley galaxies have average star formation histories intermediate between passive and star forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time, and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo > 1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from $\sim$30° to 10° for M $\sim$ 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tenneti et al. - 2014 - Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos and predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of {\$}50{\$} keV {\$}\backslashbackslashlesssim m c{\^{}}2 \backslashbackslashlesssim 345{\$} keV, can be an alternative interpretation of the central compact object in Sgr A*. We present in this work the gravitational lensing properties of this novel DM model in Milky Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the Non-Singular Isothermal Sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, {\$}m c{\^{}}2\backslashbackslashapprox 10{\^{}}{\{}2{\}}{\$} keV, we draw the following conclusions. At distances {\$}r\backslashbackslashgtrsim 20{\$} pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. We show that at distances {\$}\backslashbackslashsim 10{\^{}}{\{}-4{\}}{\$} pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances {\$}r\backslashbackslashlesssim 10{\^{}}{\{}-6{\}}{\$} pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used. We find that quantum DM cores do not show a photon sphere what implies that they do not cast a shadow. Similar conclusions apply to the other DM distributions for other fermion masses in the above specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Greene2013, -abstract = {We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions $\sigma$* ≳ 150 km s-1. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼ 10 Gyr), relatively metal-poor ([Fe/H] ≈ -0.5), and $\alpha$-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z ≈ 1.5-2). {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1308.2682}, -author = {Greene, Jenny E and Murphy, Jeremy D and Graves, Genevieve J and Gunn, James E and Raskutti, Sudhir and Comerford, Julia M and Gebhardt, Karl}, -doi = {10.1088/0004-637X/776/2/64}, -eprint = {1308.2682}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: abundances,galaxies: elliptical and lenticular,galaxies: evolution}, -number = {2}, -title = {{The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius}}, -volume = {776}, -year = {2013} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Spavone2017, -abstract = {Observations of diffuse starlight in the outskirts of galaxies are thought to be a fundamental source of constraint on the cosmological context of galaxy assembly in the $\Lambda$CDM model. Such observations are not trivial because of the extreme faintness of such regions. In this work, we investigated the photometric properties of six massive early-type galaxies (ETGs) in the VEGAS sample (NGC 1399, NGC 3923, NGC 4365, NGC 4472, NGC 5044, and NGC 5846) out to extremely low surface brightness levels with the goal of characterizing the global structure of their light profiles for comparison to state-of-the-art galaxy formation models. We carried out deep and detailed photometric mapping of our ETG sample taking advantage of deep imaging with VST/OmegaCAM in the g and i bands. By fitting the light profiles, and comparing the results to simulations of elliptical galaxy assembly, we have identified signatures of a transition between relaxed and unrelaxed accreted components and can constrain the balance between in situ and accreted stars. The very good agreement of our results with predictions from theoretical simulations demonstrates that the full VEGAS sample of {\$\sim${}}100 ETGs will allow us to use the distribution of diffuse light as a robust statistical probe of the hierarchical assembly of massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1703.10835}, -author = {Spavone, Marilena and Capaccioli, Massimo and Napolitano, Nicola R and Iodice, Enrichetta and Grado, Aniello and Limatola, Luca and Cooper, Andrew P and Cantiello, Michele and Forbes, Duncan A and Paolillo, Maurizio and Schipani, Pietro}, -doi = {10.1051/0004-6361/201629111}, -eprint = {1703.10835}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: halos,Techniques: image processing,cD}, -number = {3}, -pages = {A38}, -title = {{VEGAS: A VST Early-type GAlaxy Survey: II. Photometric study of giant ellipticals and their stellar halos}}, -url = {http://www.aanda.org/10.1051/0004-6361/201629111}, -volume = {603}, -year = {2017} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of supermassive black hole (SMBH) formation and evolution is used, as in Tremmel et al., allowing us to explicitly follow the SMBH dynamics at the centre of galaxies. A high SIDM constant cross-section is chosen, $\sigma$ = 10 cm2gr-1, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in cold dark matter (CDM), with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals, the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80 per cent of the SMBH population is offcentred in the SIDM case, as opposed to the CDM case in which {\$\sim${}}90 per cent of SMBHs have reached their host's centre. SMBHs are found as far as {\$\sim${}}9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction time-scale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in core stalling. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to the SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@article{Xie2018, -abstract = {We study the formation and evolution of brightest cluster galaxies starting from a z = 2 population of quiescent ellipticals and following them to z = 0. To this end, we use a suite of nine high-resolution dark matter only simulations of galaxy clusters in a $\lambda$ cold dark matter ($\lambda$CDM)universe.We develop a scheme inwhich simulation particles are weighted to generate realistic and dynamically stable stellar density profiles at z = 2. Our initial conditions assign a stellar mass to every identified dark halo as expected from abundance matching; assuming that there exists a one-to-one relation between the visible properties of galaxies and their host haloes. We setthe sizes of the luminous components according to the observed relations for z $\sim$ 2 massive quiescent galaxies. We study the evolution of the mass-sizerelation, the fate of satellite galaxies and the mass aggregation of the cluster central. From z = 2, these galaxies grow on average in size by a factor of 5 to 10 and in galaxy mass by 2 to 3. The stellar mass of our simulated BCGs grow by a factor of $\sim$2.1 in the range 0.3 < z < 1.0, consistent with observations, and by a factor of $\sim$1.4 in the range 0.0 < z<0.3. Furthermore, the non-central galaxies evolve on to the present-day mass-size relation by z = 0. Assuming passively evolving stellar populations, we present surface brightness profiles for our cluster centrals which resemble those observed for the cDs in similar mass clusters both at z = 0 and at z = 1. This demonstrates that the $\lambda$CDM cosmology does indeed predict minor and major mergers to occur in galaxy clusters with the frequency and mass ratio distribution required to explain the observed growth in size of passive galaxies since z = 2. Our experiment shows that brightest cluster galaxies could, inprinciple, form through dissipationless mergers of quiescent massive z = 2 galaxies, without substantial additional star formation. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1301.5319}, -author = {Laporte, Chervin F.P. and White, Simon D.M. and Naab, Thorsten and Gao, Liang}, -doi = {10.1093/mnras/stt912}, -eprint = {1301.5319}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Laporte et al. - 2013 - The growth in size and mass of cluster galaxies since z = 2.pdf:pdf}, -isbn = {9781450301992}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Clusters: General,Galaxies,Galaxies: Elliptical and lenticular: cD,Galaxies: Evolution,Galaxies: Formation}, -number = {2}, -pages = {901--909}, -title = {{The growth in size and mass of cluster galaxies since z = 2}}, -volume = {435}, -year = {2013} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ {\textgreater} 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright}2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -volume = {786}, -year = {2014} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series that re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science data base, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies. This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution that limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ('encounter-driven') rings (such as ring and polar ring galaxies) are recognized in less than 1 per cent of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J.}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buta - 2017 - Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database(2).pdf:pdf}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{Gaitskell2004, -abstract = {This article is a brief overview of the status of direct detection experiments of the dark matter, especially searching for WIMPs (Weakly Interacting Massive Particles) at deep underground laboratory, when it was discussed at 37th international conference on high energy physics (ICHEP2018) in Seoul, Korea.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1410.0601v1}, -author = {Lee, Hyun Su}, -doi = {10.1201/b17323-11}, -eprint = {arXiv:1410.0601v1}, -isbn = {{\textless}null{\textgreater}}, -issn = {18248039}, -journal = {Proceedings of Science}, -keywords = {95.30.Cq,95.35.+d,98.62.Gq,SUSY,WIMPs,axions,cold dark matter,dark matter halo}, -month = {dec}, -number = {1}, -pages = {159--178}, -title = {{Direct detection of dark matter}}, -url = {http://www.annualreviews.org/doi/10.1146/annurev.nucl.54.070103.181244}, -volume = {340}, -year = {2018} -} -@article{Oman2017, -abstract = {We use mock interferometric HI measurements and a conventional tilted-ring modelling procedure to estimate circular velocity curves of dwarf galaxy discs from the APOSTLE suite of $\Lambda$ cold dark matter cosmological hydrodynamical simulations. The modelling yields a large diversity of rotation curves for an individual galaxy at fixed inclination, depending on the lineof- sight orientation. The diversity is driven by non-circular motions in the gas; in particular, by strong bisymmetric fluctuations in the azimuthal velocities that the tilted-ring model is ill-suited to account for and that are difficult to detect in model residuals. Large misestimates of the circular velocity arise when the kinematic major axis coincides with the extrema of the fluctuation pattern, in some cases mimicking the presence of kiloparsec-scale density 'cores', when none are actually present. The thickness of APOSTLE discs compounds this effect:more slowly rotating extra-planar gas systematically reduces the average line-of-sight speeds. The recovered rotation curves thus tend to underestimate the true circular velocity of APOSTLE galaxies in the inner regions. Non-circular motions provide an appealing explanation for the large apparent cores observed in galaxies such as DDO 47 and DDO 87, where the model residuals suggest that such motions might have affected estimates of the inner circular velocities. Although residuals from tilted-ring models in the simulations appear larger than in observed galaxies, our results suggest that non-circular motions should be carefully taken into account when considering the evidence for dark matter cores in individual galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1706.07478}, -author = {Oman, Kyle A. and Marasco, Antonino and Navarro, Julio F. and Frenk, Carlos S. and Schaye, Joop and Ben{\'{i}}tez-Llambay, Alejandro}, -doi = {10.1093/mnras/sty2687}, -eprint = {1706.07478}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oman et al. - 2019 - Non-circular motions and the diversity of dwarf galaxy rotation curves.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,ISM: kinematics and dynamics}, -number = {1}, -pages = {821--847}, -title = {{Non-circular motions and the diversity of dwarf galaxy rotation curves}}, -url = {http://arxiv.org/abs/1706.07478}, -volume = {482}, -year = {2019} -} -@article{Handley2015, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, $M_{BH}$, that had been imaged at $3.6\sim\mu m$ with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between $M_{ BH}$ and the host spheroid (and galaxy) luminosity, $L_{sph}$ (and $L_{gal}$), and also stellar mass, $M_{*,sph}$. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have $M_{BH} < 10^7\simM_\odot$, and allows us to better investigate the poorly studied low-mass end of the $M_{BH} - M_{*,sph}$ correlation. The bulges of early-type galaxies follow $M_{BH} \propto M_{*,sph}^{1.04 \pm 0.10}$ and define a tight red sequence with intrinsic scatter $\epsilon = 0.43 \pm 0.06\simdex$ and a median $M_{BH}/M_{*,sph}$ ratio of $0.68 \pm 0.04\%$, i.e.$\sim$a $\pm 2\sigma$ range of 0.1-5%. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with $M_{BH} \propto M_{*,sph}^{2-3}$, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index $n<2$, argued by some to be pseudo-bulges, are not offset to lower $M_{BH}$ from the correlation defined by the current bulge sample with $n>2$; and iii) $L_{sph}$ and $L_{gal}$ correlate equally well with $M_{BH}$, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with $L_{ sph}$ is better than that with $L_{gal}$.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A. D. and Graham, Alister W. and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Savorgnan et al. - 2016 - Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M ,Sph Diagr(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as ‘notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude (≤50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 ≤ G ≤ 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G M and Prod'homme, T and Murray, N J and Crowley, C and Hopkinson, G and Brown, A G A and Kohley, R and Holland, A}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Mendez-Abreu2016, -abstract = {We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area data release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log (M∗/MȮ) > 11), the galaxy population is dominated by galaxies modelled with a single S{\'{e}}rsic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T > 0.2. At intermediate masses (9.5 < log (M∗/MȮ) < 11), galaxies described with bulge+disc but B/T < 0.2 are preponderant, whereas, at the low mass end (log (M∗/MȮ) < 9.5), the prevailing population is constituted by galaxies modelled with either purediscs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57% of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5 < log (M∗/MȮ) < 11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62%, 28%, and 10% for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.}, -archivePrefix = {arXiv}, -arxivId = {1610.05324}, -author = {M{\'{e}}ndez-Abreu, J. and Ruiz-Lara, T. and S{\'{a}}nchez-Menguiano, L. and {De Lorenzo-C{\'{a}}ceres}, A. and Costantin, L. and Catal{\'{a}}n-Torrecilla, C. and Florido, E. and Aguerri, J. A.L. and Bland-Hawthorn, J. and Corsini, E. M. and Dettmar, R. J. and Galbany, L. and Garc{\'{i}}a-Benito, R. and Marino, R. A. and M{\'{a}}rquez, I. and Ortega-Minakata, R. A. and Papaderos, P. and S{\'{a}}nchez, S. F. and S{\'{a}}nchez-Blazquez, P. and Spekkens, K. and {Van De Ven}, G. and Wild, V. and Ziegler, B.}, -doi = {10.1051/0004-6361/201629525}, -eprint = {1610.05324}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/M{\'{e}}ndez-Abreu et al. - 2017 - Two-dimensional multi-component photometric decomposition of CALIFA galaxies(2).pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -title = {{Two-dimensional multi-component photometric decomposition of CALIFA galaxies}}, -url = {http://arxiv.org/abs/1610.05324%0Ahttp://dx.doi.org/10.1051/0004-6361/201629525}, -volume = {598}, -year = {2017} -} -@inproceedings{MartinNavarro2013, -author = {Mart$\backslash$'$\backslash$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kilo parsecs. These stellar halos provide a fossil record of galaxy assembly histories. Using data that is both wide ({\$\sim${}}100 square degree) and deep (i{\textgreater}28.5 mag/arcsec{\^{}}2 in i-band), we present a systematic study of the stellar halos of a sample of more than 3000 galaxies at 0.3 {\textless} z {\textless} 0.5 with {\$}\backslashlog M{\_}{\{}\backslashstar{\}}/M{\_}{\{}\backslashodot{\}} {\textgreater} 11.4{\$}. Our study is based on high-quality (0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP), which enables us to individually estimate surface mass density profiles to 100 kpc without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles. When this extended light is not properly accounted for as a result of shallow imaging or inadequate profile modeling, the derived stellar mass function can be significantly underestimated at the highest masses. Across our sample, the ellipticity of outer light profiles increases substantially as we probe larger radii. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass-dependence in outer color gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at late times from a series of merging events. We provide surface mass surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Bellstedt2018, -abstract = {We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 1010 {\textless} M*/M⊙ {\textless} 1011.6 that cover a large radial range of 0.1-4.0 effective radii.We combine SLUGGS and ATLAS3D data sets to model the total-mass profiles of a sample of 21 fast-rotator galaxies, utilizing a hyperparameter method to combine the two independent data sets. The total-mass density profile slope values derived for these galaxies are consistent with those measured in the inner regions of galaxies by other studies. Furthermore, the total-mass density slopes ($\gamma$tot) appear to be universal over this broad stellar mass range, with an average value of $\gamma$tot= -2.24± 0.05, i.e. slightly steeper than isothermal. We compare our results to model galaxies from the Magneticum and EAGLE cosmological hydrodynamic simulations, in order to probe the mechanisms that are responsible for varying total-mass density profile slopes. The simulated-galaxy slopes are shallower than the observed values by {\$\sim${}}0.3-0.5, indicating that the physical processes shaping the mass distributions of galaxies in cosmological simulations are still incomplete. For galaxies with M* {\textgreater} 1010.7M⊙ in the Magneticum simulations, we identify a significant anticorrelation between total-mass density profile slopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas this anticorrelation is weaker for lower stellar masses, implying that the measured total-mass density slopes for low-mass galaxies are less likely to be determined by merger activity.}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A and Romanowsky, Aaron J and Remus, Rhea Silvia and Stevens, Adam R H and Brodie, Jean P and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to {\$\sim${}}4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Papadopoulos2013, -abstract = {Not Available}, -archivePrefix = {arXiv}, -arxivId = {1207.2048}, -author = {Fukui, Yasuo}, -doi = {10.1007/978-3-642-35410-6}, -eprint = {1207.2048}, -isbn = {978-3-642-35409-0}, -journal = {Molecular and Atomic Gas in the Young TeV gamma-Ray SNRs RX J1713.7-3946 and RX J0852.0-4622; Evidence for the Hadronic Rroduction of gamma-Rays}, -pages = {21}, -title = {{Cosmic Rays in Star-Forming Environments}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2013ASSP...34.....T&link_type=EJOURNAL%5Cnpapers2://publication/doi/10.1007/978-3-642-35410-6}, -volume = {34}, -year = {2013} -} -@article{Milosavljevic2001, -abstract = {We investigate a model in which galactic nuclei form via the coalescence of pre-existing stellar systems containing supermassive black holes. Merger simulations are carried out using N-body algorithms that can follow the formation and decay of a black-hole binary and its effect on the surrounding stars down to sub-parsec scales. Our initial stellar systems have steep central density cusps similar to those in low-luminosity elliptical galaxies. Formation of a black-hole binary transfers energy to the stars and lowers the central density; continued decay of the binary creates a $\sim$1/r density cusp similar to those observed in bright elliptical galaxies, with a break radius that extends well beyond the sphere of gravitational influence of the black holes. The decay of the black hole binary is followed over a factor of $\sim$20 in separation after formation of a hard binary, considerably farther than in previous simulations. We see almost no dependence of the binary's decay rate on number of particles in the simulation, contrary to earlier studies in which a lower initial density of stars led to a more rapid depletion of the binary's loss cone. We nevertheless argue that the decay of a black hole binary in a real galaxy would be expected to stall at separations of 0.01-1 pc unless some additional mechanism is able to extract energy from the binary. Our results support a picture in which the observed dependence of nuclear cusp slope on galaxy luminosity is a consequence of galaxy interactions. We also discuss the implications of our results for the survivability of dark-matter cusps.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103350}, -author = {Milosavljevi{\'{c}}, Milo{\v{s}} and Merritt, David}, -doi = {10.1086/323830}, -eprint = {0103350}, -isbn = {1476-4687 (Electronic)\n0028-0836 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Black Hole Physics,Galaxies: Nuclei,Stellar Dynamics}, -month = {dec}, -number = {1}, -pages = {34--62}, -pmid = {20123743}, -primaryClass = {astro-ph}, -title = {{Formation of Galactic Nuclei}}, -url = {http://arxiv.org/abs/astro-ph/0103350%0Ahttp://dx.doi.org/10.1086/323830}, -volume = {563}, -year = {2001} -} -@article{Tenneti2016, -abstract = {We study the shapes and intrinsic alignments of disks and elliptical galaxies in the MassiveBlack-II (MBII) and Illustris cosmological hydrodynamic simulations, with volumes of {\$}(100h{\^{}}{\{}-1{\}}Mpc){\^{}}{\{}3{\}}{\$} and {\$}(75h{\^{}}{\{}-1{\}}Mpc){\^{}}{\{}3{\}}{\$} respectively. We find that simulated disk galaxies are more oblate in shape and more misaligned with the shape of their host dark matter subhalo when compared with ellipticals. The disk major axis is found to be oriented towards the location of nearby elliptical galaxies. We also find that the disks are thinner in MBII and misalignments with dark matter halo orientations are smaller in both disks and ellipticals when compared with Illustris. As a result, the intrinsic alignment correlation functions at fixed mass have a higher amplitude in MBII than in Illustris. Finally, at scales above {\$}\backslashsim 0.1{\$}$\backslash$hmpc, the intrinsic alignment two-point correlation functions for disk galaxies in both simulations are consistent with a null detection, unlike those for ellipticals. Despite significant differences in the treatments of hydrodynamics and baryonic physics in the simulations, we find that the {\$}w{\_}{\{}\backslashdelta +{\}}{\$} correlation function scales similarly with transverse separation. However, the less massive galaxies show different scale dependence in the ED correlation. This result indicates that, while hydrodynamic simulations are a promising tool to study intrinsic alignments, further study is needed to understand the impact of differences in the implementations of hydrodynamics and baryonic feedback.}, -archivePrefix = {arXiv}, -arxivId = {1510.07024}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana}, -doi = {10.1093/mnras/stw1823}, -eprint = {1510.07024}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies,Gravitational lensing: weak,Hydrodynamics,Kinematics and dynamics,Methods,Numerical}, -number = {3}, -pages = {2668--2680}, -title = {{Intrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris simulations}}, -volume = {462}, -year = {2016} -} -@article{Sonnenfeld2013b, -abstract = {We present Hubble Space Telescope (HST) imaging data and Canada-France-Hawaii Telescope (CFHT) near-infrared ground-based images for the final sample of 56 candidate galaxy-scale lenses uncovered in the CFHT Legacy Survey as part of the Strong Lensing in the Legacy Survey project. The new images are used to perform lens modeling, measure surface photometry, and estimate stellar masses of the deflector early-type galaxies (ETGs). Lens modeling is performed on the HST images (or CFHT when HST is not available) by fitting the spatially extended light distribution of the lensed features assuming a singular isothermal ellipsoid mass profile and by reconstructing the intrinsic source light distribution on a pixelized grid. Based on the analysis of systematic uncertainties and comparison with inference based on different methods, we estimate that our Einstein radii are accurate to ∼3%. HST imaging provides a much higher success rate in confirming gravitational lenses and measuring their Einstein radii than CFHT imaging does. Lens modeling with ground-based images, however, when successful, yields Einstein radius measurements that are competitive with space-based images. Information from the lens models is used together with spectroscopic information from companion Paper IV to classify the systems, resulting in a final sample of 39 confirmed (grade A) lenses and 17 promising candidates (grade B,C). This represents an increase of half an order of magnitude in sample size with respect to the sample of confirmed lenses studied in Papers I and II. The Einstein radii of the confirmed lenses in our sample span the range 5-15 kpc and are typically larger than those of other surveys, probing the mass in regions where the dark matter contribution is more important. Stellar masses are in the range 10 11-1012 M {\textperiodcentered}, covering the range of massive ETGs. The redshifts of the main deflector span a range 0.3 ≤ z d ≤ 0.8, which nicely complements low-redshift samples like the Sloan Lens ACS survey and thus provides an excellent sample for the study of the cosmic evolution of the mass distribution of ETGs over the second half of the history of the universe. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1307.4764}, -author = {Sonnenfeld, Alessandro and Gavazzi, Rapha{\"{e}}l and Suyu, Sherry H. and Treu, Tommaso and Marshall, Philip J.}, -doi = {10.1088/0004-637X/777/2/97}, -eprint = {1307.4764}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,gravitational lensing: strong}, -number = {2}, -pages = {97}, -title = {{The SL2S Galaxy-scale lens sample. III. lens models, surface photometry, and stellar masses for the final sample}}, -url = {http://arxiv.org/abs/1307.4764}, -volume = {777}, -year = {2013} -} -@article{Ellison2017, -abstract = {The tight correlation between total galaxy stellar mass and star formation rate (SFR) has become known as the star forming main sequence. Using {\$\sim${}}487,000 spaxels from galaxies observed as part of the Sloan Digital Sky Survey Mapping Galaxies at Apache Point Observatory (MaNGA) survey, we confirm previous results that a correlation also exists between the surface densities of star formation (Sigma{\_}SFR) and stellar mass (Sigma{\_}mass) on kpc scales, representing a `resolved' main sequence. Using a new metric (Delta Sigma{\_}SFR), which measures the relative enhancement or deficit of star formation on a spaxel-by-spaxel basis relative to the resolved main sequence, we investigate the SFR profiles of 864 galaxies as a function of their position relative to the global star forming main sequence (Delta SFR). For galaxies above the global main sequence (positive Delta SFR) Delta Sigma{\_}SFR is elevated throughout the galaxy, but the greatest enhancement in star formation occurs at small radii ({\textless} 3 kpc, or 0.5 R{\_}e). Moreover, galaxies that are at least a factor of three above the main sequence show diluted gas phase metallicities out to 2 R{\_}e, indicative of metal-poor gas inflows accompanying the starbursts. For quiescent/passive galaxies that lie at least a factor of 10 below the star forming main sequence there is an analogous deficit of star formation throughout the galaxy with the lowest values of Delta Sigma{\_}SFR in the central 3 kpc. Our results are in qualitative agreement with the `compaction' scenario in which a central starburst leads to mass growth in the bulge and may ultimately precede galactic quenching from the inside-out.}, -archivePrefix = {arXiv}, -arxivId = {1711.00915}, -author = {Ellison, Sara L and S{\'{a}}nchez, Sebastian F and Ibarra-Medel, Hector and Antonio, Braulio and Mendel, J Trevor and Barrera-Ballesteros, Jorge}, -doi = {10.1093/mnras/stx2882}, -eprint = {1711.00915}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: interactions,Galaxies: star formation}, -number = {2}, -pages = {2039--2054}, -title = {{Star formation is boosted (and quenched) from the inside-out: Radial star formation profiles from MaNGA}}, -url = {http://arxiv.org/abs/1711.00915}, -volume = {474}, -year = {2018} -} -@article{Gadotti2011, -abstract = {I present results from the modelling of stellar bars in nearly 300 barred galaxies in the local universe through parametric multicomponent multiband image fitting. The surface brightness radial profile of bars is described using a S{\'{e}}rsic function and parameters, such as the bar effective radius, ellipticity, boxiness, length and mass, and bar-to-total luminosity and mass ratios, are determined, which is unprecedented for a sample of this size. The properties of bars in galaxies with classical bulges and pseudo-bulges are compared. For a fixed bar-to-total mass ratio, pseudo-bulges are on average significantly less massive than classical bulges, indicating that, if pseudo-bulges are formed through bars, further processes are necessary to build a classical bulge. I find a correlation between bar ellipticity and boxiness, and define a new parameter as the product of these two quantities. I also find correlations between this product and the normalized bar size, between the sizes of bars and bulges, and between the normalized bar size and bulge-to-total ratio. Bars with different ellipticities follow parallel lines in the latter two correlations. These correlations can arise if, starting off with different normalized sizes and ellipticities, bars grow longer and stronger with dynamical age, as a result of angular momentum exchange between the inner and outer parts of galaxies, consistent with previous theoretical predictions. A plausible consequence is that bar pattern speeds should become lower with bar dynamical age and towards galaxies with more prominent bulges. {\textcopyright}2011 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1003.1719}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2011.18945.x}, -eprint = {1003.1719}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {3308--3318}, -title = {{Secular evolution and structural properties of stellar bars in galaxies}}, -volume = {415}, -year = {2011} -} -@article{2001es, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Xie2014, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stu2487}, -volume = {447}, -year = {2015} -} -@article{Brainerd2005, -abstract = {The distribution of satellite galaxies relative to isolated host galaxies in the Sloan Digital Sky Survey (SDSS) is investigated. Host-satellite systems are selected using three different methods, yielding samples of {\$\sim${}}3300, {\$\sim${}}1600, and {\$\sim${}}950 satellites. In the plane of the sky, the distributions of all three samples show highly significant deviations from circular symmetry ({\textgreater}99.99{\%}, {\textgreater}99.99{\%}, and 99.79{\%} confidence levels, respectively), and the degree of anisotropy is a strong function of the projected radius, r p , at which the satellites are found. For r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 100 kpc, the SDSS satellites are aligned preferentially with the major axes of the hosts. This is in stark contrast to the Holmberg effect, in which satellites are aligned with the minor axes of host galaxies. The degree of anisotropy in the distribution of the SDSS satellites decreases with r p and is consistent with an isotropic distribution at of order the 1 $\sigma$ level for 250 kpc {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 500 kpc.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408559}, -author = {Brainerd, Tereasa G}, -doi = {10.1086/432713}, -eprint = {0408559}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L101----L104}, -primaryClass = {astro-ph}, -title = {{Anisotropic Distribution of SDSS Satellite Galaxies: Planar (Not Polar) Alignment}}, -url = {http://stacks.iop.org/1538-4357/628/i=2/a=L101}, -volume = {628}, -year = {2005} -} -@article{Jullo2010, -abstract = {Current efforts in observational cosmology are focused on characterizing the mass-energy content of the universe. We present results from a geometric test based on strong lensing in galaxy clusters. Based on Hubble Space Telescope images and extensive ground-based spectroscopic follow-up of the massive galaxy cluster Abell 1689, we used a parametric model to simultaneously constrain the cluster mass distribution and dark energy equation of state. Combining our cosmological constraints with those from x-ray clusters and the Wilkinson Microwave Anisotropy Probe 5-year data gives $\Omega$m = 0.25 ±0.05 and Wx = -0.97 ±0.07, which are consistent with results from other methods. Inclusion of our method with all other available techniques brings down the current 2$\sigma$ contours on the dark energy equation-of-state parameter wx by ∼30{\%}.}, -archivePrefix = {arXiv}, -arxivId = {1008.4802}, -author = {Jullo, Eric and Natarajan, Priyamvada and Kneib, Jean Paul and D'Aloisio, Anson and Limousin, Marceau and Richard, Johan and Schimd, Carlo}, -doi = {10.1126/science.1185759}, -eprint = {1008.4802}, -issn = {00368075}, -journal = {Science}, -number = {5994}, -pages = {924--927}, -title = {{Cosmological constraints from strong gravitational lensing in clusters of galaxies}}, -volume = {329}, -year = {2010} -} -@article{Hoekstra2004, -abstract = {We present the results of a study of weak lensing by galaxies based on 45.5 deg{\$}{\^{}}2{\$} of {\$}R{\_}C{\$} band imaging data from the Red-Sequence Cluster Survey (RCS). We present the first weak lensing detection of the flattening of galaxy dark matter halos. We use a simple model in which the ellipticity of the halo is {\$}f{\$} times the observed ellipticity of the lens. We find a best fit value of {\$}f=0.77{\^{}}{\{}+0.18{\}}{\_}{\{}-0.21{\}}{\$}, suggesting that the dark matter halos are somewhat rounder than the light distribution. The fact that we detect a significant flattening implies that the halos are well aligned with the light distribution. Given the average ellipticity of the lenses, this implies a halo ellipticity of {\$}{\textless}e{\_}{\{}\backslashrm halo{\}} {\textgreater}=0.33{\^{}}{\{}+0.07{\}}{\_}{\{}-0.09{\}}{\$}, in fair agreement with results from numerical simulations of CDM. This result provides strong support for the existence of dark matter, as an isotropic lensing signal is excluded with 99.5{\%} confidence. We also study the average mass profile around the lenses, using a maximum likelihood analysis. We consider two models for the halo mass profile: a truncated isothermal sphere (TIS) and an NFW profile. We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo. The best fit NFW model yields a mass {\$}M{\_}{\{}200{\}}=(8.4\backslashpm0.7\backslashpm0.4)\backslashtimes 10{\^{}}{\{}11{\}} h{\^{}}{\{}-1{\}} M{\_}\backslashodot{\$} and a scale radius {\$}r{\_}s=16.2{\^{}}{\{}+3.6{\}}{\_}{\{}-2.9{\}} h{\^{}}{\{}-1{\}}{\$} kpc. This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, H K C and Gladders, Michael D}, -doi = {10.1086/382726}, -eprint = {0306515}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of Galaxy Dark Matter Halos from Weak Lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2004} -} -@article{Rest2001, -author = {Rest, Armin and Bosch, Frank C V A N D E N and Tran, Hien and Tsvetanov, Zlatan and Ford, Holland C and Davies, James and Schafer, Joanna}, -journal = {Database}, -keywords = {cd {\`{e}} galaxies,elliptical and lenticular,galaxies,nuclei {\`{e}} galaxies,structure}, -number = {1995}, -title = {{WFPC2 IMAGES OF THE CENTRAL REGIONS OF EARLY-TYPE GALAXIES . I . THE DATA AND We present high-resolution R-band images of the central regions of 67 early-type galaxies obtained with the Wide Field and Planetary Camera 2 ( WFPC2 ) aboard the Hubble Space T}}, -year = {2001} -} -@article{Goerdt2010, -abstract = {We perform a detailed investigation into the disruption of central cusps via the transfer of energy from sinking massive objects. Constant density inner regions form at the radius where the enclosed mass approximately matches the mass of the infalling body. We explore parameter space using numerical simulations and give an empirical relation for the size of the resulting core within structures that have different initial cusp slopes. We find that infalling bodies always stall at the edge of these newly formed cores, experiencing no dynamical friction over many dynamical times. As applications, we consider the resulting decrease in the dark matter annihilation flux due to centrally destroyed cusps, and we present a new theory for the formation of close binary nuclei-the "stalled binary" model.We focus on one particularly interesting binary nucleus system, the dwarf spheroidal galaxy VCC 128 which is darkmatter dominated at all radii.We showthat its nucleiwould rapidly coalesce within a fewmillion years if it has a central dark matter cusp slope steeper than r-1. However, if its initial dark matter cusp is slightly shallower than a logslope of-0.75 at∼0.1% of the virial radius, then the sinking nuclei naturally create a core equal to their observed separation and stall. This is close to the logslope measured in a recent billion particle cold darkmatter halo simulation. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0806.1951}, -author = {Goerdt, Tobias and Moore, Ben and Read, J. I. and Stadel, Joachim}, -doi = {10.1088/0004-637X/725/2/1707}, -eprint = {0806.1951}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Cosmology: theory,Dark matter,Galaxies: dwarf,Galaxies: individual (VCC 128),Methods: numerical}, -month = {dec}, -number = {2}, -pages = {1707--1716}, -title = {{Core creation in galaxies and halos via sinking massive objects}}, -url = {http://stacks.iop.org/0004-637X/725/i=2/a=1707?key=crossref.f1a39f421687694dc69519d38297f745}, -volume = {725}, -year = {2010} -} -@article{Zehavi2017, -abstract = {We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -- halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto- and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.}, -archivePrefix = {arXiv}, -arxivId = {1706.07871}, -author = {Zehavi, Idit and Contreras, Sergio and Padilla, Nelson and Smith, Nicholas J and Baugh, Carlton M and Norberg, Peder}, -doi = {10.3847/1538-4357/aaa54a}, -eprint = {1706.07871}, -issn = {1538-4357}, -keywords = {clustering,cosmology,evolution,galaxies,halos,large-scale structure of universe,statistics,theory}, -title = {{The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos}}, -url = {http://arxiv.org/abs/1706.07871%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaa54a}, -year = {2017} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos and predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of {\$}50{\$} keV {\$}\backslashlesssim m c{\^{}}2 \backslashlesssim 345{\$} keV, can be an alternative interpretation of the central compact object in Sgr A*. We present in this work the gravitational lensing properties of this novel DM model in Milky Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the Non-Singular Isothermal Sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, {\$}m c{\^{}}2\backslashapprox 10{\^{}}{\{}2{\}}{\$} keV, we draw the following conclusions. At distances {\$}r\backslashgtrsim 20{\$} pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. We show that at distances {\$}\backslashsim 10{\^{}}{\{}-4{\}}{\$} pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances {\$}r\backslashlesssim 10{\^{}}{\{}-6{\}}{\$} pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used. We find that quantum DM cores do not show a photon sphere what implies that they do not cast a shadow. Similar conclusions apply to the other DM distributions for other fermion masses in the above specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Blanton2003, -abstract = {Using photometry and spectroscopy of 144,609 galaxies from the Sloan Digital Sky Survey, we present bivariate distributions of pairs of seven galaxy properties: four optical colors, surface brightness, radial profile shape as measured by the Sersic index, and absolute magnitude. In addition, we present the dependence of local galaxy density (smoothed on 8 h{\^{}}{\{}-1{\}} Mpc scales) on all of these properties. Several classic, well-known relations among galaxy properties are evident at extremely high signal-to-noise ratio: the color-color relations of galaxies, the color-magnitude relations, the magnitude-surface brightness relation, and the dependence of density on color and absolute magnitude. We show that most of the i-band luminosity density in the universe is in the absolute magnitude and surface brightness ranges used. Some of the relationships between parameters, in particular the color--magnitude relations, show stronger correlations for exponential galaxies and concentrated galaxies taken separately than for all galaxies taken together. We provide a simple set of fits of the dependence of galaxy properties on luminosity for these two sets of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0209479}, -author = {Blanton, Michael R and Hogg, David W and Bahcall, Neta A and Baldry, Ivan K and Brinkmann, J and Csabai, Istvan and Eisenstein, Daniel and Fukugita, Masataka and Gunn, James E and Ivezi{\'{c}}, {\v{Z}}eljko and Lamb, D Q and Lupton, Robert H and Loveday, Jon and Munn, Jeffrey A and Nichol, R C and Okamura, Sadanori and Schlegel, David J and Shimasaku, Kazuhiro and Strauss, Michael A and Vogeley, Michael S and Weinberg, David H}, -doi = {10.1086/375528}, -eprint = {0209479}, -isbn = {0004-6256}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Fundamental Parameters,Galaxies: Photometry,Galaxies: Statistics}, -month = {sep}, -number = {1}, -pages = {186--207}, -pmid = {19408790}, -primaryClass = {astro-ph}, -title = {{ The Broadband Optical Properties of Galaxies with Redshifts 0.02 {\textless} z {\textless} 0.22 }}, -url = {http://arxiv.org/abs/astro-ph/0209479%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/375528}, -volume = {594}, -year = {2003} -} -@article{Geometryei, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{VanDerWel2012, -abstract = {We present global structural parameter measurements of 109,533 unique, H F160W-selected objects from the CANDELS multi-cycle treasury program. S{\'{e}}rsic model fits for these objects are produced with GALFIT in all available near-infrared filters (H F160W, J F125W and, for a subset, Y F105W). The parameters of the best-fitting S{\'{e}}rsic models (total magnitude, half-light radius, S{\'{e}}rsic index, axis ratio, and position angle) are made public, along with newly constructed point-spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties, we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements - to 10% or better - of all structural parameters can typically be obtained for galaxies with H F160W < 23, with comparable fidelity for basic size and shape measurements for galaxies to H F160W ∼ 24.5. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1211.6954}, -author = {{Van Der Wel}, A. and Bell, E. F. and H{\"{a}}ussler, B. and McGrath, E. J. and Chang, Yu Yen and Guo, Yicheng and McIntosh, D. H. and Rix, H. W. and Barden, M. and Cheung, E. and Faber, S. M. and Ferguson, H. C. and Galametz, A. and Grogin, N. A. and Hartley, W. and Kartaltepe, J. S. and Kocevski, D. D. and Koekemoer, A. M. and Lotz, J. and Mozena, M. and Peth, M. A. and Peng, Chien Y.}, -doi = {10.1088/0067-0049/203/2/24}, -eprint = {1211.6954}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Van Der Wel et al. - 2012 - Structural parameters of galaxies in candels.pdf:pdf}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: high-redshift,galaxies: statistics,galaxies: structure surveys}, -number = {2}, -title = {{Structural parameters of galaxies in candels}}, -volume = {203}, -year = {2012} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S{\`{e}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as Mh(M*) ∝ reff$\eta$ (M*). We find that, on average, our lens galaxies have an $\eta$ = 0.42 ± 0.12, i.e. larger galaxies live in more massive dark matter haloes. The $\eta$ is strongest for high-mass luminous red galaxies. Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed M*, satellite galaxies have a larger $\eta$ and greater scatter in the Mh and reff relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J L and Hudson, Michael J and Balogh, Michael L and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Emsellem2004, -abstract = {We present the stellar kinematics of 48 representative elliptical and lenticular galaxies obtained with our custom-built integral-field spectrograph SAURON operating on the William Herschel Telescope. The data were homogeneously processed through a dedicated reduction and analysis pipeline. All resulting SAURON data cubes were spatially binned to a constant minimum signal-to-noise ratio. We have measured the stellar kinematics with an optimized (penalized pixel-fitting) routine which fits the spectra in pixel space, via the use of optimal templates, and prevents the presence of emission lines to affect the measurements. We have thus generated maps of the mean stellar velocity V, the velocity dispersion $\sigma$, and the Gauss-Hermite moments h 3 and h 4 of the line-of-sight velocity distributions. The maps extend to approximately one effective radius. Many objects display kinematic twists, kinematically decoupled components, central stellar discs, and other peculiarities, the nature of which will be discussed in future papers of this series.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0404034}, -author = {Emsellem, Eric and Cappellari, Michele and Peletier, Reynier F. and McDermid, Richard M. and Bacon, R. and Bureau, M. and Copin, Y. and Davies, Roger L. and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Miller, Bryan W. and {De Zeeuw}, P. Tim}, -doi = {10.1111/j.1365-2966.2004.07948.x}, -eprint = {0404034}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: bulges,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -month = {aug}, -number = {3}, -pages = {721--743}, -pmid = {235696500003}, -primaryClass = {astro-ph}, -title = {{The SAURON project - III. Integral-field absorption-line kinematics of 48 elliptical and lenticular galaxies}}, -volume = {352}, -year = {2004} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of {\$\sim${}}1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ($M_{*}>10^{10} M_{\odot}$), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at $z\sim2$. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that $39.2^{+3.9}_{-3.6}$\% (65/166) of cSFGs at $1.4 0.5 in the B band. The formation of the galaxy spins up the dark matter within 0.1Rvir such that the specific halo angular momentum increases by ≈50 per cent in the median. The dark matter angular momentum becomes better aligned, but there remains a broad distribution of (mis-)alignments between the halo and the central galaxy, with a median angle between their angular momenta of ∼30°. Galaxies have a range of orientations relative to the shape of the halo: half of them have their minor axes misaligned by more than 45°, although only about 10 per cent of the galaxies lie within 30° of the plane perpendicular to the major axis of their halo. Finally, we align a sample of haloes according to the orientation of their galaxies and stack the projected mass distributions. Although the individual haloes are significantly aspherical, galaxy-halo misalignments produce a stacked mass distribution that cannot be distinguished from circular. If the lack of alignment found in our simulations is realistic, it will be extremely difficult for weak lensing studies to measure the ellipticity of cold dark matter haloes using this technique. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0906.2785}, -author = {Bett, Philip and Eke, Vincent and Frenk, Carlos S. and Jenkins, Adrian and Okamoto, Takashi}, -doi = {10.1111/j.1365-2966.2010.16368.x}, -eprint = {0906.2785}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Methods: N-body simulations}, -month = {may}, -number = {3}, -pages = {1137--1156}, -title = {{The angular momentum of cold dark matter haloes with and without baryons}}, -volume = {404}, -year = {2010} -} -@article{Weinberg2007, -abstract = {A galaxy remains near equilibrium for most of its history. Only through resonances can non-axisymmetric features, such as spiral arms and bars, exert torques over large scales and change the overall structure of the galaxy. In this paper, we describe the resonant interaction mechanism in detail, derive explicit criteria for the particle number required to simulate these dynamical processes accurately using N-body simulations, and illustrate them with numerical experiments. To do this, we perform a direct numerical solution of perturbation theory, in short, by solving for each orbit in an ensemble and make detailed comparisons with N-body simulations. The criteria include: sufficient particle coverage in phase space near the resonance and enough particles to minimize gravitational potential fluctuations that will change the dynamics of the resonant encounter. These criteria are general in concept and can be applied to any dynamical interaction. We use the bar-halo interaction as our primary example owing to its technical simplicity and astronomical ubiquity. Some of our more surprising findings are as follows. First, the inner Lindblad like resonance, responsible for coupling the bar to the central halo cusp, requires more than script O sign (108) equal-mass particles within the virial radius or O(107) inside the bar radius for a Milky Way like bar in a Navarro, Frenk & White profile. Secondly, orbits that linger near the resonance receive more angular momentum than orbits that move through the resonance quickly. Small-scale fluctuations present in state-of-the-art particle-particle simulations can knock orbits out of resonance, preventing them from lingering and, thereby, decrease the torque per orbit. This can be offset by the larger number of orbits affected by the resonance due to the diffusion. However, noise from orbiting substructure remains at least an order of magnitude too small to be of consequence. Applied to N-body simulations, the required particle numbers are sufficiently high for scenarios of interest that apparent convergence in particle number is misleading: the convergence with N may still be in the noise-dominated regime. State-of-the-art simulations are not adequate to follow all aspects of secular evolution driven by the bar-halo interaction. It is not possible to derive particle number requirements that apply to all situations, for example, more subtle interactions may be even more difficult to simulate. Therefore, we present a procedure to test the requirements for individual N-body codes to the actual problem of interest. {\textcopyright} 2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508166}, -author = {Weinberg, Martin D. and Katz, Neal}, -doi = {10.1111/j.1365-2966.2006.11306.x}, -eprint = {0508166}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxy: structure,Stellar dynamics}, -month = {feb}, -number = {2}, -pages = {425--459}, -primaryClass = {astro-ph}, -title = {{The bar-halo interaction - I. From fundamental dynamics to revised N-body requirements}}, -volume = {375}, -year = {2007} -} -@article{Martizzi2013, -abstract = {In a recent study, we used cosmological simulations to show that active galactic nuclei (AGN) feedback on the gas distribution in clusters of galaxies can be important in determining the spatial distribution of stars and dark matter in the central regions of these systems. The hierarchical assembly of dark matter, baryons and black holes obscures the physical mechanism behind the restructuring process. Here, we use idealized simulations to follow the response of a massive dark matter halo as we feed the central black hole with a controlled supply of cold gas. This removes most of the complexity taking place in the cosmological simulations that may have biased our previous study.We confirm our previous results: gas heated and expelled from the central regions of the halo by AGN feedback can return after cooling; repeated cycles generate gravitational potential fluctuations responsible for irreversible modifications of the dark matter mass profile. The main result is the expulsion of large amounts of baryons and dark matter from the central regions of the halo. According to the work presented here, outflowinduced fluctuations represent the only mechanism able to efficiently create dark matter cores in clusters of galaxies. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1211.2648}, -author = {Martizzi, Davide and Teyssier, Romain and Moore, Ben}, -doi = {10.1093/mnras/stt297}, -eprint = {1211.2648}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cosmology: theory,Galaxies: clusters: general,Galaxies: formation,Large-scale structure of universe,Methods: numerical}, -month = {jul}, -number = {3}, -pages = {1947--1954}, -title = {{Cusp-core transformations induced by AGN feedback in the progenitors of cluster galaxies}}, -volume = {432}, -year = {2013} -} -@article{Trujillo2004, -abstract = {We fitted the surface-brightness profiles of 21 elliptical galaxies using both the Sersic function and a new empirical model that combines an inner power law with an outer S√{\textcopyright}rsic function. The profiles are combinations of deconvolved Hubble Space Telescope (HST) profiles from the literature and ellipse fits to the full WFPC2 mosaic images and thus span a radial range from $\sim$0.02" to about twice the half-light radius. We are able to accurately fit the entire profiles using either the S√{\textcopyright}rsic function or our new model. In doing so, we demonstrate that most, if not all, so-called ``power-law'' galaxies are better described as ``S√{\textcopyright}rsic galaxies''-they are well modeled by the three-parameter S√{\textcopyright}rsic profile into the limits of HST resolution-and that ``core'' galaxies are best understood as consisting of an outer S√{\textcopyright}rsic profile with an inner power-law cusp, which is a downward deviation from the inward extrapolation of the S√{\textcopyright}rsic profile. This definition of cores resolves ambiguities that result when the popular ``Nuker law'' is fitted to the profiles of ellipticals and bulges, particularly at lower luminosities. We also find that using the Nuker law to model core-galaxy nuclear profiles systematically overestimates the core radii by factors of 1.5-4.5 and underestimates the inner power-law slope by $\sim$20%-40% or more.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0403659}, -author = {Trujillo, I. and Erwin, Peter and Ramos, A. Asensio and Graham, Alister W.}, -doi = {10.1086/382712}, -eprint = {0403659}, -issn = {0004-6256}, -journal = {AJ}, -keywords = {Galaxies: Elliptical and Lenticular,Galaxies: Fundamental Parameters,Galaxies: Nuclei,Galaxies: Photometry,Galaxies: Structure,cD}, -month = {apr}, -number = {4}, -pages = {1917--1942}, -primaryClass = {astro-ph}, -title = {{Evidence for a New Elliptical-Galaxy Paradigm: Srsic and Core Galaxies}}, -url = {http://stacks.iop.org/1538-3881/127/i=4/a=1917}, -volume = {127}, -year = {2004} -} -@article{Tinker2016, -abstract = {We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen etal (2012) clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of Mgal for galaxies with logMgal{\textgreater}=11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma{\_}logM. Using this approach, we find sigma{\_}logM=0.18{\^{}}{\{}+0.01{\}}{\_}{\{}-0.02{\}}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L and Brownstein, Joel R and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {121}, -title = {{The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -volume = {839}, -year = {2017} -} -@article{Dutton2007, -abstract = {We use observed rotation velocity-luminosity (VL) and size-luminosity (RL) relations to single out a specific scenario for disk galaxy formation in the $\Lambda$CDM cosmology. Our model involves four independent lognormal random variables: dark halo concentration c, disk spin $\lambda$gal, disk mass fraction mgal, and stellar mass-to-light ratio $\Upsilon$I. A simultaneous match of the VL and RL zero points with adiabatic contraction requires low-c halos, but this model has V2.2{\$\sim${}}1.8Vvir (where V2.2 and Vvir are the circular velocity at 2.2 disk scale lengths and the virial radius, respectively), which will be unable to match the luminosity function (LF). Similarly models without adiabatic contraction but standard c also predict high values of V2.2/Vvir. Models in which disk formation induces an expansion rather than the commonly assumed contraction of the dark matter halos have V2.2{\$\sim${}}1.2Vvir, which allows a simultaneous fit of the LF. This may result from nonspherical, clumpy gas accretion, where dynamical friction transfers energy from the gas to the dark matter. This model requires low $\lambda$gal and mgal values, contrary to naive expectations. However, the low $\lambda$gal is consistent with the notion that disk galaxies predominantly survive in halos with a quiet merger history, while a low mgal is also indicated by galaxy-galaxy lensing. The smaller than expected scatter in the RL relation and the lack of correlation between the residuals of the VL and RL relations, respectively, imply that the scatter in $\lambda$gal and in c needs to be smaller than predicted for $\Lambda$CDM halos, again consistent with the idea that disk galaxies preferentially reside in halos with a quiet merger history.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0604553}, -author = {Dutton, Aaron A and van den Bosch, Frank C and Dekel, Avishai and Courteau, Stephane}, -doi = {10.1086/509314}, -eprint = {0604553}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Formation,Galaxies: Fundamental Parameters,Galaxies: Spiral,Galaxies: Structure}, -month = {jan}, -number = {1}, -pages = {27--52}, -primaryClass = {astro-ph}, -title = {{A Revised Model for the Formation of Disk Galaxies: Low Spin and Dark Halo Expansion}}, -url = {http://adsabs.harvard.edu/abs/2007ApJ...654...27D}, -volume = {654}, -year = {2006} -} -@article{Khochfar2011, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* > 1010.5M⊙ contributing $\sim$20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between $\sim$50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z > 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) > 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z < 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive (>1010M⊙) fast rotators being more than one order of magnitude more frequent at z$\sim$ 2. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R. and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Khochfar et al. - 2011 - The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies.pdf:pdf}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: structure}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1138?key=crossref.6ebb2a01dc7b45f1fa5c66089a37542b}, -volume = {709}, -year = {2010} -} -@article{LSSTDarkEnergyScienceCollaboration2012, -abstract = {This white paper describes the LSST Dark Energy Science Collaboration (DESC), whose goal is the study of dark energy and related topics in fundamental physics with data from the Large Synoptic Survey Telescope (LSST). It provides an overview of dark energy science and describes the current and anticipated state of the field. It makes the case for the DESC by laying out a robust analytical framework for dark energy science that has been defined by its members and the comprehensive three-year work plan they have developed for implementing that framework. The analysis working groups cover five key probes of dark energy: weak lensing, large scale structure, galaxy clusters, Type Ia supernovae, and strong lensing. The computing working groups span cosmological simulations, galaxy catalogs, photon simulations and a systematic software and computational framework for LSST dark energy data analysis. The technical working groups make the connection between dark energy science and the LSST system. The working groups have close linkages, especially through the use of the photon simulations to study the impact of instrument design and survey strategy on analysis methodology and cosmological parameter estimation. The white paper describes several high priority tasks identified by each of the 16 working groups. Over the next three years these tasks will help prepare for LSST analysis, make synergistic connections with ongoing cosmological surveys and provide the dark energy community with state of the art analysis tools. Members of the community are invited to join the LSST DESC, according to the membership policies described in the white paper. Applications to sign up for associate membership may be made by submitting the Web form at http://www.slac.stanford.edu/exp/lsst/desc/signup.html with a short statement of the work they wish to pursue that is relevant to the LSST DESC.}, -archivePrefix = {arXiv}, -arxivId = {1211.0310}, -author = {{LSST Dark Energy Science Collaboration}}, -eprint = {1211.0310}, -journal = {arXiv preprint arXiv:1211.0310}, -keywords = {Astrophysics - Cosmology and Extragalactic Astroph,High Energy Physics - Experiment}, -pages = {133}, -title = {{Large Synoptic Survey Telescope: Dark Energy Science Collaboration}}, -url = {http://arxiv.org/abs/1211.0310}, -year = {2012} -} -@article{Sonnenfeld2013a, -abstract = {We describe the goals of the CASTLES (CfA-Arizona-Space-Telescope-LEns-Survey) 1 project including a sample of NICMOS images of gravitational lenses and a brief list of the preliminary findings.}, -annote = {From Duplicate 14 (Supermassive black holes and their host spheroids I. Galaxy vivisection - Savorgnan, Giulia A. D.; Graham, Alister W.) - -NULL}, -archivePrefix = {arXiv}, -arxivId = {1211.0310}, -author = {Mu{\~{n}}oz, J. A. and Falco, E. E. and Kochanek, C. S. and Leh{\'{a}}r, J. and Mcleod, B. A. and Impey, C. D. and Rix, H. W. and Peng, C. Y.}, -doi = {10.1023/a:1002120921330}, -eprint = {1211.0310}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ding et al. - 2017 - H0LiCOW. VI. Testing the fidelity of lensed quasar host galaxy reconstruction.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sonnenfeld, Nipoti, Treu - 2014 - Purely dry mergers do not explain the observed evolution of massive early-type galaxies since z ∼ 1.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2014 - Measurements of charge transfer efficiency in a proton-irradiated swept charge device.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Savorgnan - 2016 - SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE M BH – n sph CORRELATION.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tessore, Bellagamba, Metcalf - 2016 - LENSED A code for the forward reconstruction of lenses and sources from strong lensing observation.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/LSST Dark Energy Science Collaboration - 2012 - Large Synoptic Survey Telescope Dark Energy Science Collaboration.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Springel et al. - 2018 - First results from the IllustrisTNG simulations Matter and galaxy clustering.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xia et al. - 2017 - Halo Intrinsic Alignment Dependence on Mass, Formation Time, and Environment.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kruk et al. - 2017 - Galaxy Zoo Finding offset discs and bars in SDSS galaxies.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Belfiore et al. - 2018 - SDSS IV MaNGA - sSFR profiles and the slow quenching of discs in green valley galaxies.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Peng et al. - 2002 - Detailed Structural Decomposition of Galaxy Images.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buitrago et al. - 2008 - Size Evolution of the Most Massive Galaxies at 1.7 z 3 from GOODS NICMOS Survey Imaging.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Spindler et al. - 2018 - SDSS-IV MaNGA The spatial distribution of star formation and its dependence on mass, structure, and environment.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Van Der Wel et al. - 2012 - Structural parameters of galaxies in candels.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Mu{\~{n}}oz et al. - 1998 - The castles project.pdf:pdf}, -isbn = {doi:10.1088/0004-637X/786/2/89}, -issn = {0004640X}, -journal = {Astrophysics and Space Science}, -keywords = {Astrophysics - Cosmology and Extragalactic Astroph,Black hole physics,Data analysis,Galaxies: active,Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure,Gravitational lensing: strong-methods,High Energy Physics - Experiment,Methods: numerical,Methods: statistical,Techniques: image processing,active,cD,catalogs,ccd,cte,cti,dwarf,evolution,formation,fundamental parameters,galaxies,galaxies: elliptical and lenticular,galaxies: formation,galaxies: high-redshift,galaxies: photometry,galaxies: statistics,galaxies: structure,galaxies: structure surveys,general,gravitational lensing,hxmt,interactions,irregular,ism,keyword1,keyword2,keyword3,le,proton-irradiated,quasars,scd,star formation,strong - galaxies,struc-,structure}, -month = {jun}, -number = {1-4}, -pages = {51--54}, -title = {{The castles project}}, -url = {http://arxiv.org/abs/1211.0310}, -volume = {263}, -year = {1998} -} -@article{Strigari2008, -abstract = {We use kinematic data from three new, nearby, extremely low-luminosity Milky Way dwarf galaxies (Ursa Major II, Willman 1, and Coma Berenices) to constrain the properties of their dark matter halos, and from these make predictions for the gamma-ray flux from annihilation of dark matter particles in these halos. We show that these 10{\^{}}3 solar luminosity dwarfs are the most dark matter dominated galaxies in the Universe, with total masses within 100 pc in excess of 10{\^{}}6 solar masses. Coupled with their relative proximity, their large masses imply that they should have mean gamma-ray fluxes comparable to or greater than any other known satellite galaxy of the Milky Way. Our results are robust to both variations of the inner slope of the density profile and the effect of tidal interactions. The fluxes could be boosted by up to two orders of magnitude if we include the density enhancements caused by surviving dark matter substructure.}, -archivePrefix = {arXiv}, -arxivId = {0709.1510}, -author = {Strigari, Louis E and Koushiappas, Savvas M and Bullock, James S and Kaplinghat, Manoj and Simon, Joshua D and Geha, Marla and Willman, Beth}, -doi = {10.1086/529488}, -eprint = {0709.1510}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Subject headingg s,cosmology,theory — dark matter}, -number = {2}, -pages = {614--620}, -pmid = {22580847}, -title = {{The Most Dark Matter Dominated Galaxies: Predicted Gamma-ray Signals from the Faintest Milky Way Dwarfs}}, -url = {http://arxiv.org/abs/0709.1510%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/529488}, -volume = {678}, -year = {2007} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted $\sim$100-200 luminous satellite galaxies in the past \$\sim$12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ($\sim$80%) coming from the \$\sim$15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of $\sim$9 Gyr in the past, while surviving satellite systems have median accretion times of $\sim$5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S. and Johnston, Kathryn V.}, -doi = {10.1086/497422}, -eprint = {0506467}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bullock, Johnston - 2005 - Tracing Galaxy Formation with Stellar Halos. I. Methods.pdf:pdf}, -isbn = {0272-9490 (Print)$\$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Yang2019, -abstract = {Using the Atacama Large Millimeter/submillimeter Array (ALMA), we report high angular-resolution observations of the redshift z = 3.63 galaxy H-ATLAS J083051.0+013224 (G09v1.97), one of the most luminous strongly lensed galaxies discovered by the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). We present 0.″2-0.″4 resolution images of the rest-frame 188 and 419 $\mu$m dust continuum and the CO(6-5), H2O(211-202), and Jup = 2 H2O+ line emission. We also report the detection of H2O(211-202) in this source. The dust continuum and molecular gas emission are resolved into a nearly complete ∼1.″5 diameter Einstein ring plus a weaker image in the center, which is caused by a special dual deflector lensing configuration. The observed line profiles of the CO(6-5), H2O(211-202), and Jup = 2 H2O+ lines are strikingly similar. In the source plane, we reconstruct the dust continuum images and the spectral cubes of the CO, H2O, and H2O+ line emission at sub-kiloparsec scales. The reconstructed dust emission in the source plane is dominated by a compact disk with an effective radius of 0.7 ± 0.1 kpc plus an overlapping extended disk with a radius twice as large. While the average magnification for the dust continuum is $\mu$ ∼ 10-11, the magnification of the line emission varies from 5 to 22 across different velocity components. The line emission of CO(6-5), H2O(211-202), and H2O+ have similar spatial and kinematic distributions. The molecular gas and dust content reveal that G09v1.97 is a gas-rich major merger in its pre-coalescence phase, with a total molecular gas mass of ∼1011 M. Both of the merging companions are intrinsically ultra-luminous infrared galaxies (ULIRGs) with infrared luminosities LIR reaching 4 × 1012 L, and the total LIR of G09v1.97 is (1.4 ± 0.7)×1013 L. The approaching southern galaxy (dominating from V = -400 to -150 km s-1 relative to the systemic velocity) shows no obvious kinematic structure with a semi-major half-light radius of as = 0.4 kpc, while the receding galaxy (0 to 350 km s-1) resembles an as = 1.2 kpc rotating disk. The two galaxies are separated by a projected distance of 1.3 kpc, bridged by weak line emission (-150 to 0 km s-1) that is co-spatially located with the cold dust emission peak, suggesting a large amount of cold interstellar medium (ISM) in the interacting region. As one of the most luminous star-forming dusty high-redshift galaxies, G09v1.97 is an exceptional source for understanding the ISM in gas-rich starbursting major merging systems at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {1903.00273}, -author = {Yang, C and Gavazzi, R and Beelen, A and Cox, P and Omont, A and Lehnert, M D and Gao, Y and Ivison, R J and Swinbank, A M and Barcos-Mu{\~{n}}oz, L and Neri, R and Cooray, A and Dye, S and Eales, S and Fu, H and Gonz{\'{a}}lez-Alfonso, E and Ibar, E and Micha{\l}owski, M J and Nayyeri, H and Negrello, M and Nightingale, J and P{\'{e}}rez-Fournon, I and Riechers, D A and Smail, I and {Van Der Werf}, P}, -doi = {10.1051/0004-6361/201833876}, -eprint = {1903.00273}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: ISM,Galaxies: high-redshift,Gravitational lensing: strong,ISM: molecules,Radio lines: ISM,Submillimeter: galaxies}, -pages = {23--42}, -title = {{CO, H2O, H2O+ line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales}}, -url = {http://arxiv.org/abs/1903.00273}, -volume = {624}, -year = {2019} -} -@article{Ding2018a, -abstract = {Strong gravitational lenses with measured time delay are a powerful tool to measure cosmological parameters, especially the Hubble constant ({\$}H{\_}0{\$}). Recent studies show by combining just three multiply-imaged AGN systems, one can determine {\$}H{\_}0{\$} down to 3{\%} precision. Furthermore, the number of time-delay lens is growing rapidly, enabling the determination of {\$}H{\_}0{\$} to 1{\%} precision in the near future. However, it is important to ensure that systematic errors and biases remain subdominant. For this purpose, challenges with simulated datasets are a key component. Following the experience of the past challenge on time delay, where it was shown that time delays can be measured precisely and accurately at the sub-percent level, we now present the "Time Delay Lens Modeling Challenge" (TDLMC). The goal of TDLMC is to assess the present capabilities of lens modeling codes and assumptions and test the level of accuracy of inferred cosmological parameters given realistic mock datasets. We invite scientists to model a set of simulated HST observations of 50 mock lens systems. The systems are organized in rungs, with the complexity and realism increasing going up the ladder. The goal of the challenge is to infer {\$}H{\_}0{\$} for each rung, given the HST images, the time delay, and a stellar velocity dispersion of the deflector, for a fixed background cosmology. The TDLMC challenge will start with the mock data release on 2018 January 8th. The deadline for blind submission is different for each rung. The deadline for Rung0-1 is 2018 Sept. 8; the deadline for Rung2 is 2019 Apr. 8 and the one for Rung3 is 2019 Sept. 8. This first paper gives an overview of the challenge including the data design, and a set of metrics to quantify the modeling performance and challenge details. After the deadline, the results of the challenge will be presented in a companion paper with all challenge participants as co-authors.}, -archivePrefix = {arXiv}, -arxivId = {1801.01506}, -author = {Ding, Xuheng and Treu, Tommaso and Shajib, Anowar J and Xu, Dandan and Chen, Geoff C -F. and More, Anupreeta and Despali, Giulia and Frigo, Matteo and Fassnacht, Christopher D and Gilman, Daniel and Hilbert, Stefan and Marshall, Philip J and Sluse, Dominique and Vegetti, Simona}, -eprint = {1801.01506}, -title = {{Time Delay Lens Modeling Challenge: I. Experimental Design}}, -url = {http://arxiv.org/abs/1801.01506}, -year = {2018} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) 'CMASS' sample at z {\$\sim${}} 0.5. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogues which include selection effects, reproduce the overall SMF, the projected two-point correlation function wp, the CMASS dn/dz, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of 'age matching' and show that these effects are markedly different compared to the ones explored by Hearin et al. at lower stellar masses. We construct two models, one in which galaxy colour is stochastic ('AbM' model) as well as a model which contains assembly bias effects ('AgM' model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colours are not a stochastic process in high-mass haloes. Our results suggest that the colours of galaxies in high-mass haloes are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P and Bundy, Kevin and Zentner, Andrew R and Behroozi, Peter S and Reid, Beth A and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L and White, Martin and Schneider, Donald P}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P{\_}KS $\backslash$simeq 1.5 $\backslash$times 10{\^{}}{\{}-4{\}}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability $\backslash$simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R and Kravtsov, Andrey V and Gnedin, Oleg Y and Klypin, Anatoly A}, -doi = {10.1086/431355}, -eprint = {0502496}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centres of typical $\sim$ L* and lower mass spheroids exhibit power-law 'cusps' with $\Sigma$ $\alpha$ R-$\eta$, where 0.5 ≲ $\eta$ ≲ 1 for radii $\sim$ 1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for, or strongly modify, the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m = 1 lopsided/eccentric disc instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*(< R) « MBH. When the stellar surface density profile is comparatively shallow with $\eta$ < 1/2, the modes cannot efficiently propagate to R = 0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than $\eta$ = 1, the inward propagation of eccentricity is strongly damped, suppressing inflow and bringing $\eta$ down again. Together these results produce an equilibrium slope of 1/2 ≲ $\eta$ ≲ 1 in the potential of the central black hole. These physical arguments are supported by non-linear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies. {\textcopyright} 2010 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F. and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins, Quataert - 2011 - An explanation for the slopes of stellar cusps in galaxy spheroids.pdf:pdf}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Lilly2016, -abstract = {There are very strong observed correlations between the specific star-formation rates (sSFR) of galaxies and their mean surface mass densities, {\{}$\backslash$Sigma{\}}, as well as other aspects of their internal structure. These strong correlations have often been taken to indicate that the internal structure of a galaxy must play a major physical role, directly or indirectly, in the control of star-formation. In this paper we show by means of a very simple toy model that these correlations can arise naturally without any such physical role once the observed evolution of the size-mass relation for star-forming galaxies is taken into account. In particular, the model reproduces the sharp threshold in {\{}$\backslash$Sigma{\}} between galaxies that are star-forming and those that are quenched, and the evolution of this threshold with redshift. Similarly, it produces iso-quenched-fraction contours in the {\$}{\{}f{\_}Q(m,R{\_}e){\}}{\$} plane that are almost exactly parallel to lines of constant {\{}$\backslash$Sigma{\}} for centrals and shallower for satellites. It does so without any dependence on quenching on size or {\{}$\backslash$Sigma{\}}, and without invoking any differences between centrals and satellites, beyond the different mass-dependences of their quenching laws. The toy-model also reproduces several other observations, including the sSFR gradients within galaxies and the appearance of inside-out build-up of passive galaxies. Finally, it is shown that curvature in the Main Sequence sSFR-mass relation can produce curvature in the apparent B/T ratios with mass. Our analysis therefore suggests that many of the strong correlations that are observed between galaxy structure and sSFR may well be a consequence of things unrelated to quenching and should not be taken as evidence of the physical processes that drive quenching.}, -archivePrefix = {arXiv}, -arxivId = {1604.06459}, -author = {Lilly, Simon J and Carollo, C Marcella}, -doi = {10.3847/0004-637x/833/1/1}, -eprint = {1604.06459}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {1}, -pmid = {15540530}, -title = {{Surface Density Effects in Quenching: Cause or Effect?}}, -url = {http://arxiv.org/abs/1604.06459%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/833/1/1}, -volume = {833}, -year = {2016} -} -@article{Tessore2015, -abstract = {The deflection, potential, shear and magnification of a gravitational lens following an elliptical power law mass model are investigated. This mass model is derived from the circular power law profile through a rescaling of the axes, similar to the case of a singular isothermal ellipsoid. The resulting deflection can be calculated explicitly and given in terms of the Gaussian hypergeometric function. Analytic expressions for the remaining lensing properties are found as well. Because the power law profile lens contains a number of well-known lens models as special cases, the equivalence of the new expressions with known results is checked. Finally, it is shown how these results naturally lead to a fast and accurate numerical scheme for computing the deflection and other lens quantities, making this method a useful tool for realistically modelling observed lenses.}, -archivePrefix = {arXiv}, -arxivId = {1507.01819}, -author = {Tessore, Nicolas and Metcalf, R. B.}, -doi = {10.1051/0004-6361/201526773}, -eprint = {1507.01819}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Tessore2016PowerLaw.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Gravitational lensing: strong,Methods: analytical}, -number = {1}, -pages = {1--6}, -title = {{The elliptical power law profile lens}}, -volume = {580}, -year = {2015} -} -@article{Brewer2012, -archivePrefix = {arXiv}, -arxivId = {1201.1677}, -author = {Brewer, B.$\sim$J. and Dutton, A.$\sim$A. and Treu, T and Auger, M.$\sim$W. and Marshall, P.$\sim$J. and Barnab{\`{e}}, M and Bolton, A.$\sim$S. and Koo, D.$\sim$C. and Koopmans, L.$\sim$V.$\sim$E.}, -doi = {10.1111/j.1365-2966.2012.20870.x}, -eprint = {1201.1677}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brewer et al. - 2012 - The SWELLS survey - III. Disfavouring 'heavy' initial mass functions for spiral lens galaxies.pdf:pdf}, -journal = {\mnras}, -keywords = {galaxies: fundamental parameters,galaxies: spiral,gravitational lensing: strong,mass function,stars: luminosity function}, -month = {jun}, -pages = {3574--3590}, -title = {{The SWELLS survey - III. Disfavouring 'heavy' initial mass functions for spiral lens galaxies}}, -volume = {422}, -year = {2012} -} -@article{Minor2021a, -abstract = {We demonstrate that the perturbations of strongly lensed images by low-mass dark matter subhaloes are significantly impacted by the concentration of the perturbing subhalo. For subhalo concentrations expected in Lambda cold dark matter ($\Lambda$CDM), significant constraints on the concentration can be obtained at Hubble Space Telescope (HST) resolution for subhaloes with masses larger than about 1010, M⊙. Constraints are also possible for lower mass subhaloes, if their concentrations are higher than the expected scatter in CDM. We also find that the concentration of lower mass perturbers down to ∼ 108, M⊙ can be well constrained with a resolution of ∼0.01 arcsec, which is achievable with long-baseline interferometry. Subhalo concentration also plays a critical role in the detectability of a perturbation, such that only high-concentration perturbers with mass ≲ 109, M⊙ are likely to be detected at HST resolution. If scatter in the $\Lambda$CDM mass-concentration relation is not accounted for during lens modelling, the inferred subhalo mass can be biased by up to a factor of 3 (6) for subhaloes of mass 109, M⊙, (1010, M⊙); this bias can be eliminated if one varies both mass and concentration during lens fitting. Alternatively, one may robustly infer the projected mass within the subhalo's perturbation radius, defined by its distance to the critical curve of the lens being perturbed. With a sufficient number of detections, these strategies will make it possible to constrain the halo mass-concentration relation at low masses in addition to the mass function, offering a probe of dark matter physics as well as the small-scale primordial power spectrum.}, -archivePrefix = {arXiv}, -arxivId = {2011.10629}, -author = {Minor, Quinn and Kaplinghat, Manoj and Chan, Tony H. and Simon, Emily}, -doi = {10.1093/mnras/stab2209}, -eprint = {2011.10629}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Minor2021DMConcentration.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {dark matter,galaxies: dwarf,gravitational lensing: strong}, -number = {1}, -pages = {1202--1215}, -title = {{Inferring the concentration of dark matter subhaloes perturbing strongly lensed images}}, -volume = {507}, -year = {2021} -} -@article{Oser:2010aa, -abstract = {Cosmological simulations of galaxy formation appear to show a "two-phase" character with a rapid early phase at z≳2 duringwhich "in situ" stars are formedwithin the galaxy from infalling cold gas followed by an extended phase since z≲3 duringwhich "ex situ" stars are primarily accreted. In the latter phase, massive systems growconsiderably in mass and radius by accretion of smaller satellite stellar systems formed at quite early times (z > 3) outside of the virial radius of the forming central galaxy. These tentative conclusions are obtained from high-resolution resimulations of 39 individual galaxies in a full cosmological context with present-day virial halomasses ranging from 7×10 11M⊙ h -1 ≲ Mvir ≲ 2.7×1013M⊙ h -1 (h = 0.72) and central galaxy masses between 4.5×1010M⊙ h -1 ≲ M* ≲ 3.6 × 1011M⊙ h -1. The simulations include the effects of a uniform UV background, radiative cooling, star formation, and energetic feedback from Type II supernova. The importance of stellar accretion increases with galaxy mass and toward lower redshift. In our simulations, lower mass galaxies (M* ≲ 9 × 10 10M⊙ h -1) accrete about 60% of their present-day stellar mass. High-mass galaxy (M* ≳ 1.7 × 10 11M⊙ h -1) assembly is dominated by accretion and merging with about 80% of the stars added by the present day. In general the simulated galaxies approximately double their mass since z = 1. For massive systems this mass growth is not accompanied by significant star formation. The majority of the in situ created stars are formed at z > 2, primarily out of cold gas flows. We recover the observational result of "archaeological downsizing," where the most massive galaxies harbor the oldest stars. We find that this is not in contradiction with hierarchical structure formation. Most stars in the massive galaxies are formed early on in smaller structures; the galaxies themselves are assembled late. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1010.1381}, -author = {Oser, Ludwig and Ostriker, Jeremiah P. and Naab, Thorsten and Johansson, Peter H. and Burkert, Andreas}, -doi = {10.1088/0004-637X/725/2/2312}, -eprint = {1010.1381}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oser et al. - 2010 - The two phases of galaxy formation(3).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Cosmology:theory,Dark matter,Galaxies:evolution,Galaxies:formation,Methods:numerical}, -month = {dec}, -number = {2}, -pages = {2312--2323}, -title = {{The two phases of galaxy formation}}, -volume = {725}, -year = {2010} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of supermassive black hole (SMBH) formation and evolution is used, as in Tremmel et al., allowing us to explicitly follow the SMBH dynamics at the centre of galaxies. A high SIDM constant cross-section is chosen, $\sigma$ = 10 cm2gr-1, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in cold dark matter (CDM), with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals, the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80 per cent of the SMBH population is offcentred in the SIDM case, as opposed to the CDM case in which $\sim$90 per cent of SMBHs have reached their host's centre. SMBHs are found as far as $\sim$9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction time-scale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in core stalling. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to the SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Di Cintio et al. - 2017 - A rumble in the dark Signatures of self-interacting dark matter in supermassive black hole dynamics and gal(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287----a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{Tazzari2018, -abstract = {We present GALARIO, a computational library that exploits the power of modern graphical processing units (GPUs) to accelerate the analysis of observations from radio interferometers like Atacama Large Millimeter and sub-millimeter Array or the Karl G. Jansky Very Large Array. GALARIO speeds up the computation of synthetic visibilities from a generic 2D model image or a radial brightness profile (for axisymmetric sources). On a GPU, GALARIO is 150 faster than standard PYTHON and 10 times faster than serial C++ code on a CPU. Highly modular, easy to use, and to adopt in existing code,GALARIOcomes as two compiled libraries, one for Nvidia GPUs and one for multicore CPUs, where both have the same functions with identical interfaces. GALARIO comes with PYTHON bindings but can also be directly used in C or C++. The versatility and the speed of GALARIO open new analysis pathways that otherwise would be prohibitively time consuming, e.g. fitting high-resolution observations of large number of objects, or entire spectral cubes of molecular gas emission. It is a general tool that can be applied to any field that uses radio interferometer observations. The source code is available online at http://github.com/mtazzari/galario under the open source GNU Lesser General Public License v3.}, -archivePrefix = {arXiv}, -arxivId = {1709.06999}, -author = {Tazzari, Marco and Beaujean, Frederik and Testi, Leonardo}, -doi = {10.1093/mnras/sty409}, -eprint = {1709.06999}, -file = {:C\:/Users/Jammy/Documents/Papers/uvplane/Tazzari2017GALARIO.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: numerical,Submillimetre: general,Techniques: interferometric}, -number = {4}, -pages = {4527--4542}, -title = {{GALARIO: A GPU accelerated library for analysing radio interferometer observations}}, -volume = {476}, -year = {2018} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the $\Lambda$CDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no significant detection of a stellar halo, as in the case of M101, NGC 3351 and NGC 1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies in the range M200 = 8 × 1011-2 × 1012 M⊙ with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction fSH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming, and assemble their dark matter halos earlier than galaxies with similar masses. They have also accreted more low-mass satellites at earlier infall times than centrals with high fSH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretiondominated r $\sim$ 45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers at higher redshifts and evolved unperturbed in the last $\sim$10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M. and Sales, Laura V. and Creasey, Peter and Cooper, Michael C. and Bullock, James S. and {Michael Rich}, R. and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Elias et al. - 2018 - Stellar halos in illustris Probing the histories of milky way-mass galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high-resolution N-body simulations of galactic dark matter haloes to test if this remarkable property can be understood within the context of the cold dark matter (CDM) cosmology. We construct halo merger trees from the simulations and use a semi-analytic model to follow the formation of satellite galaxies. We find that in all six of our simulations, the 11 brightest satellites are indeed distributed along thin, disc-like structures analogous to that traced by the satellites of the Milky Way. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhaloes within it, which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhaloes but is similar to that of the subset of subhaloes that had the most massive progenitors at earlier times. The elongated disc-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I and Frenk, Carlos S and Cole, Shaun and Helly, John C and Jenkins, Adrian and Navarro, Julio F and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Amorisco2017, -abstract = {The accreted component of stellar haloes is composed of the contributions of several satellites, falling on to their host with their different masses, at different times, on different orbits. This work uses a suite of idealized, collisionless N-body simulations of minor mergers and a particle-tagging technique to understand how these different ingredients shape each contribution to the accreted halo, in both density and kinematics. I find that more massive satellites deposit their stars deeper into the gravitational potential of the host, with a clear segregation enforced by dynamical friction. Earlier accretion events contribute more to the inner regions of the halo; more concentrated subhaloes sink deeper through increased dynamical friction. The orbital circularity of the progenitor at infall is only important for low-mass satellites: dynamical friction efficiently radializes the most massive minor mergers erasing the imprint of the infall orbit for satellite-to-host virial mass ratios ≳ 1/20. The kinematics of the stars contributed by each satellite is also ordered with satellite mass: low-mass satellites contribute fast-moving populations, in both ordered rotation and radial velocity dispersion. In turn, contributions by massive satellites have lower velocity dispersion and lose their angular momentum to dynamical friction, resulting in a strong radial anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {1511.08806}, -author = {Amorisco, N. C.}, -doi = {10.1093/mnras/stw2229}, -eprint = {1511.08806}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Amorisco - 2017 - Contributions to the accreted stellar halo An atlas of stellar deposition(3).pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Amorisco - 2017 - Contributions to the accreted stellar halo An atlas of stellar deposition(4).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: interactions,Galaxies: kinematics and dynamics,Galaxies: structure,Galaxy: halo}, -number = {3}, -pages = {2882--2895}, -title = {{Contributions to the accreted stellar halo: An atlas of stellar deposition}}, -url = {http://arxiv.org/abs/1511.08806%0Ahttp://dx.doi.org/10.1093/mnras/stw2229}, -volume = {464}, -year = {2017} -} -@article{Lauer2005, -abstract = {We present observations of 77 early-type galaxies imaged with the PC1 CCD of the Hubble Space Telescope (HST) WFPC2. "Nuker-law" parametric fits to the surface brightness profiles are used to classify the central structure into "core" or "power-law" forms. Core galaxies are typically rounder than power-law galaxies. Nearly all power-law galaxies with central ellipticities $\epsilon$ ≥ 0.3 have stellar disks, implying that disks are present in power-law galaxies with $\epsilon$ {\textless} 0.3 but are not visible because of unfavorable geometry. A few low-luminosity flattened core galaxies also have disks; these may be transition forms from power-law galaxies to more luminous core galaxies, which lack disks. Several core galaxies have strong isophote twists interior to their break radii, although power-law galaxies have interior twists of similar physical significance when the photometric perturbations implied by the twists are evaluated. Central color gradients are typically consistent with the envelope gradients; core galaxies have somewhat weaker color gradients than power-law galaxies. Nuclei are found in 29{\%} of the core galaxies and 60{\%} of the power-law galaxies. Nuclei are typically bluer than the surrounding galaxy. While some nuclei are associated with active galactic nuclei (AGNs), just as many are not; conversely, not all galaxies known to have a low-level AGN exhibit detectable nuclei in the broadband filters. NGC 4073 and 4382 are found to have central minima in their intrinsic starlight distributions; NGC 4382 resembles the double nucleus of M31. In general, the peak brightness location is coincident with the photocenter of the core to a typical physical scale of {\textless} 1 pc. Five galaxies, however, have centers significantly displaced from their surrounding cores; these may be unresolved asymmetric double nuclei. Finally, as noted by previous authors, central dust is visible in about half of the galaxies. The presence and strength of dust correlates with nuclear emission; thus, dust may outline gas that is falling into the central black hole. The prevalence of dust and its morphology suggest that dust clouds form, settle to the center, and disappear repeatedly on ∼ 10 8 yr timescales. We discuss the hypothesis that cores are created by the decay of a massive black hole binary formed in a merger. Apart from their brightness profiles, there are no strong differences between core galaxies and power-law galaxies that demand this scenario; however, the rounder shapes of core, their lack of disks, and their reduced color gradients may be consistent with it. {\textcopyright}2005. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0412040}, -author = {Lauer, Tod R and Faber, S M and Gebhardt, Karl and Richstone, Douglas and Tremaine, Scott and Ajhar, Edward A and Aller, M C and Bender, Ralf and Dressler, Alan and Filippenko, Alexei V and Green, Richard and Grillmair, Carl J and Ho, Luis C and Kormendy, John and Magorrian, John and Pinkney, Jason and Siopis, Christos}, -doi = {10.1086/429565}, -eprint = {0412040}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2138--2185}, -primaryClass = {arXiv:astro-ph}, -title = {{ The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry }}, -url = {http://stacks.iop.org/1538-3881/129/i=5/a=2138}, -volume = {129}, -year = {2005} -} -@article{Bullock2001, -abstract = {We study dark matter halo density profiles in a high-resolution N-body simulation of a $\Lambda$CDM cosmology. Our statistical sample contains ∼5000 haloes in the range 1011-1014 h-1 M⊙, and the resolution allows a study of subhaloes inside host haloes. The profiles are parametrized by an NFW form with two parameters, an inner radius rs and a virial radius Rvir, and we define the halo concentration cvir ≡ Rvir/rs. First, we find that, for a given halo mass, the redshift dependence of the median concentration is cvir ∝ (1 + z)-1. This corresponds to rs(z) ∼ constant, and is contrary to earlier suspicions that cvir does not vary much with redshift. The implications are that high-redshift galaxies are predicted to be more extended and dimmer than expected before. Secondly, we find that the scatter in halo profiles is large, with a 1$\sigma$ $\Delta$(log cvir) = 0.18 at a given mass, corresponding to a scatter in maximum rotation velocities of $\Delta$Vmax/Vmax = 0.12. We discuss implications for modelling the Tully-Fisher relation, which has a smaller reported intrinsic scatter. Thirdly, subhaloes and haloes in dense environments tend to be more concentrated than isolated haloes, and show a larger scatter. These results suggest that cvir is an essential parameter for the theory of galaxy modelling, and we briefly discuss implications for the universality of the Tully-Fisher relation, the formation of low surface brightness galaxies, and the origin of the Hubble sequence. We present an improved analytic treatment of halo formation that fits the measured relations between halo parameters and their redshift dependence, and can thus serve semi-analytic studies of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9908159}, -author = {Bullock, J. S. and Kolatt, T. S. and Sigad, Y. and Somerville, R. S. and Kravtsov, A. V. and Klypin, A. A. and Primack, J. R. and Dekel, A.}, -doi = {10.1046/j.1365-8711.2001.04068.x}, -eprint = {9908159}, -isbn = {978-1-4244-6023-6}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: formation,Galaxies: structure}, -number = {3}, -pages = {559--575}, -pmid = {25246403}, -primaryClass = {astro-ph}, -title = {{Profiles of dark haloes: Evolution, scatter and environment}}, -url = {http://mnras.oxfordjournals.org/content/321/3/559.short}, -volume = {321}, -year = {2001} -} -@article{Croom2009, -abstract = {We present the quasi-stellar object (QSO) luminosity function (LF) of the completed 2dF-SDSS LRG and QSO (2SLAQ) survey, based on QSOs photometrically selected from Sloan Digital Sky Survey (SDSS) imaging data and then observed spectroscopically using the 2dF instrument on the Anglo-Australian Telescope. We analyse 10 637 QSOs in the redshift range 0.4 < z < 2.6 to a g-band flux limit of 21.85 (extinction-corrected) and an absolute continuum magnitude of Mg(z = 2) < -21.5. This sample covers an area of 191.9 deg 2. The binned QSO LF agrees with that of the brighter SDSS main QSO sample, but extends ∼2.5 mag fainter, clearly showing the flattening of the LF towards faint absolute magnitudes. 2SLAQ finds an excess of QSOs compared to the 2dF QSO Redshift Survey at g > 20.0, as found previously by Richards et al. The LF is consistent with other previous, much smaller, samples produced to the depth of 2SLAQ. By combining the 2SLAQ and SDSS QSO samples, we produce a QSO LF with an unprecedented combination of precision and dynamic range. With this we are able to accurately constrain both the bright and faint ends of the QSO LF. While the overall trends seen in the evolution of the QSO LF appear similar to pure luminosity evolution, the data show very significant departures from such a model. Most notably we see clear evidence that the number density of faint QSOs peaks at lower redshift than bright QSOs: QSOs with Mg > -23 have space densities which peak at z < 1, while QSOs at M g < -26 peak at z > 2. By fitting simple LF models in narrow Mg intervals, we find that this downsizing is significant at the 99.98 per cent level. We show that LF models which follow the pure luminosity evolution form [i.e. M*g ≡ M*g(z)], but with a redshift-dependent bright-end slope and an additional density evolution term, $\Phi$*≡ $\Phi$*(z), provide a much improved fit to the data. The bright-end slope, $\alpha$, steepens from $\alpha$ ≃ -3.0 at z ≃ 0.5 to $\alpha$ = -3.5 at z ≃ 2.5. This steepening is significant at the 99.9 per cent level. We find a decline in $\Phi$*from z ≃ 0.5 to 2.5 which is significant at the 94 per cent level. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0907.2727}, -author = {Croom, Scott M. and Richards, Gordon T. and Shanks, Tom and Boyle, Brian J. and Strauss, Michael A. and Myers, Adam D. and Nichol, Robert C. and Pimbblet, Kevin A. and Ross, Nicholas P. and Schneider, Donald P. and Sharp, Robert G. and Wake, David A.}, -doi = {10.1111/j.1365-2966.2009.15398.x}, -eprint = {0907.2727}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Seyfert,Galaxies: active,Quasars: general}, -month = {nov}, -number = {4}, -pages = {1755--1772}, -title = {{The 2dF-SDSS LRG and QSO survey: The QSO luminosity function at 0.4 < z < 2.6}}, -volume = {399}, -year = {2009} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned r- and g-band images from a sample of 45 508 galaxies from Sloan Digital Sky Survey Data Release 9 in the redshift range 0.06≤z≤0.1 and in the mass range 1010.0M⊙ {\textless}M* {\textless} 1011.4M⊙.We derive surface brightness profiles to a depth of almost $\mu$r ̃ 32 mag arcsec-2. We find that the ellipticity of the stellar halo is a function of galaxy stellar mass and that the haloes of high-concentration galaxies are more elliptical than those of low-concentration galaxies. Where the g - r colour of the stellar halo can be measured, we find that the stellar light is always bluer than in the main galaxy. The colour of the stellar halo is redder for more massive galaxies. We further demonstrate that the full two-dimensional surface intensity distribution of our galaxy stacks can only be fit through multicomponent S{\'{e}}rsic models. Using the fraction of light in the outer component of the models as a proxy for the fraction of accreted stellar light, we show that this fraction is a function of stellar mass and galaxy type. The fraction of accreted stellar light rises from 30 to 70 per cent and from 2 to 25 per cent for high- and low-concentration galaxies, respectively, over the mass range 1010.0-1011.4M⊙. {\textcopyright}2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1404.2123}, -author = {D'Souza, Richard and Kauffman, Guinevere and Wang, Jing and Vegetti, Simona}, -doi = {10.1093/mnras/stu1194}, -eprint = {1404.2123}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: halo,Galaxy: structure}, -number = {2}, -pages = {1433--1450}, -title = {{Parametrizing the stellar haloes of galaxies}}, -volume = {443}, -year = {2014} -} -@article{Bentabol2016, -abstract = {We examine a sample of 1495 galaxies in the CANDELS fields to determine the evolution of two-component galaxies, including bulges and discs, within massive galaxies at the epoch 1 {\textless} z {\textless}3 when the Hubble sequence forms. We fit all of our galaxies' light profiles with a single S{\'{e}}rsic fit, as well as with a combination of exponential and S{\'{e}}rsic profiles. The latter is done in order to describe a galaxy with an inner and an outer component, or bulge and disc component. We develop and use three classification methods (visual, F-test and the residual flux fraction) to separate our sample into one-component galaxies (disc/spheroidslike galaxies) and two-component galaxies (galaxies formed by an 'inner part' or bulge and an 'outer part' or disc). We then compare the results from using these three different ways to classify our galaxies.We find that the fraction of galaxies selected as two-component galaxies increases on average 50 per cent from the lowest mass bin to the most massive galaxies, and decreases with redshift by a factor of 4 from z = 1 to 3. We find that single S{\'{e}}rsic 'disc-like' galaxies have the highest relative number densities at all redshifts, and that two-component galaxies have the greatest increase and become at par with S{\'{e}}rsic discs by z = 1. We also find that the systems we classify as two-component galaxies have an increase in the sizes of their outer components, or 'discs', by about a factor of 3 from z = 3 to 1.5, while the inner components or 'bulges' stay roughly the same size. This suggests that these systems are growing from the inside out, whilst the bulges or protobulges are in place early in the history of these galaxies. This is also seen to a lesser degree in the growth of single 'disc-like' galaxies versus 'spheroid-like' galaxies over the same epoch.}, -archivePrefix = {arXiv}, -arxivId = {1606.07405}, -author = {Margalef-Bentabol, Berta and Conselice, Christopher J and Mortlock, Alice and Hartley, Will and Duncan, Kenneth and Ferguson, Harry C and Dekel, Avishai and Primack, Joel R}, -doi = {10.1093/mnras/stw1451}, -eprint = {1606.07405}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure}, -number = {3}, -pages = {1--21}, -title = {{The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z {\textless} 3}}, -volume = {461}, -year = {2016} -} -@article{PyNUFFT, -abstract = {A Python non-uniform fast Fourier transform (PyNUFFT) package has been developed to accelerate multidimensional non-Cartesian image reconstruction on heterogeneous platforms. Since scientific computing with Python encompasses a mature and integrated environment, the time efficiency of the NUFFT algorithm has been a major obstacle to real-time non-Cartesian image reconstruction with Python. The current PyNUFFT software enables multi-dimensional NUFFT accelerated on a heterogeneous platform, which yields an efficient solution to many non-Cartesian imaging problems. The PyNUFFT also provides several solvers, including the conjugate gradient method, 1 total variation regularized ordinary least square (L1TV-OLS), and 1 total variation regularized least absolute deviation (L1TV-LAD). Metaprogramming libraries have been employed to accelerate PyNUFFT. The PyNUFFT package has been tested on multi-core central processing units (CPUs) and graphic processing units (GPUs), with acceleration factors of 6.3–9.5× on a 32-thread CPU platform and 5.4–13× on a GPU.}, -author = {Lin, Jyh Miin}, -doi = {10.3390/jimaging4030051}, -issn = {2313433X}, -journal = {Journal of Imaging}, -keywords = {Graphic processing unit (GPU),Heterogeneous system architecture (HSA),Magnetic resonance imaging (MRI),Multi-core system,Total variation (TV)}, -number = {3}, -pages = {1--22}, -title = {{Python non-uniform fast fourier transform (PyNUFFT): An accelerated non-cartesian MRI package on a heterogeneous platform (CPU/GPU)}}, -volume = {4}, -year = {2018} -} -@article{Bonaca2019, -abstract = {We present a model for the interaction of the GD-1 stellar stream with a massive perturber that naturally explains many of the observed stream features, including a gap and an off-stream spur of stars. The model involves an impulse by a fast encounter, after which the stream grows a loop of stars at different orbital energies. At specific viewing angles, this loop appears offset from the stream track. A quantitative comparison of the spur and gap features prefers models where the perturber is in the mass range of {\$}10{\^{}}6\backslash,\backslashrm M{\_}\backslashodot{\$} to {\$}10{\^{}}8\backslash,\backslashrm M{\_}\backslashodot{\$}. Orbit integrations back in time show that the stream encounter could not have been caused by any known globular cluster or dwarf galaxy with a determined orbit, and mass, size and impact-parameter arguments show that it could not have been caused by a molecular cloud in the Milky Way disk. The most plausible explanation for the gap-and-spur structure is an encounter with a dark-matter substructure, like those predicted to populate galactic halos in LCDM cosmology. However, the expected densities of LCDM subhalos in this mass range and in this part of the Milky Way are {\$}2-3\backslash,\backslashsigma{\$} lower than the inferred density of the GD-1 perturber. This observation opens up the possibility that detailed observations of streams could measure the mass spectrum of dark-matter substructures and even identify individual substructures and their orbits in the Galactic halo.}, -archivePrefix = {arXiv}, -arxivId = {1811.03631}, -author = {Bonaca, Ana and Hogg, David W and Price-Whelan, Adrian M and Conroy, Charlie}, -doi = {10.3847/1538-4357/ab2873}, -eprint = {1811.03631}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cosmology,dark matter,galaxy,gravitation,halo,kinematics and dynamics,observations,stars}, -number = {1}, -pages = {38}, -title = {{The Spur and the Gap in GD-1: Dynamical Evidence for a Dark Substructure in the Milky Way Halo}}, -volume = {880}, -year = {2019} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58 arcsec in the i band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including an {\$\sim${}}10 per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally,we check the sensitivity of our shear calibration estimates to other cutsmade on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalogue are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{Amblard2010, -abstract = {We present colour-colour diagrams of detected sources in the Herschel-ATLAS science demonstration field from 100 to 500 $\mu$m using both PACS and SPIRE. We fit isothermal modified black bodies to the spectral energy distribution (SED) to extract the dust temperature of sources with counterparts in Galaxy And Mass Assembly (GAMA) or SDSS surveys with either a spectroscopic or a photometric redshift. For a subsample of 330 sources detected in at least three FIR bands with a significance greater than 3$\sigma$, we find an average dust temperature of (28±8) K. For sources with no known redshift, we populate the colour-colour diagram with a large number of SEDs generated with a broad range of dust temperatures and emissivity parameters, and compare to colours of observed sources to establish the redshift distribution of this sample. For another subsample of 1686 sources with fluxes above 35 mJy at 350 $\mu$m and detected at 250 and 500 $\mu$m with a significance greater than 3$\sigma$, we find an average redshift of 2.2±0.6. {\textcopyright} 2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1005.2412}, -author = {Amblard, A. and Cooray, A. and Serra, P. and Temi, P. and Barton, E. and Negrello, M. and Auld, R. and Baes, M. and Baldry, I. K. and Bamford, S. and Blain, A. and Bock, J. and Bonfield, D. and Burgarella, D. and Buttiglione, S. and Cameron, E. and Cava, A. and Clements, D. and Croom, S. and Dariush, A. and {De Zotti}, G. and Driver, S. and Dunlop, J. and Dunne, L. and Dye, S. and Eales, S. and Frayer, D. and Fritz, J. and Gardner, Jonathan P. and Gonzalez-Nuevo, J. and Herranz, D. and Hill, D. and Hopkins, A. and Hughes, D. H. and Ibar, E. and Ivison, R. J. and Jarvis, M. and Jones, D. H. and Kelvin, L. and Lagache, G. and Leeuw, L. and Liske, J. and Lopez-Caniego, M. and Loveday, J. and Maddox, S. and Micha{\l}owski, M. and Norberg, P. and Parkinson, H. and Peacock, J. A. and Pearson, C. and Pascale, E. and Pohlen, M. and Popescu, C. and Prescott, M. and Robotham, A. and Rigby, E. and Rodighiero, G. and Samui, S. and Sansom, A. and Scott, D. and Serjeant, S. and Sharp, R. and Sibthorpe, B. and Smith, D. J.B. and Thompson, M. A. and Tuffs, R. and Valtchanov, I. and {Van Kampen}, E. and {Van Der Werf}, P. and Verma, A. and Vieira, J. and Vlahakis, C.}, -doi = {10.1051/0004-6361/201014586}, -eprint = {1005.2412}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: high-redshift,Galaxy: evolution,Submillimeter: galaxies}, -number = {1}, -pages = {1--5}, -title = {{Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours}}, -url = {http://arxiv.org/abs/1005.2412%0Ahttp://dx.doi.org/10.1051/0004-6361/201014586}, -volume = {518}, -year = {2010} -} -@article{Costantin2017, -abstract = {Context. The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. Aims. We aim to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. Methods. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the i-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new (B=A, C=A) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. Results. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations of 25° ≤ $\theta$ ≤ 65° we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66%), with a smaller fraction of prolate spheroids (19%), and triaxial ellipsoids (15%). The majority of triaxial bulges are in barred galaxies (75%). Moreover, we found that bulges with low S{\'{e}}rsic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, bulges in late-type galaxies or in less massive galaxies have no preference for being oblate, prolate, or triaxial. On the contrary, bulges with high S{\'{e}}rsic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. Conclusions. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L. and M{\'{e}}ndez-Abreu, J. and Corsini, E. M. and Eliche-Moral, M. C. and Tapia, T. and Morelli, L. and Elena, Dalla Bont{\`{a}} and Pizzella, A.}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Costantin et al. - 2018 - The intrinsic shape of bulges in the CALIFA survey.pdf:pdf}, -issn = {14320746}, -journal = {A&A}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -volume = {609}, -year = {2018} -} -@article{Governato2010, -abstract = {For almost two decades the properties of dwarf galaxies have challenged the cold dark matter (CDM) model of galaxy formation. Most observed dwarf galaxies consist of a rotating stellar disk embedded in a massive dark-matter halo with a near-constant-density core. Models based on the dominance of CDM, however, invariably form galaxies with dense spheroidal stellar bulges and steep central dark-matter profiles, because low-angular-momentum baryons and dark matter sink to the centres of galaxies through accretion and repeated mergers. Processes that decrease the central density of CDM halos have been identified, but have not yet reconciled theory with observations of present-day dwarfs. This failure is potentially catastrophic for the CDM model, possibly requiring a different dark-matter particle candidate. Here we report hydrodynamical simulations (in a framework assuming the presence of CDM and a cosmological constant) in which the inhomogeneous interstellar medium is resolved. Strong outflows from supernovae remove low-angular-momentum gas, which inhibits the formation of bulges and decreases the dark-matter density to less than half of what it would otherwise be within the central kiloparsec. The analogues of dwarf galaxiesbulgeless and with shallow central dark-matter profilesarise naturally in these simulations. {\textcopyright} 2010 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0911.2237}, -author = {Governato, F. and Brook, C. and Mayer, L. and Brooks, A. and Rhee, G. and Wadsley, J. and Jonsson, P. and Willman, B. and Stinson, G. and Quinn, T. and Madau, P.}, -doi = {10.1038/nature08640}, -eprint = {0911.2237}, -isbn = {0028-0836}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7278}, -pages = {203--206}, -pmid = {20075915}, -title = {{Bulgeless dwarf galaxies and dark matter cores from supernova-driven outflows}}, -url = {http://arxiv.org/abs/0911.2237%5Cnhttp://dx.doi.org/10.1038/nature08640%5Cnhttp://www.nature.com/doifinder/10.1038/nature08640}, -volume = {463}, -year = {2010} -} -@article{Martin-Navarro2018, -abstract = {Supermassive black holes, with masses more than a million times that of the Sun, seem to inhabit the centres of all massive galaxies. Cosmologically motivated theories of galaxy formation require feedback from these supermassive black holes to regulate star formation. In the absence of such feedback, state-of-the-art numerical simulations fail to reproduce the number density and properties of massive galaxies in the local Universe. There is, however, no observational evidence of this strongly coupled coevolution between supermassive black holes and star formation, impeding our understanding of baryonic processes within galaxies. Here we report that the star formation histories of nearby massive galaxies, as measured from their integrated optical spectra, depend on the mass of the central supermassive black hole. Our results indicate that the black-hole mass scales with the gas cooling rate in the early Universe. The subsequent quenching of star formation takes place earlier and more efficiently in galaxies that host higher-mass central black holes. The observed relation between black-hole mass and star formation efficiency applies to all generations of stars formed throughout the life of a galaxy, revealing a continuous interplay between black-hole activity and baryon cooling.}, -archivePrefix = {arXiv}, -arxivId = {1801.00807}, -author = {Mart{\'{i}}n-Navarro, Ignacio and Brodie, Jean P. and Romanowsky, Aaron J. and Ruiz-Lara, Tom{\'{a}}s and {Van De Ven}, Glenn}, -doi = {10.1038/nature24999}, -eprint = {1801.00807}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/MartinNavvro2018RegulatedSF.pdf:pdf}, -issn = {14764687}, -journal = {Nature}, -number = {7688}, -pages = {307--309}, -pmid = {29291597}, -title = {{Black-hole-regulated star formation in massive galaxies}}, -volume = {553}, -year = {2018} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in SPH simulations. About half the gas shock heats to roughly the virial temperature of the galaxy potential well before cooling, condensing, and forming stars, but the other half radiates its acquired gravitational energy at much lower temperatures, typically T{\textless}10{\^{}}5 K, and the histogram of maximum gas temperatures is clearly bimodal. The "cold mode" of gas accretion dominates for low mass galaxies (M{\_}baryon {\textless}10{\^{}}{\{}10.3{\}}Msun or M{\_}halo {\textless}10{\^{}}{\{}11.4{\}}Msun), while the conventional "hot mode" dominates the growth of high mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasi-spherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with cold mode dominating at high redshift and in low density regions today, and hot mode dominating in group and cluster environments at low redshift. Star formation rates closely track accretion rates, and we discuss the physics behind the observed environment and redshift dependence of galactic scale star formation. If we allowed hot accretion to be suppressed by conduction or AGN feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colors of ellipticals and the cutoff of the galaxy luminosity function. The transition between cold and hot accretion at M{\_}h {\$\sim${}} 10{\^{}}{\{}11.4{\}}Msun is similar to that found by Birnboim {\&} Dekel (2003) using 1-d simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. (2003) find a marked shift in galaxy properties. We speculate on connections between these theoretical and observational transitions.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Hopkins2011, -abstract = {We present analytic calculations of angular momentum transport and gas inflow in galaxies, from scales of {\$\sim${}}kpc to deep in the potential of a central black hole (BH). We compare these analytic calculations to numerical simulations and use them to develop a sub-grid model of BH growth that can be incorporated into semi-analytic models or cosmological simulations. Both analytic calculations and simulations argue that the strongest torque on gas arises when non-axisymmetric perturbations to the stellar gravitational potential produces orbit crossings and shocks in the gas. This is true both at large radii {\$\sim${}}0.01-1 kpc, where bar-like modes dominate the non-axisymmetric potential, and at smaller radii {\textless}10 pc, where a lopsided/eccentric disk dominates. The traditional orbit crossing criterion is not always adequate to predict the locations of, and inflow due to, shocks in gas+stellar disks with finite sound speeds. We derive a modified criterion that predicts the presence of shocks in stellar dominated systems even absent formal orbit crossing. We then derive analytic expressions for the loss of angular momentum and the resulting gas inflow rates in the presence of such shocks. We test our analytic predictions using hydrodynamic simulations at a range of galactic scales, and show that they successfully predict the mass inflow rates and quasi-steady gas surface densities with small scatter (0.3 dex). We use our analytic results to construct a new estimate of the BH accretion rate given galaxy properties at larger radii. This captures the key scalings in the numerical simulations. Alternate estimates such as the local viscous accretion rate or the spherical Bondi rate fail systematically to reproduce the simulations.}, -archivePrefix = {arXiv}, -arxivId = {1007.2647}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1365-2966.2011.18542.x}, -eprint = {1007.2647}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Quasars: general}, -number = {2}, -pages = {1027--1050}, -title = {{An analytic model of angular momentum transport by gravitational torques: From galaxies to massive black holes}}, -volume = {415}, -year = {2011} -} -@article{Hopkins2010c, -abstract = {We present a simple estimate of the mass 'deficits' in cored spheroids, as a function of galaxy mass and radius within the galaxy. Previous attempts to measure such deficits depended on fitting some functional form to the profile at large radii and extrapolating inwards; this is sensitive to the assumed functional form and does not allow for variation in nuclear profile shapes. We take advantage of larger data sets to directly construct stellar mass profiles of observed systems and measure the stellar mass enclosed in a series of physical radii (M({\textless}R)), for samples of cusp and core spheroids at the same stellar mass. There is a significant bimodality in this distribution at small radii, and we non-parametrically measure the median offset between core and cusp populations (the deficit Delta{\_}M({\textless}R)). We construct the scoured mass profile as a function of radius, without reference to any assumed functional form. The mass deficit rises in power-law fashion (Delta{\_}M({\textless}R) R{\^{}}{\{}1.3-1.8{\}}) from a significant but small mass at R{\textless}10pc, to asymptote to a maximum {\$\sim${}}0.5-2 M{\_}BH at {\$\sim${}}100pc. At larger radii there is no statistically significant separation between populations; the upper limit to the cumulative scoured mass at {\$\sim${}}kpc is {\$\sim${}}2-4 M{\_}BH. This does not depend strongly on stellar mass. The dispersion in M({\textless}R) appears larger in the core population, possibly reflecting the fact that scouring increases the scatter in profile shapes. These results are in good agreement with models of scouring from BH binary systems.}, -archivePrefix = {arXiv}, -arxivId = {1006.0488}, -author = {Hopkins, Philip F and Hernquist, Lars}, -doi = {10.1111/j.1365-2966.2010.16915.x}, -eprint = {1006.0488}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {447--457}, -title = {{A non-parametric estimate of mass 'scoured' in galaxy cores}}, -url = {http://arxiv.org/abs/1006.0488%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2010.16915.x}, -volume = {407}, -year = {2010} -} -@article{Guo2011, -abstract = {We report the detection of color gradients in massive (stellar mass \nM{\textgreater}10{\textless}SUP{\textgreater}10{\textless}/SUP{\textgreater} Msun) galaxies with low specific star formation \nrate (SSFR{\textless}10{\textless}SUP{\textgreater}-11{\textless}/SUP{\textgreater}/yr) at redshift z 2. The galaxies are \nselected by means of SED fitting to spectral population synthesis models \nusing the Great Observatories Origins Deep Survey (GOODS) broad--band \nphotometry, which spans the optical, near--IR and mid--IR windows, \naugmented by recent ultra--deep near--IR images obtained with HST WFC3. \nThe estimated stellar mass and SSFR would place these galaxies among \ntoday's Hubble early types, while their rest--frame optical morphology, \nas shown by the WFC3 images, is consistent with that of spheroidal \nsystems. The inner regions of these galaxies are found to have redder \nrest UV--optical colors than their outer parts. The slope of the color \ngradient has no obvious dependence on the redshift and stellar mass of \nthe galaxies. It does depend, however, on the overall dust obscuration \nand rest-frame U-V color of the galaxies mildly, with more obscured or \nredder galaxies having steeper color gradient. The slope of the color \ngradient is generally steeper than that of local early-type galaxies. We \nfind that the gradient of a single parameter (age, extinction or \nmetallicity) cannot fully explain the observed color gradient. To study \nthe physical implications of these color gradients, we fit spatially \nresolved HST seven--bands photometry from ACS and WFC3 images (BVizYJH) \nin concentric shells across the light profile of each galaxies, sampling \nthe color gradients. Regardless of the assumed metallicity gradient, the \nredder inner regions always have slightly higher dust obscuration than \nthe bluer outer regions, implying that a dust gradient may partly \ncontribute to the observed color gradients. Because of the \nage--metallicity degeneracy, the derived age gradient is coupled with \nthe assumed metallicity gradient. We discuss the plausibility and \nimplication of each derived age gradient.}, -author = {Guo, Yicheng and Giavalisco, M and Cassata, P and Koekemoer, A}, -journal = {Bulletin of the {American} {Astronomical} {Society}}, -pages = {18}, -title = {{Color {Gradients} and {Stellar} {Population} {Gradients} of {Early}-type {Galaxies} at z 2 in the {Hubble} {Ultra} {Deep} {Field}}}, -url = {http://cdsads.u-strasbg.fr/abs/2011AAS...21733503G}, -volume = {217}, -year = {2011} -} -@article{Lilly2016, -abstract = {There are very strong observed correlations between the specific star formation rates (sSFRs) of galaxies and their mean surface mass densities, {\$}\Sigma{\$}, as well as other aspects of their internal structure. These strong correlations have often been taken to argue that the internal structure of a galaxy must play a major physical role, directly or indirectly, in the control of star formation. In this paper we show by means of a very simple toy model that these correlations can arise naturally without any such physical role once the observed evolution of the size–mass relation for star-forming galaxies is taken into account. In particular, the model reproduces the sharp threshold in {\$}\Sigma{\$}between galaxies that are star-forming and those that are quenched and the evolution of this threshold with redshift. Similarly, it produces iso-quenched-fraction contours in the f Q (m, R e) plane that are almost exactly parallel to lines of constant {\$}\Sigma{\$}for centrals and shallower for satellites. It does so without any dependence on quenching on size or {\$}\Sigma{\$}and without invoking any differences between centrals and satellites, beyond the different mass dependences of their quenching laws. The toy model also reproduces several other observations, including the sSFR gradients within galaxies and the appearance of inside-out build-up of passive galaxies. Finally, it is shown that curvature in the main-sequence sSFR–mass relation can produce curvature in the apparent B/T ratios with mass. Our analysis therefore suggests that many of the strong correlations that are observed between galaxy structure and sSFR may well be a consequence of things unrelated to quenching and should not be taken as evidence of the physical processes that drive quenching.}, -archivePrefix = {arXiv}, -arxivId = {1604.06459}, -author = {Lilly, Simon J and Carollo, C Marcella}, -doi = {10.3847/0004-637X/833/1/1}, -eprint = {1604.06459}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {1}, -pmid = {15540530}, -title = {{Surface Density Effects in Quenching: Cause or Effect?}}, -url = {http://stacks.iop.org/0004-637X/833/i=1/a=1?key=crossref.e8eb282687d660fdf733577b98c3d5a7}, -volume = {833}, -year = {2016} -} -@article{DiMauro2014, -abstract = {Millisecond pulsars (MSPs) are old fast-spinning neutron stars that represent the second most abundant source population discovered by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope (Fermi). As guaranteed $\gamma$-ray emitters, they might contribute non-negligibly to the diffuse emission measured at high latitudes by Fermi-LAT (i.e., the Isotropic Diffuse $\gamma$-Ray Background (IDGRB)), which is believed to arise from the superposition of several components of galactic and extragalactic origin. Additionally, $\gamma$-ray sources also contribute to the anisotropy of the IDGRB measured on small scales by Fermi-LAT. In this manuscript we aim to assess the contribution of the unresolved counterpart of the detected MSPs population to the IDGRB and the maximal fraction of the measured anisotropy produced by this source class. To this end, we model the MSPs' spatial distribution in the Galaxy and the $\gamma$-ray emission parameters by considering observational constraints coming from the Australia Telescope National Facility pulsar catalog and the Second Fermi-LAT Catalog of $\gamma$-ray pulsars. By simulating a large number of MSP populations through a Monte Carlo simulation, we compute the average diffuse emission and the anisotropy 1$\sigma$ upper limit. We find that the emission from unresolved MSPs at 2 GeV, where the peak of the spectrum is located, is at most 0.9% of the measured IDGRB above 10° in latitude. The 1$\sigma$ upper limit on the angular power for unresolved MSP sources turns out to be about a factor of 60 smaller than Fermi-LAT measurements above 30°. Our results indicate that this galactic source class represents a negligible contributor to the high-latitude $\gamma$-ray sky and confirm that most of the intensity and geometrical properties of the measured diffuse emission are imputable to other extragalactic source classes (e.g., blazars, misaligned active galactic nuclei, or star-forming galaxies). Nevertheless, because MSPs are more concentrated toward the galactic center, we expect them to contribute significantly to the $\gamma$-ray diffuse emission at low latitudes. Because, along the galactic disk, the population of young pulsars overcomes in number that of MSPs, we compute the $\gamma$-ray emission from the whole population of unresolved pulsars, both young and millisecond, in two low-latitude regions: the inner Galaxy and the galactic center.}, -archivePrefix = {arXiv}, -arxivId = {1406.2706}, -author = {Calore, F. and {Di Mauro}, M. and Donato, F.}, -doi = {10.1088/0004-637X/796/1/14}, -eprint = {1406.2706}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {gamma rays: diffuse background}, -number = {1}, -pages = {14}, -title = {{Diffuse $\gamma$-ray emission from galactic pulsars}}, -url = {http://stacks.iop.org/0004-637X/796/i=1/a=14?key=crossref.f8fce2f05305d1112c8bc78e23f499d0}, -volume = {796}, -year = {2014} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani} and Caldwell, Nelson}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Governato2015, -abstract = {We use high-resolution Hydro+N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass {\$\sim${}}106-7 M⊙, total mass 1010 M⊙) in $\Lambda$-dominated cold dark matter (CDM) and 2 keV warm dark matter (WDM) cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the dark matter (DM) model, but proportionally to the SF efficiency, gas outflows lower the central mass density through 'dynamical heating', such that all realizations have circular velocities {\textless} 20 km s-1 at 500 pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial colour- magnitude diagrams and star formation histories (SFHs) in order to directly compare to available observations. The simulated galaxies formed most of their stars in many {\$\sim${}}10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including 'baryon physics' in simulations when (1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and (2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F and Weisz, D and Pontzen, A and Loebman, S and Reed, D and Brooks, A M and Behroozi, P and Christensen, C and Madau, P and Mayer, L and Shen, S and Walker, M and Quinn, T and Keller, B W and Wadsley, J}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, n=10[cm-3], results in strong expansion of the DM halo in galaxies with stellar masses in the range 107.5 ≤ Mstar ≤ 109.5 M⊙. We find that lower thresholds such as n = 0.1 (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e. ≤50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with n = 10 have gas fractions of ∼0.2 and variations of ∼0.1, while n = 0.1 simulations have order of magnitude lower gas fractions and hence do not expand the halo. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with n = 0.1 and n = 1, but in a reasonable agreement with n = 10. Star formation rates are more variable for higher n, lower galaxy masses, and when star formation is measured on shorter time-scales. For example, simulations with n = 10 have up to 0.4 dex higher scatter in specific star formation rates than simulations with n = 0.1. Thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625}, -author = {Dutton, Aaron A and MacCi{\`{o}}, Andrea V and Buck, Tobias and Dixon, Keri L and Blank, Marvin and Obreja, Aura}, -doi = {10.1093/mnras/stz889}, -eprint = {1811.10625}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure,methods: numerical}, -number = {1}, -pages = {655--671}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://arxiv.org/abs/1811.10625%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stz889}, -volume = {486}, -year = {2019} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 {\textless} z {\textless} 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J{\textless}inf{\textgreater}125{\textless}/inf{\textgreater}, i{\textless}inf{\textgreater}814{\textless}/inf{\textgreater}, v{\textless}inf{\textgreater}606{\textless}/inf{\textgreater} HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.1736}, -volume = {444}, -year = {2014} -} -@article{Graham2001b, -abstract = {We present evidence for a strong correlation between the concentration of bulges and the mass of their central supermassive black hole (Mbh)-more concentrated bulges have more massive black holes. Using Cre(1/3) from Trujillo, Graham, & Caon as a measure of bulge concentration, we find that log(Mbh/Msolar)=6.81(+/- 0.95)Cre(1/3)+5.03+/-0.41. This correlation is shown to be marginally stronger (Spearman's rs=0.91) than the relationship between the logarithm of the stellar velocity dispersion and logMbh (Spearman's rs=0.86) and has comparable or less scatter (0.31 dex in logMbh, which decreases to 0.19 dex when we use only those galaxies whose supermassive black hole radii of influence are resolved and we remove one well-understood outlying data point).}, -author = {Graham, Alister W. and Erwin, Peter and Caon, N. and Trujillo, I.}, -doi = {10.1086/338500}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Grapham2001SMBHSersic.pdf:pdf}, -issn = {0004637X}, -journal = {ApJ}, -number = {1}, -pages = {L11--L14}, -title = {{A Correlation between Galaxy Light Concentration and Supermassive Black Hole Mass}}, -volume = {563}, -year = {2001} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently-discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially-interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorised according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}10{\^{}}11 Msun to {\textgreater}10{\^{}}13 Msun. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}10{\^{}}11 Msun. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW05). The two low-mass outliers are J0206-095 (SW19) and J2217+015 (SW42); if these two are indeed lenses, they probe an interesting regime of very low star-formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Li2018a, -abstract = {We investigate the discrepancy between the two-dimensional projected lensing mass and the dynam- ical mass for an ensemble of 97 strong gravitational lensing systems discovered by the Sloan Lens ACS (SLACS) Survey, the BOSS Emission-Line Lens Survey (BELLS), and the BELLS for GALaxy-Ly{\alpha} EmitteR sYs- tems (BELLS GALLERY) Survey. We fit the lensing data to obtain the Einstein mass, and use the velocity dispersion of the lensing galaxies provided by the Sloan Digital Sky Survey (SDSS) to get the projected dynamical mass within the Einstein radius by assuming the power-law mass approximation. The discrepancy is found to be obvious and quantified by Bayesian analysis. For the singular isothermal sphere (SIS) mass model, we obtain that the Einstein mass is 20.7% more than the dynamical mass, and the discrepancy increases with the redshift of the lensing galaxies. For more general power-law mass model, the discrepancy still exists within 1{\sigma} credible region. The main reason of the the discrepancy could be mass contamination, including all invisible masses along the line of sight. In addition, the measurement errors and the approximation of the mass models could lead to part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1803.00819}, -author = {Li, Rui and Wang, Jiancheng and Shu, Yiping and Xu, Zhaoyi}, -doi = {10.3847/1538-4357/aaab50}, -eprint = {1803.00819}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Li et al. - 2018 - The Discrepancy between Einstein Mass and Dynamical Mass for SIS and Power-law Mass Models.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {64}, -title = {{The Discrepancy between Einstein Mass and Dynamical Mass for SIS and Power-law Mass Models}}, -url = {http://arxiv.org/abs/1803.00819%0Ahttp://dx.doi.org/10.3847/1538-4357/aaab50}, -volume = {855}, -year = {2018} -} -@article{Sahu2019, -abstract = {Analyzing a sample of 84 early-type galaxies with directly-measured super-massive black hole masses---nearly doubling the sample size of such galaxies with multi-component decompositions---a symmetric linear regression on the reduced (merger-free) sample of 76 galaxies reveals $M_{BH}\propto M_{*,sph}^{1.27\pm 0.07}$ with a total scatter of $\Delta_{rms}=$ 0.52 dex in the $\log(M_{BH})$ direction. However, and importantly, we discover that the ES/S0-type galaxies with disks are offset from the E-type galaxies by more than a factor of ten in their $M_{BH}/M_{*,sph}$ ratio, with ramifications for formation theories, simulations, and some virial factor measurements used to convert AGN virial masses into $M_{BH}$. Separately, each population follows a steeper relation with slopes of $1.86\pm0.20$ and $1.90\pm0.20$, respectively. The offset mass ratio is mainly due to the exclusion of the disk mass, with the two populations offset by only a factor of two in their $M_{BH}/M_{*,gal}$ ratio in the $M_{BH}$-$M_{*,gal}$ diagram where $M_{BH}\propto M_{*,gal}^{1.8\pm 0.2}$ and $\Delta_{rms}=0.6\pm 0.1$ dex depending on the sample. For $M_{BH} \gtrsim 10^7 M_{\odot}$, we detect no significant bend nor offset in either the $M_{BH}$-$M_{*,sph}$ or $M_{BH}$-$M_{*,gal}$ relations due to barred versus non-barred, or core-S\'ersic versus S\'ersic, early-type galaxies. For reference, the ensemble of late-type galaxies (which invariably are S\'ersic galaxies) follow $M_{BH}$-$M_{*,sph}$ and $M_{BH}$-$M_{*,gal}$ relations with slopes equal to $2.16\pm 0.32$ and $3.05\pm 0.70$, respectively. Finally, we provide some useful conversion coefficients, $\upsilon$, accounting for the different stellar mass-to-light ratios used in the literature, and we report the discovery of a local, compact massive spheroid in NGC 5252.}, -archivePrefix = {arXiv}, -arxivId = {1903.04738}, -author = {Sahu, Nandini and Graham, Alister W. and Davis, Benjamin L.}, -doi = {10.3847/1538-4357/ab0f32}, -eprint = {1903.04738}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sahu, Graham, Davis - 2019 - Black Hole Mass Scaling Relations for Early-type Galaxies. I. M BH – M , sph and M BH – M ,gal.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {black hole physics,bulges,cd,elliptical and lenticular,evolution,galaxies,photometry,structure}, -number = {2}, -pages = {155}, -title = {{ Black Hole Mass Scaling Relations for Early-type Galaxies. I. M BH – M *, sph and M BH – M *,gal }}, -volume = {876}, -year = {2019} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z > 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G.}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2006 - Breaking the hierarchy of galaxy formation(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -publisher = {MNRAS}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high-resolution N-body simulations of galactic dark matter haloes to test if this remarkable property can be understood within the context of the cold dark matter (CDM) cosmology. We construct halo merger trees from the simulations and use a semi-analytic model to follow the formation of satellite galaxies. We find that in all six of our simulations, the 11 brightest satellites are indeed distributed along thin, disc-like structures analogous to that traced by the satellites of the Milky Way. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhaloes within it, which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhaloes but is similar to that of the subset of subhaloes that had the most massive progenitors at earlier times. The elongated disc-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I and Frenk, Carlos S and Cole, Shaun and Helly, John C and Jenkins, Adrian and Navarro, Julio F and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Murray2013, -abstract = {A multi-level clocking scheme has been developed to improve the parallel CTE of four-phase CCDs by suppressing the effects of traps located in the transport channel under barrier phases by inverting one of these phases throughout the transfer sequence. In parallel it was apparent that persistence following optical overload in Euclid VIS detectors would lead to undesirable signal released in subsequent rows and frames and that a suitable scheme for flushing this signal would be required. With care, the negatively biased electrodes during the multi-level transfer sequence can be made to pin the entire surface, row-by-row, and annihilate the problematic charges. This process can also be extended for use during integration to significantly reduce the unusable area of the detector, as per the clocked anti-blooming techniques developed many years ago; however, with the four-phase electrodes architecture of modern CCDs, we can take precautionary measures to avoid the problem of charge pumping and clock induced charge within the science frames. Clock induced charge is not all bad! We also propose the use of on-orbit trap-pumping for Euclid VIS to provide calibration input to ground based correction algorithms and as such a uniform, low noise background is require. Clock induced charge can be manipulated to provide a very suitable, low signal and noise background to the imaging array. Here we describe and present results of multi-level parallel clocking schemes for use in four-phase CCDs that could improve performance of high precision astronomy applications such as Euclid VIS. ? 2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Holland, Andrew D and Stefanov, Konstantin D and Gow, Jason P D and MacCormick, Calum and Dryer, Ben J and Allanwood, Edgar A H}, -doi = {10.1117/12.2024839}, -isbn = {9780819497109}, -issn = {0277786X 1996756X}, -journal = {Proceedings of SPIE - The International Society for Optical Engineering}, -keywords = {Blooming,CAB,CCD,CIC,CTE,Euclid VIS,Mu,[BFW}, -pages = {88600K}, -title = {{Multi-level parallel clocking of CCDs for: improving charge transfer efficiency, clearing persistence, clocked anti-blooming, and generating low-noise backgrounds for pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024839}, -volume = {8860}, -year = {2013} -} -@article{Griffiths2019, -abstract = {We report an embarrassingly parallel method for the evaluation of thermodynamic properties over an energy landscape exhibiting broken ergodicity, nested is the likelihood of the observed data D givenbasin-sampling (NBS). We also introduce the No Galilean U-Turn Sampler (NoGUTS), a new sampling scheme based on the No U-Turn Sampler (NUTS) introduced by Hoffman and Gelman (2014) that works with the Galilean Monte Carlo scheme introduced by Betancourt (2012) to aid the efficient generation of new live points. NoGUTS can be thought of as a form of reflective slice sampling with an automatic stopping criterion. We apply this approach to a benchmark atomic cluster of 31 Lennard-Jones atoms, which exhibits a low temperature solid-solid heat capacity peak. The calculated heat capacity is compared with results generated by parallel tempering (PT), basin-sampling parallel tempering (BSPT), and standard nested sampling (NS) simulations. NBS reproduces the full heat capacity curve predicted by PT and BSPT, while the NS calculation with similar computational cost fails to resolve the low-temperature solid-solid phase transition.}, -author = {Griffiths, Matthew and Wales, David J}, -doi = {10.1021/acs.jctc.9b00567}, -issn = {15499626}, -journal = {Journal of Chemical Theory and Computation}, -number = {12}, -pages = {6865--6881}, -title = {{Nested Basin-Sampling}}, -volume = {15}, -year = {2019} -} -@article{VanDeVyvere2022a, -abstract = {In the context of gravitational lensing, the density profile of lensing galaxies is often considered to be perfectly elliptical. Potential angular structures are generally ignored, except to explain flux ratios of point-like sources (i.e. flux ratio anomalies). Surprisingly, the impact of azimuthal structures on extended images of the source has not been characterised, nor has its impact on the H0 inference. We address this task by creating mock images of a point source embedded in an extended source and lensed by an elliptical galaxy on which multipolar components are added to emulate boxy or discy isodensity contours. Modelling such images with a density profile free of angular structure allows us to explore the detectability of image deformation induced by the multipoles in the residual frame. Multipole deformations are almost always detectable for our highest signal-To-noise ratio (S/N) mock data. However, the detectability depends on the lens ellipticity and Einstein radius, on the S/N of the data, and on the specific lens modelling strategy. Multipoles also introduce small changes to the time-delays. We therefore quantify how undetected multipoles would impact H0 inference. When no multipoles are detected in the residuals, the impact on H0 for a given lens is in general less than a few km s, but in the worst-case scenario, combining low S/N in the ring and large intrinsic boxyness or discyness, the bias on H0 can reach 10a. If we now look at the inference on H0 from a population of lensing galaxies with a distribution of multipoles representative of what is found in the light profile of elliptical galaxies, we find a systematic bias on H0 of less than 1%. A comparison of our mock systems to the state-of-The-Art time-delay lens sample studied by the H0LiCOW and TDCOSMO collaborations indicates that multipoles are currently unlikely to be a source of substantial systematic bias on the inferred value of H0 from time-delay lenses.}, -archivePrefix = {arXiv}, -arxivId = {2112.03932}, -author = {{Van De Vyvere}, Lyne and Gomer, Matthew R. and Sluse, Dominique and Xu, Dandan and Birrer, Simon and Galan, Aymeric and Vernardos, Georgios}, -doi = {10.1051/0004-6361/202141551}, -eprint = {2112.03932}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/vandevyree2022BoxynessDiscyness.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Cosmological parameters,Galaxies: structure,Gravitational lensing: strong}, -pages = {1--21}, -title = {{TDCOSMO: VII. Boxyness/discyness in lensing galaxies: Detectability and impact on H 0}}, -volume = {659}, -year = {2022} -} -@article{Sales2012, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Wang2014a, -abstract = {Charged Coupled Devices (CCDs) have been successfully used in several low energy X-ray astronomical satellites over the past two decades. Their high energy resolution and high spatial resolution make them a perfect tool for low energy astronomy, such as observing the formation of galaxy clusters and the environment around black holes. The Low Energy X-ray Telescope (LE) group is developing a Swept Charge Device (SCD) for the Hard X-ray Modulation Telescope (HXMT) satellite. A SCD is a special low energy X-ray CCD, which can be read out a thousand times faster than traditional CCDs, simultaneously keeping excellent energy resolution. A test method for measuring the charge transfer efficiency (CTE) of a prototype SCD has been set up. Studies of the charge transfer inefficiency (CTI) with a proton-irradiated SCD have been performed at a range of operating temperatures. The SCD is irradiated by 3 × 10 8cm-2 10 MeV protons. {\textcopyright}2014 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1308.1698}, -author = {Wang, Yu Sa and Yang, Yan Ji and Chen, Yong and Liu, Xiao Yan and Cui, Wei Wei and Xu, Yu Peng and Li, Cheng Kui and Li, Mao Shun and Han, Da Wei and Chen, Tian Xiang and Huo, Jia and Wang, Juan and Li, Wei and Hu, Wei and Zhang, Yi and Lu, Bo and Yin, Guo He and Zhu, Yue and Zhang, Zi Liang}, -doi = {10.1088/1674-1137/38/6/066001}, -eprint = {1308.1698}, -issn = {16741137}, -journal = {Chinese Physics C}, -keywords = {CCD,CTE,CTI,HXMT,LE,SCD,proton-irradiated}, -number = {6}, -pages = {66001}, -title = {{Measurements of charge transfer efficiency in a proton-irradiated swept charge device}}, -url = {http://stacks.iop.org/1674-1137/38/i=6/a=066001?key=crossref.02a5cb134fd3859a1cfa309d04df9b61}, -volume = {38}, -year = {2014} -} -@article{Metcalf2018, -abstract = {Large-scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images, and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects, reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100 000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. Having multi-band, ground based data is found to be better for this purpose than single-band space based data with lower noise and higher resolution, suggesting that multi-colour data is crucial. Multi-band space based data will be superior to ground based data. The most difficult challenge for a lens finder is differentiating between rare, irregular and ring-like face-on galaxies and true gravitational lenses. The degree to which the efficiency and biases of lens finders can be quantified largely depends on the realism of the simulated data on which the finders are trained.}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R B and Meneghetti, M and Avestruz, C and Bellagamba, F and Bom, C R and Bertin, E and Cabanac, R and Courbin, F and Davies, A and Decenci{\`{e}}re, E and Flamary, R and Gavazzi, R and Geiger, M and Hartley, P and Huertas-Company, M and Jackson, N and Jacobs, C and Jullo, E and Kneib, J P and Koopmans, L V E and Lanusse, F and Li, C L and Ma, Q and Makler, M and Li, N and Lightman, M and Petrillo, C E and Serjeant, S and Sch{\"{a}}fer, C and Sonnenfeld, A and Tagore, A and Tortora, C and Tuccillo, D and Valent{\'{i}}n, M B and Velasco-Forero, S and {Verdoes Kleijn}, G A and Vernardos, G}, -doi = {10.1051/0004-6361/201832797}, -eprint = {1802.03609}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Gravitational lensing: strong - methods: data anal}, -title = {{The strong gravitational lens finding challenge}}, -url = {http://arxiv.org/abs/1802.03609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201832797}, -volume = {625}, -year = {2019} -} -@article{Jaroszynski2012, -abstract = {We investigate strong lensing by non-singular finite isothermal ellipsoids taking into account the influence of the matter along the line of sight and in the close lens vicinity. We compare three descriptions of light propagation: the full approach taking into account all matter inhomogeneities along the rays; the single plane approach, where we take into account the influence of the strong lens neighbours but neglect the foreground and background objects; and the single lens approach. In each case, we simulate many strong lensing configurations placing a point source at the same redshift but in different locations inside the region surrounded by caustics. We further analyse configurations of four or five images. For every simulated strong lensing configuration, we attempt to fit a simplified lens model using a single isothermal ellipsoid or a single isothermal ellipsoid with external shear. The single lens fits to configurations obtained in the full approach are rejected in majority of cases with 95per cent significance. For configurations obtained in the single plane approach, the rejection rate is substantially lower. Also the inclusion of external shear in simplified modelling improves the chances of obtaining acceptable fits, but the problem is not solved completely. The quantitative estimates of the rates of rejection of simplified models depend on the required accuracy of the models, and we present few illustrative examples, which show that both matter close to the lens and matter along the rays do have important influence on lens modelling. We also estimate the typical value of the external shear and compare the fitted parameters of the simplified models with the parameters of the lenses used in the simulations. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1204.6223}, -author = {Jaroszynski, M and Kostrzewa-Rutkowska, Z}, -doi = {10.1111/j.1365-2966.2012.21197.x}, -eprint = {1204.6223}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: strong,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {1}, -pages = {325--332}, -title = {{Background, foreground and nearby matter influence on strong gravitational lenses}}, -volume = {424}, -year = {2012} -} -@inproceedings{MartinNavarro2013, -abstract = {We have developed an innovative 'index scanning technique” to map the stellar kinematics of early-type galaxies by measuring for the first time the absorption line strength of the near-IR CaII triplet with the Red Tunable Filters of OSIRIS at GTC. Unlike classical spectroscopy, these filters allow us to perform a two-dimensional study, taking advantage of a 10.4 meter class telescope with a unvignetted field of view of 7.8 × 7.8 arcmin. We show the velocity fields obtained for two Virgo elliptical galaxies of very different masses and their globular cluster systems reaching galactocentric distances beyond 2 effective radii.}, -author = {Mart{\'{i}}n-Navarro, Ignacio and Vazdekis, Alexander and Bongiovanni, {\'{A}}ngel and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and Cepa, Jordi and Cenarro, Javier and S{\'{a}}nchez-Bl{\'{a}}zquez, Patricia}, -booktitle = {Proceedings of the 10th Scientific Meeting of the Spanish Astronomical Society - Highlights of Spanish Astrophysics VII, SEA 2012}, -editor = {Guirado, J.$\sim$C. and Lara, L.$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable filters at gtc: A novel approach}}, -year = {2020} -} -@article{Navarro1997, -abstract = {We use high-resolution N-body simulations to study the equilibrium density profiles of dark matter halos in hierarchically clustering universes. We find that all such profiles have the same shape, independent of halo mass, of initial density fluctuation spectrum, and of the values of the cosmological parameters. Spherically averaged equilibrium profiles are well fit over two decades in radius by a simple formula originally proposed to describe the structure of galaxy clusters in a cold dark matter universe. In any particular cosmology the two scale parameters of the fit, the halo mass and its characteristic density, are strongly correlated. Low-mass halos are significantly denser than more massive systems, a correlation which reflects the higher collapse redshift of small halos. The characteristic density of an equilibrium halo is proportional to the density of the universe at the time it was assembled. A suitable definition of this assembly time allows the same proportionality constant to be used for all the cosmologies that we have tested. We compare our results to previous work on halo density profiles and show that there is good agreement. We also provide a step-by-step analytic procedure, based on the Press-Schechter formalism, which allows accurate equilibrium profiles to be calculated as a function of mass in any hierarchical model.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9611107}, -author = {Navarro, Julio F. and Frenk, Carlos S. and White, Simon D. M.}, -doi = {10.1086/304888}, -eprint = {9611107}, -isbn = {0004-637X}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Cosmology: Dark Matter,Cosmology: Theory,Galaxies: Halos,Methods: Numerical}, -month = {dec}, -number = {2}, -pages = {493--508}, -primaryClass = {astro-ph}, -title = {{A Universal Density Profile from Hierarchical Clustering}}, -url = {http://arxiv.org/abs/astro-ph/9611107}, -volume = {490}, -year = {1997} -} -@article{Reynolds2015, -abstract = {Compact radio sources sometimes exhibit intervals of large, rapid changes in their flux-density, due to lensing by interstellar plasma crossing the line-of-sight. A novel survey program has made it possible to discover these "Extreme Scattering Events" (ESEs) in real time, resulting in a high-quality dynamic spectrum of an ESE observed in PKS 1939-315. Here we present a method for determining the column-density profile of a plasma lens, given only the dynamic radio spectrum of the lensed source, under the assumption that the lens is either axisymmetric or totally anisotropic. Our technique relies on the known, strong frequency dependence of the plasma refractive index in order to determine how points in the dynamic spectrum map to positions on the lens. We apply our method to high-frequency (4.2-10.8 GHz) data from the Australia Telescope Compact Array of the PKS 1939-315 ESE. The derived electron column-density profiles are very similar for the two geometries we consider, and both yield a good visual match to the data. However, the fit residuals are substantially above the noise level, and deficiencies are evident when we compare the predictions of our model to lower-frequency (1.6-3.1 GHz) data on the same ESE, thus motivating future development of more sophisticated inversion techniques.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1512.03411}, -author = {Tuntsov, Artem V and Walker, Mark A and Koopmans, Leon V E and Bannister, Keith W and Stevens, Jamie and Johnston, Simon and Reynolds, Cormac and Bignall, Hayley E}, -doi = {10.3847/0004-637X/817/2/176}, -eprint = {1512.03411}, -issn = {15384357}, -number = {December}, -title = {{Dynamic spectral mapping of interstellar plasma lenses}}, -url = {http://arxiv.org/abs/1512.03411%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/2/176}, -year = {2015} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work conducted to interpret this phenomenon has found that it is due to the non-spherical nature of dark matter halos. However, most studies overpredict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shapes of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations where satellite galaxies without associated subhalos ("orphan galaxies") are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region. {\textcopyright}2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W P and Kang, X and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%7B%5C%25%7D5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem%7B%5C&%7Dsid=IOPP%7B%5C%25%7D3Ajnl%7B%5C_%7Dref%7B%5C&%7Dspage=305%7B%5C&%7Dtitle=ArA%7B%5C&%7Dvolume=5%7B%5C&%7Ddate=1969%7B%5C&%7Dv%7B%5C}, -volume = {786}, -year = {2014} -} -@article{Ding2018a, -abstract = {Strong gravitational lenses with measured time delay are a powerful tool to measure cosmological parameters, especially the Hubble constant ($H_0$). Recent studies show by combining just three multiply-imaged AGN systems, one can determine $H_0$ down to 3% precision. Furthermore, the number of time-delay lens is growing rapidly, enabling the determination of $H_0$ to 1% precision in the near future. However, it is important to ensure that systematic errors and biases remain subdominant. For this purpose, challenges with simulated datasets are a key component. Following the experience of the past challenge on time delay, where it was shown that time delays can be measured precisely and accurately at the sub-percent level, we now present the "Time Delay Lens Modeling Challenge" (TDLMC). The goal of TDLMC is to assess the present capabilities of lens modeling codes and assumptions and test the level of accuracy of inferred cosmological parameters given realistic mock datasets. We invite scientists to model a set of simulated HST observations of 50 mock lens systems. The systems are organized in rungs, with the complexity and realism increasing going up the ladder. The goal of the challenge is to infer $H_0$ for each rung, given the HST images, the time delay, and a stellar velocity dispersion of the deflector, for a fixed background cosmology. The TDLMC challenge will start with the mock data release on 2018 January 8th. The deadline for blind submission is different for each rung. The deadline for Rung0-1 is 2018 Sept. 8; the deadline for Rung2 is 2019 Apr. 8 and the one for Rung3 is 2019 Sept. 8. This first paper gives an overview of the challenge including the data design, and a set of metrics to quantify the modeling performance and challenge details. After the deadline, the results of the challenge will be presented in a companion paper with all challenge participants as co-authors.}, -archivePrefix = {arXiv}, -arxivId = {1801.01506}, -author = {Ding, Xuheng and Treu, Tommaso and Shajib, Anowar J. and Xu, Dandan and Chen, Geoff C. -F. and More, Anupreeta and Despali, Giulia and Frigo, Matteo and Fassnacht, Christopher D. and Gilman, Daniel and Hilbert, Stefan and Marshall, Philip J. and Sluse, Dominique and Vegetti, Simona}, -eprint = {1801.01506}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ding et al. - 2018 - Time Delay Lens Modeling Challenge I. Experimental Design(2).pdf:pdf}, -title = {{Time Delay Lens Modeling Challenge: I. Experimental Design}}, -url = {http://arxiv.org/abs/1801.01506}, -year = {2018} -} -@article{Bose2016, -abstract = {The recent detection of a 3.5 keV X-ray line from the centres of galaxies and clusters by Bulbul et al. and Boyarsky et al. has been interpreted as emission from the decay of 7 keV sterile neutrinos which could make up the (warm) dark matter (WDM). As part of the Copernicus Complexio (COCO) programme, we investigate the properties of dark matter haloes formed in a high-resolution cosmological N-body simulation from initial conditions similar to those expected in a universe in which the dark matter consists of 7 keV sterile neutrinos. This simulation and its cold dark matter (CDM) counterpart have $\sim$13.4 bn particles, each of mass $\sim$105 h-1M⊙, providing detailed information about halo structure and evolution down to dwarf galaxy mass scales. Non-linear structure formation on small scales (M200 ≲2 × 109 h-1M⊙) begins slightly later in COCO-WARM than in COCO-COLD. The halo mass function at the present day in theWDM model begins to drop below its CDM counterpart at a mass $\sim$2 × 109 h-1M⊙ and declines very rapidly towards lower masses so that there are five times fewer haloes of mass M200 = 108 h-1M⊙ in COCO-WARM than in COCO-COLD. Halo concentrations on dwarf galaxy scales are correspondingly smaller in COCO-WARM, and we provide a simple functional form that describes its evolution with redshift. The shapes of haloes are similar in the two cases, but the smallest haloes in COCO-WARM rotate slightly more slowly than their CDM counterparts.}, -archivePrefix = {arXiv}, -arxivId = {1507.01998}, -author = {Bose, Sownak and Hellwing, Wojciech A. and Frenk, Carlos S. and Jenkins, Adrian and Lovell, Mark R. and Helly, John C. and Li, Baojiu}, -doi = {10.1093/mnras/stv2294}, -eprint = {1507.01998}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Methods: numerical}, -month = {jan}, -number = {1}, -pages = {318--333}, -title = {{The Copernicus Complexio: Statistical properties of warm dark matter haloes}}, -volume = {455}, -year = {2016} -} -@article{Bose2017, -abstract = {We use the Copernicus Complexio (COCO) high-resolution N-body simulations to investigate differences in the properties of small-scale structures in the standard cold dark matter (CDM) model and in a model with a cutoff in the initial power spectrum of density fluctuations consistent with both a thermally produced warm dark matter (WDM) particle with a rest mass of 3.3 keV and a sterile neutrino with mass 7 keV and leptogenesis parameter L6 = 8.7. The latter corresponds to the 'coldest' model with this sterile neutrino mass compatible with the identification of the recently detected 3.5 keV X-ray line as resulting from particle decay. CDM and WDM predict very different number densities of subhaloes with mass ≲ 109 h-1M⊙ although they predict similar, nearly universal, normalized subhalo radial density distributions. Haloes and subhaloes in both models have cuspy Navarro-Frenk-White profiles, but WDM subhaloes below the cut-off scale in the power spectrum (corresponding to maximum circular velocities V maxz=0 ≤ 50 kms-1) are less concentrated than their CDM counterparts. We make predictions for observable properties using the GALFORM semi-analytic model of Galaxy formation. Both models predict Milky Way satellite luminosity functions consistent with observations, although the WDM model predicts fewer very faint satellites. This model, however, predicts slightly more UV bright galaxies at redshift z > 7 than CDM, but both are consistent with observations. Gravitational lensing offers the best prospect of distinguishing between the models.}, -archivePrefix = {arXiv}, -arxivId = {1604.07409}, -author = {Bose, Sownak and Hellwing, Wojciech A. and Frenk, Carlos S. and Jenkins, Adrian and Lovell, Mark R. and Helly, John C. and Li, Baojiu and Gonzalez-Perez, Violeta and Gao, Liang}, -doi = {10.1093/mnras/stw2686}, -eprint = {1604.07409}, -file = {:C\:/Users/Jammy/Documents/Papers/DarkMatterModels/Bose2016WDMSims.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: high redshift,Methods: numerical}, -number = {4}, -pages = {4520--4533}, -title = {{Substructure and galaxy formation in the Copernicus Complexio warm dark matter simulations}}, -volume = {464}, -year = {2017} -} -@article{RomanoDiaz2010, -abstract = {We compare the substructure evolution in pure dark matter (DM) halos with those in the presence of baryons, hereafter PDM and BDM models, respectively. The prime halos have been analyzed in the previous work. Models have been evolved from identical initial conditions which have been constructed by means of the constrained realization method. The BDM model includes star formation and feedback from stellar evolution onto the gas. A comprehensive catalog of subhalo populations has been compiled and individual and statistical properties of subhalos analyzed, including their orbital differences. We find that subhalo population mass functions in PDM and BDM are consistent with a single power law, M $\alpha$sbh, for each of the models in the mass range of ∼ 2 × 108 M ⊙-2 × 1011 M ⊙. However, we detect a nonnegligible shift between these functions, the time-averaged $\alpha$ ∼ -0.86 for the PDM and -0.98 for the BDM models. Overall, $\alpha$ appears to be a nearly constant in time, with variations of ± 15%. Second, we find that the radial mass distribution of subhalo populations can be approximated by a power law, with a steepening that occurs at the radius of a maximal circular velocity, R vmax, in the prime halos. Here we find that $\gamma$sbh ∼ -1.5 for the PDM and -1 for the BDM models, when averaged over time inside R vmax. The slope is steeper outside this region and approaches -3. We detect little spatial bias (less than 10%) between the subhalo populations and the DM distribution of the main halos. Also, the subhalo population exhibits much less triaxiality in the presence of baryons, in tandem with the shape of the prime halo. Finally, we find that, counter-intuitively, the BDM population is depleted at a faster rate than the PDM one within the central 30kpc of the prime halo. The reason for this is that although the baryons provide a substantial glue to the subhalos, the main halo exhibits the same trend. This assures a more efficient tidal disruption of the BDM subhalo population. However, this effect can be reversed for a more efficient feedback from stellar evolution and the central supermassive black holes, which will expel baryons from the center and decrease the central concentration of the prime halo. We compare our results with via Lactea and Aquarius simulations and other published results. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1002.4200}, -author = {Romano-D{\'{i}}az, Emilio and Shlosman, Isaac and Heller, Clayton and Hoffman, Yehuda}, -doi = {10.1088/0004-637X/716/2/1095}, -eprint = {1002.4200}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: interactions,Galaxies: kinematics and dynamics}, -month = {jun}, -number = {2}, -pages = {1095--1104}, -title = {{Dissecting galaxy formation. II. Comparing substructure in pure dark matter and baryonic models}}, -url = {http://adsabs.harvard.edu/abs/2010ApJ...716.1095R}, -volume = {716}, -year = {2010} -} -@article{EuclidCollaboration2025a, -abstract = {Strong gravitational lensing has the potential to provide a powerful probe of astrophysics and cosmology, but fewer than 1000 strong lenses have been confirmed previously. With \ang{;;0.16} resolution covering a third of the sky, the \Euclid telescope will revolutionise strong lens finding, with \num{170000} lenses forecasted to be discovered amongst its 1.5 billion galaxies. We present an analysis of the performance of five machine-learning models at finding strong gravitational lenses in the quick release of \Euclid data (Q1), covering 63\,deg$^{2}$. The models are validated with citizen scientists and expert visual inspection. We focus on the best performing network: a fine-tuned version of the \texttt{Zoobot} pretrained model, originally trained to classify galaxy morphologies in heterogeneous astronomical imaging surveys. Of the one million Q1 objects that \texttt{Zoobot} was tasked to find strong lenses within, the top 1000 ranked objects contained 122 grade A lenses (almost certain lenses), and 41 grade B lenses (probable lenses). A deeper search with the five networks combined with visual inspection discovered 250 (247) grade A (B) lenses, of which 224 (182) are ranked in the top \num{20000} by \texttt{Zoobot}. When extrapolated to the full \Euclid survey, the highest ranked one million images will contain \num{75000} grade A or B strong gravitational lenses.}, -archivePrefix = {arXiv}, -arxivId = {2503.15326}, -author = {{Euclid Collaboration} and Lines, N. E. P. and Collett, T. E. and Walmsley, M. and Rojas, K. and Li, T. and Leuzzi, L. and Manj{\'{o}}n-Garc{\'{i}}a, A. and Vincken, S. H. and Wilde, J. and Holloway, P. and Verma, A. and Metcalf, R. B. and Andika, I. T. and Melo, A. and Melchior, M. and S{\'{a}}nchez, H. Dom{\'{i}}nguez and D{\'{i}}az-S{\'{a}}nchez, A. and Barroso, J. A. Acevedo and Cl{\'{e}}ment, B. and Krawczyk, C. and Pearce-Casey, R. and Serjeant, S. and Courbin, F. and Despali, G. and Gavazzi, R. and Schuldt, S. and Degaudenzi, H. and Ecker, L. R. and Enzi, W. J. R. and Finner, K. and Galan, A. and Giocoli, C. and Hogg, N. B. and Jahnke, K. and Kruk, S. and Mahler, G. and More, A. and Nagam, B. C. and Pearson, J. and de Murieta, A. Sainz and Scarlata, C. and Sluse, D. and Sonnenfeld, A. and Spiniello, C. and Thai, T. T. and Tortora, C. and Ulivi, L. and Weisenbach, L. and Zumalacarregui, M. and Aghanim, N. and Altieri, B. and Amara, A. and Andreon, S. and Auricchio, N. and Aussel, H. and Baccigalupi, C. and Baldi, M. and Balestra, A. and Bardelli, S. and Battaglia, P. and Bender, R. and Bernardeau, F. and Biviano, A. and Bonchi, A. and Bonino, D. and Branchini, E. and Brescia, M. and Brinchmann, J. and Camera, S. and Ca{\~{n}}as-Herrera, G. and Capobianco, V. and Carbone, C. and Cardone, V. F. and Carretero, J. and Casas, S. and Castellano, M. and Castignani, G. and Cavuoti, S. and Chambers, K. C. and Cimatti, A. and Colodro-Conde, C. and Congedo, G. and Conselice, C. J. and Conversi, L. and Copin, Y. and Costille, A. and Courtois, H. M. and Cropper, M. and {Da Silva}, A. and {De Lucia}, G. and {Di Giorgio}, A. M. and Dolding, C. and Dole, H. and Dubath, F. and Duncan, C. A. J. and Dupac, X. and Escoffier, S. and Fabricius, M. and Farina, M. and Farinelli, R. and Faustini, F. and Ferriol, S. and Finelli, F. and Fotopoulou, S. and Frailis, M. and Franceschi, E. and Fumana, M. and Galeotta, S. and George, K. and Gillard, W. and Gillis, B. and G{\'{o}}mez-Alvarez, P. and Gracia-Carpio, J. and Granett, B. R. and Grazian, A. and Grupp, F. and Guzzo, L. and Gwyn, S. and Haugan, S. V. H. and Holmes, W. and Hook, I. M. and Hormuth, F. and Hornstrup, A. and Hudelot, P. and Jhabvala, M. and Keih{\"{a}}nen, E. and Kermiche, S. and Kiessling, A. and Kubik, B. and K{\"{u}}mmel, M. and Kunz, M. and Kurki-Suonio, H. and Boulc'h, Q. Le and Brun, A. M. C. Le and Mignant, D. Le and Ligori, S. and Lilje, P. B. and Lindholm, V. and Lloro, I. and Mainetti, G. and Maino, D. and Maiorano, E. and Mansutti, O. and Marcin, S. and Marggraf, O. and Martinelli, M. and Martinet, N. and Marulli, F. and Massey, R. and Maurogordato, S. and Medinaceli, E. and Mei, S. and Mellier, Y. and Meneghetti, M. and Merlin, E. and Meylan, G. and Mora, A. and Moresco, M. and Moscardini, L. and Nakajima, R. and Neissner, C. and Nichol, R. C. and Niemi, S. -M. and Nightingale, J. W. and Padilla, C. and Paltani, S. and Pasian, F. and Pedersen, K. and Percival, W. J. and Pettorino, V. and Pires, S. and Polenta, G. and Poncet, M. and Popa, L. A. and Pozzetti, L. and Raison, F. and Rebolo, R. and Renzi, A. and Rhodes, J. and Riccio, G. and Romelli, E. and Roncarelli, M. and Saglia, R. and Sakr, Z. and S{\'{a}}nchez, A. G. and Sapone, D. and Sartoris, B. and Schewtschenko, J. A. and Schirmer, M. and Schneider, P. and Schrabback, T. and Secroun, A. and Seidel, G. and Seiffert, M. and Serrano, S. and Simon, P. and Sirignano, C. and Sirri, G. and Mancini, A. Spurio and Stanco, L. and Steinwagner, J. and Tallada-Cresp{\'{i}}, P. and Taylor, A. N. and Tereno, I. and Toft, S. and Toledo-Moreo, R. and Torradeflot, F. and Tutusaus, I. and Valentijn, E. A. and Valenziano, L. and Valiviita, J. and Vassallo, T. and Kleijn, G. Verdoes and Veropalumbo, A. and Wang, Y. and Weller, J. and Zacchei, A. and Zamorani, G. and Zerbi, F. M. and Zucca, E. and Allevato, V. and Ballardini, M. and Bolzonella, M. and Bozzo, E. and Burigana, C. and Cabanac, R. and Cappi, A. and {Di Ferdinando}, D. and Vigo, J. A. Escartin and Gabarra, L. and Mart{\'{i}}n-Fleitas, J. and Matthew, S. and Mauri, N. and Pezzotta, A. and P{\"{o}}ntinen, M. and Porciani, C. and Risso, I. and Scottez, V. and Sereno, M. and Tenti, M. and Viel, M. and Wiesmann, M. and Akrami, Y. and Anselmi, S. and Archidiacono, M. and Atrio-Barandela, F. and Benoist, C. and Benson, K. and Bergamini, P. and Bertacca, D. and Bethermin, M. and Blanchard, A. and Blot, L. and Brown, M. L. and Bruton, S. and Calabro, A. and Caro, F. and Carvalho, C. S. and Castro, T. and Charles, Y. and Cogato, F. and Cooray, A. R. and Cucciati, O. and Davini, S. and {De Paolis}, F. and Desprez, G. and Diaz, J. J. and {Di Domizio}, S. and Diego, J. M. and Enia, A. and Fang, Y. and Ferrari, A. G. and Finoguenov, A. and Fontana, A. and Franco, A. and Ganga, K. and Garc{\'{i}}a-Bellido, J. and Gasparetto, T. and Gautard, V. and Gaztanaga, E. and Giacomini, F. and Gianotti, F. and Gozaliasl, G. and Guidi, M. and Gutierrez, C. M. and Hall, A. and Hartley, W. G. and Hern{\'{a}}ndez-Monteagudo, C. and Hildebrandt, H. and Hjorth, J. and Kajava, J. J. E. and Kang, Y. and Kansal, V. and Karagiannis, D. and Kiiveri, K. and Kirkpatrick, C. C. and Graet, J. Le and Legrand, L. and Lembo, M. and Lepori, F. and Leroy, G. and Lesci, G. F. and Lesgourgues, J. and Liaudat, T. I. and Liu, S. J. and Loureiro, A. and Macias-Perez, J. and Maggio, G. and Magliocchetti, M. and Magnier, E. A. and Mannucci, F. and Maoli, R. and Martins, C. J. A. P. and Maurin, L. and Miluzio, M. and Monaco, P. and Moretti, C. and Morgante, G. and Nadathur, S. and Naidoo, K. and Navarro-Alsina, A. and Nesseris, S. and Passalacqua, F. and Paterson, K. and Patrizii, L. and Pisani, A. and Potter, D. and Quai, S. and Radovich, M. and Rocci, P. -F. and Sacquegna, S. and Sahl{\'{e}}n, M. and Sanders, D. B. and Sarpa, E. and Schneider, A. and Sciotti, D. and Sellentin, E. and Smith, L. C. and Tanidis, K. and Testera, G. and Teyssier, R. and Tosi, S. and Troja, A. and Tucci, M. and Valieri, C. and Venhola, A. and Vergani, D. and Vernardos, G. and Verza, G. and Vielzeuf, P. and Walton, N. A. and Scott, D.}, -eprint = {2503.15326}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/EuclidQ12025paperII.pdf:pdf}, -journal = {https://arxiv.org/pdf/2503.15326}, -title = {{Euclid Quick Data Release (Q1). The Strong Lensing Discovery Engine C -- Finding lenses with machine learning}}, -url = {http://arxiv.org/abs/2503.15326}, -year = {2025} -} -@article{Pillepich2017, -abstract = {We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multimode feedback. In this paper, we give a comprehensive description of the physical and numerical advances that form the core of the IllustrisTNG (The Next Generation) framework.We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black-hole-driven kinetic feedback at low accretion rates, magnetohydrodynamics and improvements to the numerical scheme. Using a suite of (25Mpc h-1)3 cosmological boxes, we assess the outcome of the new model at our fiducial resolution. The presence of a selfconsistently amplified magnetic field is shown to have an important impact on the stellar content of 1012M⊙ haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low-mass end of the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {1703.02970}, -author = {Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R{\"{u}}diger and Hernquist, Lars and Torrey, Paul and Vogelsberger, Mark and Weinberger, Rainer and Marinacci, Federico}, -doi = {10.1093/mnras/stx2656}, -eprint = {1703.02970}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {4077--4106}, -title = {{Simulating galaxy formation with the IllustrisTNG model}}, -url = {http://arxiv.org/abs/1703.02970%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx2656}, -volume = {473}, -year = {2018} -} -@article{Tinker2016, -abstract = {We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen etal (2012) clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of Mgal for galaxies with logMgal{\textgreater}=11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma{\_}logM. Using this approach, we find sigma{\_}logM=0.18{\^{}}{\{}+0.01{\}}{\_}{\{}-0.02{\}}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L and Brownstein, Joel R and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {121}, -title = {{The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -volume = {839}, -year = {2017} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashbackslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless}10{\^{}}7{\\sim{}}M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashbackslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashbackslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashbackslashepsilon = 0.43 \backslashbackslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashbackslashpm 0.04\backslashbackslash{\{}\backslash{\%}{\}}{\$}, i.e.{\$\sim${}}a {\$}\backslashbackslashpm 2\backslashbackslashsigma{\{}\backslash{\$}{\}} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashbackslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637X/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -title = {{Supermassive black holes and their host spheroids II. The red and blue sequence in the {\$}M{\_}{\{}\backslashbackslashrm BH{\}} - M{\_}{\{}\backslashbackslashrm *,sph{\}}{\$} diagram}}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -year = {2015} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright}2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{Morningstar2019, -abstract = {We present a machine learning method for the reconstruction of the undistorted images of background sources in strongly lensed systems. This method treats the source as a pixelated image and utilizes the Recurrent Inference Machine (RIM) to iteratively reconstruct the background source given a lens model. Our architecture learns to minimize the likelihood of the model parameters (source pixels) given the data using the physical forward model (ray tracing simulations) while implicitly learning the prior of the source structure from the training data. This results in better performance compared to linear inversion methods, where the prior information is limited to the 2-point covariance of the source pixels approximated with a Gaussian form, and often specified in a relatively arbitrary manner. We combine our source reconstruction network with a convolutional neural network that predicts the parameters of the mass distribution in the lensing galaxies directly from telescope images, allowing a fully automated reconstruction of the background source images and the foreground mass distribution.}, -archivePrefix = {arXiv}, -arxivId = {1901.01359}, -author = {Morningstar, Warren R and Levasseur, Laurence Perreault and Hezaveh, Yashar D and Blandford, Roger and Marshall, Phil and Putzky, Patrick and Rueter, Thomas D and Wechsler, Risa and Welling, Max}, -doi = {10.3847/1538-4357/ab35d7}, -eprint = {1901.01359}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {14}, -title = {{Data-driven Reconstruction of Gravitationally Lensed Galaxies Using Recurrent Inference Machines}}, -url = {http://arxiv.org/abs/1901.01359}, -volume = {883}, -year = {2019} -} -@article{Zwicky1937, -abstract = {Not Available}, -author = {Zwicky, F.}, -doi = {10.1103/PhysRev.51.290}, -issn = {0031899X}, -journal = {Physical Review}, -month = {feb}, -number = {4}, -pages = {290}, -title = {{Nebulae as gravitational lenses [5]}}, -volume = {51}, -year = {1937} -} -@article{Cautun2015a, -abstract = {We investigate the angular and kinematic distributions of satellite galaxies around a large sample of bright isolated primaries in the spectroscopic and photometric catalogues of the Sloan Digital Sky Survey (SDSS). We detect significant anisotropy in the spatial distribution of satellites. To test whether this anisotropy could be related to the rotating discs of satellites recently found by Ibata et al. in a sample of SDSS galaxies, we repeat and extend their analysis. Ibata et al. found an excess of satellites on opposite sides of their primaries having anticorrelated radial velocities. We find that this excess is sensitive to small changes in the sample selection criteria which can greatly reduce its significance. In addition, we find no evidence for correspondingly correlated velocities for satellites observed on the same side of their primaries, which would be expected for rotating discs of satellites. We conclude that the detection of rotating planes of satellites in the observational sample of Ibata et al. is not robust to changes in the sample selection criteria. We compare our data to the $\Lambda$ cold dark matter Millennium simulations populated with galaxies according to the semi-analytic model of Guo et al. We find excellent agreement with the spatial distribution of satellites in the SDSS data and the lack of a strong signal from coherent rotation.}, -archivePrefix = {arXiv}, -arxivId = {1410.7778}, -author = {Cautun, Marius and Wang, Wenting and Frenk, Carlos S. and Sawala, Till}, -doi = {10.1093/mnras/stv490}, -eprint = {1410.7778}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cautun et al. - 2015 - A new spin on discs of satellite galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {3}, -pages = {2576--2587}, -title = {{A new spin on discs of satellite galaxies}}, -volume = {449}, -year = {2015} -} -@article{Halverson2016, -abstract = {We describe a detailed radial velocity error budget for the NASA-NSF Extreme Precision Doppler Spectrometer instrument concept NEID (NN-explore Exoplanet Investigations with Doppler spectroscopy). Such an instrument performance budget is a necessity for both identifying the variety of noise sources currently limiting Doppler measurements, and estimating the achievable performance of next generation exoplanet hunting Doppler spectrometers. For these instruments, no single source of instrumental error is expected to set the overall measurement floor. Rather, the overall instrumental measurement precision is set by the contribution of many individual error sources. We use a combination of numerical simulations, educated estimates based on published materials, extrapolations of physical models, results from laboratory measurements of spectroscopic subsystems, and informed upper limits for a variety of error sources to identify likely sources of systematic error and construct our global instrument performance error budget. While natively focused on the performance of the NEID instrument, this modular performance budget is immediately adaptable to a number of current and future instruments. Such an approach is an important step in charting a path towards improving Doppler measurement precisions to the levels necessary for discovering Earth-like planets.}, -archivePrefix = {arXiv}, -arxivId = {1607.05634}, -author = {Halverson, Samuel and Terrien, Ryan and Mahadevan, Suvrath and Roy, Arpita and Bender, Chad and Stef{\'{a}}nsson, Gudmundur K. and Monson, Andrew and Levi, Eric and Hearty, Fred and Blake, Cullen and McElwain, Michael and Schwab, Christian and Ramsey, Lawrence and Wright, Jason and Wang, Sharon and Gong, Qian and Roberston, Paul}, -doi = {10.1117/12.2232761}, -eprint = {1607.05634}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Halverson et al. - 2016 - A comprehensive radial velocity error budget for next generation Doppler spectrometers.pdf:pdf}, -isbn = {9781510601956}, -issn = {0277-786X}, -journal = {Ground-based and Airborne Instrumentation for Astronomy VI}, -keywords = {exoplanets,high resolution spectroscopy,radial velocity instrumentation,systems engineering}, -pages = {99086P}, -title = {{A comprehensive radial velocity error budget for next generation Doppler spectrometers}}, -url = {http://arxiv.org/abs/1607.05634%0Ahttp://dx.doi.org/10.1117/12.2232761}, -volume = {9908}, -year = {2016} -} -@article{Wallace2012, -abstract = {The linear noise approximation (LNA) is a way of approximating the stochastic time evolution of a well-stirred chemically reacting system. It can be obtained either as the lowest order correction to the deterministic chemical reaction rate equation (RRE) in van Kampen's system-size expansion of the chemical master equation (CME), or by linearising the two-term-truncated chemical Kramers-Moyal equation. However, neither of those derivations sheds much light on the validity of the LNA. The problematic character of the system-size expansion of the CME for some chemical systems, the arbitrariness of truncating the chemical Kramers-Moyal equation at two terms, the sometimes poor agreement of the LNA with the solution of the CME, have all raised concerns about the validity usefulness of the LNA. Here, the authors argue that these concerns can be resolved by viewing the LNA as an approximation of the chemical Langevin equation (CLE). This view is already implicit in Gardiner's derivation of the LNA from the truncated Kramers-Moyal equation, as that equation is mathematically equivalent to the CLE. However, the CLE can be more convincingly derived in a way that does not involve either the truncated Kramers-Moyal equation or the system-size expansion. This derivation shows that the CLE will be valid, at least for a limited span of time, for any system that is sufficiently close to the thermodynamic (large-system) limit. The relatively easy derivation of the LNA from the CLE shows that the LNA shares the CLE's conditions of validity, it also suggests that what the LNA really gives us is a description of the initial departure of the CLE from the RRE as we back away from the thermodynamic limit to a large but finite system. The authors show that this approach to the LNA simplifies its derivation, clarifies its limitations, affords an easier path to its solution. {\textcopyright}2012 The Institution of Engineering Technology.}, -author = {Wallace, E W J and Gillespie, D T and Sanft, K R and Petzold, L R}, -doi = {10.1049/iet-syb.2011.0038}, -issn = {17518849}, -journal = {IET Systems Biology}, -number = {4}, -pages = {102--115}, -title = {{Linear noise approximation is valid over limited times for any chemical system that is sufficiently large}}, -volume = {6}, -year = {2012} -} -@article{Sonnenfeld2013a, -abstract = {Several studies have suggested that the observed size evolution of massive early-type galaxies (ETGs) can be explained as a combination of dry mergers and progenitor bias, at least since z ∼ 1. In this paper we carry out a new test of the dry-merger scenario based on recent lensing measurements of the evolution of the mass density profile of ETGs. We construct a theoretical model for the joint evolution of the size and mass density profile slope $\gamma$′ driven by dry mergers occurring at rates given by cosmological simulations. Such dry-merger model predicts a strong decrease of $\gamma$′ with cosmic time, inconsistent with the almost constant $\gamma$′ inferred from observations in the redshift range 0 < z < 1. We then show with a simple toy model that a modest amount of cold gas in the mergers-consistent with the upper limits on recent star formation in ETGs-is sufficient to reconcile the model with measurements of $\gamma$′. By fitting for the amount of gas accreted during mergers, we find that models with dissipation are consistent with observations of the evolution in both size and density slope, if ∼4% of the total final stellar mass arises from the gas accreted since z ∼ 1. Purely dry merger models are ruled out at >99% CL. We thus suggest a scenario where the outer regions of massive ETGs grow by accretion of stars and dark matter, while small amounts of dissipation and nuclear star formation conspire to keep the mass density profile constant and approximately isothermal. {\textcopyright} 2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1310.3280}, -author = {Sonnenfeld, Alessandro and Nipoti, Carlo and Treu, Tommaso}, -doi = {10.1088/0004-637X/786/2/89}, -eprint = {1310.3280}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sonnenfeld, Nipoti, Treu - 2014 - Purely dry mergers do not explain the observed evolution of massive early-type galaxies since z ∼ 1.pdf:pdf}, -isbn = {doi:10.1088/0004-637X/786/2/89}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution}, -number = {2}, -pages = {89}, -title = {{Purely dry mergers do not explain the observed evolution of massive early-type galaxies since z ∼ 1}}, -url = {http://arxiv.org/abs/1310.3280%5Cnhttp://dx.doi.org/10.1088/0004-637X/786/2/89%5Cnhttp://stacks.iop.org/0004-637X/786/i=2/a=89?key=crossref.de64c6644486a7bf574a927d6caf9e8d}, -volume = {786}, -year = {2014} -} -@article{Burbidge1956, -abstract = {Abstract image available at: http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1956ApJ...124..416B&db_key=AST}, -author = {Burbidge, G. R.}, -doi = {10.1086/146237}, -isbn = {0256-9574}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {sep}, -number = {12}, -pages = {416}, -title = {{On Synchrotron Radiation from Messier 87.}}, -url = {http://adsabs.harvard.edu/doi/10.1086/146237}, -volume = {124}, -year = {1956} -} -@article{Graham2012, -abstract = {The popular log-linear relation between supermassive black hole mass, Mbh, and the dynamical mass of the host spheroid, Msph, is shown to require a significant correction. Core galaxies, typically with M bh ≳ 2 × 108 M⊙ and thought to be formed in dry merger events, are shown to be well described by a linear relation for which the median black hole mass is 0.36% - roughly double the old value of constancy. Of greater significance is that Mbh $\alpha$ M2sph among the (non-pseudobulge) lower-mass systems: specifically, log [Mbh/M⊙] = (1.92 0.38)log [M sph/7 × 1010 M⊙] + (8.38 ± 0.17). "Classical" spheroids hosting a 106 M ⊙ black hole will have Mbh/Msph 0.025%. These new relations presented herein (1) bring consistency to the relation $\alpha$ Mbh$\sigma$5 and the fact that $\alpha$ L$\sigma$x with exponents of 5 and 2 for bright (MB ≲ -20.5 mag) and faint spheroids, respectively, (2) mimic the non-(log-linear) behavior known to exist in the Mbh-(S{\'{e}}rsic n) diagram, (3) necessitate the existence of a previously overlooked Mbh$\alpha$ L2.5 relation for S{\'{e}}rsic (i.e., not core-S{\'{e}}rsic) galaxies, and (4) resolve past conflicts (in mass prediction) with the M bh-$\sigma$ relation at the low-mass end. Furthermore, the bent nature of the Mbh-Msph relation reported here for "classical" spheroids will have a host of important implications that, while not addressed in this paper, relate to (1) galaxy/black hole formation theories, (2) searches for the fundamental, rather than secondary, black hole scaling relation, (3) black hole mass predictions in other galaxies, (4) alleged pseudobulge detections, (5) estimates of the black hole mass function and mass density based on luminosity functions, (6) predictions for space-based gravitational wave detections, (7) connections with nuclear star cluster scaling relations, (8) evolutionary studies over different cosmic epochs, (9) comparisons and calibrations matching inactive black hole masses with low-mass active galactic nucleus data, and more. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.1878}, -author = {Graham, Alister W.}, -doi = {10.1088/0004-637X/746/1/113}, -eprint = {1202.1878}, -isbn = {0004-637X}, -issn = {15384357}, -journal = {ApJ}, -keywords = {black hole physics,galaxies: evolution,galaxies: nuclei}, -month = {feb}, -number = {1}, -pages = {113}, -title = {{Breaking the law: The Mbh-Mspheroid relations for core-S{\'{e}}rsic and S{\'{e}}rsic galaxies}}, -url = {http://stacks.iop.org/0004-637X/746/i=1/a=113?key=crossref.589aef5cb998332a29fe342d63e1ed81}, -volume = {746}, -year = {2012} -} -@article{Gow2016, -abstract = {{\textcopyright}2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P D and Murray, Neil J}, -doi = {10.1117/12.2232706}, -isbn = {9781510602090}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{Pontzen2014, -abstract = {One of the principal discoveries in modern cosmology is that standard model particles (including baryons, leptons and photons) together comprise only 5{\%} of the mass-energy budget of the Universe. The remaining 95{\%} consists of dark energy and dark matter (DM). Consequently our picture of the universe is known as {\{}{\$}\backslash{\$}Lambda{\}}CDM, with {\{}{\$}\backslash{\$}Lambda{\}} denoting dark energy and CDM cold dark matter. {\{}{\$}\backslash{\$}Lambda{\}}CDM is being challenged by its apparent inability to explain the low density of DM measured at the centre of cosmological systems, ranging from faint dwarf galaxies to massive clusters containing tens of galaxies the size of the Milky Way. But before making conclusions one should carefully include the effect of gas and stars, which were historically seen as merely a passive component during the assembly of galaxies. We now understand that these can in fact significantly alter the DM component, through a coupling based on rapid gravitational potential fluctuations.}, -archivePrefix = {arXiv}, -arxivId = {1402.1764}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1038/nature12953}, -eprint = {1402.1764}, -isbn = {1476-4687 (Electronic){\$}\backslash{\$}r0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -number = {7487}, -pages = {171--178}, -pmid = {24522596}, -title = {{Cold dark matter heats up}}, -volume = {506}, -year = {2014} -} -@article{Wang2015, -abstract = {We present a strong and weak lensing reconstruction of the massive cluster Abell 2744, the first cluster for which deep Hubble Frontier Fields (HFF) images and spectroscopy from the Grism Lens-Amplified Survey from Space (GLASS) are available. By performing a targeted search for emission lines in multiply imaged sources using the GLASS spectra, we obtain five high-confidence spectroscopic redshifts and two tentative ones. We confirm one strongly lensed system by detecting the same emission lines in all three multiple images. We also search for additional line emitters blindly and use the full GLASS spectroscopic catalog to test reliability of photometric redshifts for faint line emitters. We see a reasonable agreement between our photometric and spectroscopic redshift measurements, when including nebular emission in photometric redshift estimations. We introduce a stringent procedure to identify only secure multiple image sets based on colors, morphology, and spectroscopy. By combining 7 multiple image systems with secure spectroscopic redshifts (at 5 distinct redshift planes) with 18 multiple image systems with secure photometric redshifts, we reconstruct the gravitational potential of the cluster pixellated on an adaptive grid, using a total of 72 images. The resulting mass map is compared with a stellar mass map obtained from the deep Spitzer Frontier Fields data to study the relative distribution of stars and dark matter in the cluster. We find that the stellar to total mass ratio varies substantially across the cluster field, suggesting that stars do not trace exactly the total mass in this interacting system. The maps of convergence, shear, and magnification are made available in the standard HFF format.}, -archivePrefix = {arXiv}, -arxivId = {1504.02405}, -author = {Wang, X. and Hoag, A. and Huang, K. H. and Treu, T. and Bradac, M. and Schmidt, K. B. and Brammer, G. B. and Vulcani, B. and Jones, T. A. and Ryan, R. E. and Amorin, R. and Castellano, M. and Fontana, A. and Merlin, E. and Trenti, M.}, -doi = {10.1088/0004-637X/811/1/29}, -eprint = {1504.02405}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: clusters: individual (Abell 2744),galaxies: evolution,galaxies: high-redshift}, -month = {sep}, -number = {1}, -pages = {29}, -title = {{THE GRISM LENS-AMPLIFIED SURVEY from SPACE (GLASS). IV. MASS RECONSTRUCTION of the LENSING CLUSTER ABELL 2744 from FRONTIER FIELD IMAGING and GLASS SPECTROSCOPY}}, -url = {http://stacks.iop.org/0004-637X/811/i=1/a=29?key=crossref.6c6f3a5d9b78566dae09e2730ee37363}, -volume = {811}, -year = {2015} -} -@article{Bundy2015, -abstract = {Unit tests are one of the most widely used tools to assure a minimal level of quality and compliance during development. However, they are not used in many projects where development takes place at low-level contexts. The main reason is that unit test development itself demands more time and becomes expensive in this context and tools that assist test creation are rare or absent. In UEFI development this scenario matches the reality of most teams and unit testing as well as other testing techniques are often not used. To address this fault we propose UTTOS, a tool that parses EDKII build configuration files, mocks the UEFI-specific functions for C development and enables UEFI test suite code to run in the operating system. We show that UTTOS is able to run the test suit in the operating system and save development time.}, -archivePrefix = {arXiv}, -arxivId = {1412.1482}, -author = {Gomes, Eder C.M. and Amora, Paulo R.P. and Teixeira, Elvis M. and Lima, Antonio G.S. and Brito, Felipe T. and Ciocari, Juliano F.C. and Machado, Javam C.}, -doi = {10.1007/978-3-319-47443-4_14}, -eprint = {1412.1482}, -isbn = {9783319474427}, -issn = {16113349}, -journal = {Lecture Notes in Computer Science (including subseries Lecture Notes in Artificial Intelligence and Lecture Notes in Bioinformatics)}, -keywords = {C,Code coverage,Embedded systems,UEFI,Unit test}, -number = {1}, -pages = {218--224}, -pmid = {22210669}, -title = {{UTTOS: A tool for testing UEFI code in OS environment}}, -url = {http://stacks.iop.org/0004-637X/798/i=1/a=7?key=crossref.ce8f697114eeb3752ff6da50e3e66986}, -volume = {9976 LNCS}, -year = {2016} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}1011 to {\textgreater} 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Handley2015a, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Wang2018, -abstract = {We explore the isothermal total density profiles of early-type galaxies (ETGs) in the IllustrisTNG simulation. For the selected 559 ETGs at z = 0 with stellar masses $10^{10.7}\, \mathrm{M}_{\odot } \leqslant M_{\ast } \leqslant 10^{11.9}\, \mathrm{M}_{\odot }$, the total power-law slope has a mean of 〈$\gamma$′〉 = 2.011 ± 0.007 and a scatter of $\sigma _{\gamma ^{\prime }} = 0.171$ over the radial range 0.4–4 times the stellar half-mass radius. Several correlations between $\gamma$′ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction, and in situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduces many correlation trends, and in particular, $\gamma$′ is almost constant with redshift below z = 2. Through analysing IllustrisTNG model variations, we show that black hole kinetic winds are crucial to lowering $\gamma$′ and matching observed galaxy correlations. The effects of stellar winds on $\gamma$′ are subdominant compared to active galactic nucleus (AGN) feedback, and differ due to the presence of AGN feedback from previous works. The density profiles of the ETG dark matter haloes are well described by steeper than NFW profiles, and they are steeper in the full physics (FP) run than their counterparts in the dark matter-only (DMO) run. Their inner density slopes anticorrelate (remain constant) with the halo mass in the FP (DMO) run, and anticorrelate with the halo concentration parameter c200 in both the types of runs. The dark matter haloes of low-mass ETGs are contracted whereas high-mass ETGs are expanded, suggesting that variations in the total density profile occur through the different halo responses to baryons.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -doi = {10.1093/mnras/stz3348}, -eprint = {1811.06545}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2020 - Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons(2).pdf:pdf}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology,dark,formation,galaxies,matter,methods,numerical,structure,theory}, -number = {4}, -pages = {5188--5215}, -title = {{Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {491}, -year = {2020} -} -@article{Geometryeo, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Li2017, -abstract = {We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier {\$}\backslashbackslashrm ATLAS{\^{}}{\{}3D{\}}{\$} results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients.}, -archivePrefix = {arXiv}, -arxivId = {1703.04894}, -author = {Li, Hongyu and Ge, Junqiang and Mao, Shude and Cappellari, Michele and Long, R J and Li, Ran and Emsellem, Eric and Dutton, Aaron A and Li, Cheng and Bundy, Kevin and Thomas, Daniel and Drory, Niv and Lopes, Alexandre Roman}, -doi = {10.3847/1538-4357/aa662a}, -eprint = {1703.04894}, -isbn = {0004-637X}, -issn = {1538-4357}, -pages = {1--9}, -title = {{SDSS-IV MaNGA: variation of the stellar initial mass function in spiral and early-type galaxies}}, -url = {http://arxiv.org/abs/1703.04894%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa662a}, -year = {2017} -} -@article{Israel2015, -abstract = {Radiation damage to space-based charge-coupled device detectors creates defects which result in an increasing charge transfer inefficiency (CTI) that causes spurious image trailing. Most of the trailing can be corrected during post-processing, by modelling the charge trapping and moving electrons back to where they belong. However, such correction is not perfect - and damage is continuing to accumulate in orbit. To aid future development, we quantify the limitations of current approaches, and determine where imperfect knowledge of model parameters most degrades measurements of photometry and morphology. As a concrete application, we simulate 1.5 × 109 'worst-case' galaxy and 1.5 × 108 star images to test the performance of the Euclid visual instrument detectors. There are two separable challenges. If the model used to correct CTI is perfectly the same as that used to add CTI, 99.68 per cent of spurious ellipticity is corrected in our setup. This is because readout noise is not subject to CTI, but gets overcorrected during correction. Secondly, if we assume the first issue to be solved, knowledge of the charge trap density within $\Delta$$\rho$/$\rho$ = (0.0272 ± 0.0005) per cent and the characteristic release time of the dominant species to be known within $\Delta$$\tau$/$\tau$ = (0.0400 ± 0.0004) per cent will be required. This work presents the next level of definition of in-orbit CTI calibration procedures for Euclid.}, -archivePrefix = {arXiv}, -arxivId = {1506.07831}, -author = {Israel, Holger and Massey, Richard and Prod'homme, Thibaut and Cropper, Mark and Cordes, Oliver and Gow, Jason and Kohley, Ralf and Marggraf, Ole and Niemi, Sami and Rhodes, Jason and Short, Alex and Verhoeve, Peter}, -doi = {10.1093/mnras/stv1660}, -eprint = {1506.07831}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Israel et al. - 2015 - How well can charge transfer inefficiency be corrected A parameter sensitivity study for iterative correction.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Instrumentation: detectors,Methods: data analysis,Space vehicles: instruments}, -number = {1}, -pages = {561--580}, -title = {{How well can charge transfer inefficiency be corrected? A parameter sensitivity study for iterative correction}}, -volume = {453}, -year = {2015} -} -@article{Yang2019b, -abstract = {Using the Atacama Large Millimeter/submillimeter Array (ALMA), we report high angular-resolution observations of the redshift z = 3.63 galaxy H-ATLAS J083051.0+013224 (G09v1.97), one of the most luminous strongly lensed galaxies discovered by the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). We present 0.″2-0.″4 resolution images of the rest-frame 188 and 419 $\mu$m dust continuum and the CO(6-5), H2O(211-202), and Jup = 2 H2O+ line emission. We also report the detection of H2O(211-202) in this source. The dust continuum and molecular gas emission are resolved into a nearly complete ∼1.″5 diameter Einstein ring plus a weaker image in the center, which is caused by a special dual deflector lensing configuration. The observed line profiles of the CO(6-5), H2O(211-202), and Jup = 2 H2O+ lines are strikingly similar. In the source plane, we reconstruct the dust continuum images and the spectral cubes of the CO, H2O, and H2O+ line emission at sub-kiloparsec scales. The reconstructed dust emission in the source plane is dominated by a compact disk with an effective radius of 0.7 ± 0.1 kpc plus an overlapping extended disk with a radius twice as large. While the average magnification for the dust continuum is $\mu$ ∼ 10-11, the magnification of the line emission varies from 5 to 22 across different velocity components. The line emission of CO(6-5), H2O(211-202), and H2O+ have similar spatial and kinematic distributions. The molecular gas and dust content reveal that G09v1.97 is a gas-rich major merger in its pre-coalescence phase, with a total molecular gas mass of ∼1011 M. Both of the merging companions are intrinsically ultra-luminous infrared galaxies (ULIRGs) with infrared luminosities LIR reaching 4 × 1012 L, and the total LIR of G09v1.97 is (1.4 ± 0.7)×1013 L. The approaching southern galaxy (dominating from V = -400 to -150 km s-1 relative to the systemic velocity) shows no obvious kinematic structure with a semi-major half-light radius of as = 0.4 kpc, while the receding galaxy (0 to 350 km s-1) resembles an as = 1.2 kpc rotating disk. The two galaxies are separated by a projected distance of 1.3 kpc, bridged by weak line emission (-150 to 0 km s-1) that is co-spatially located with the cold dust emission peak, suggesting a large amount of cold interstellar medium (ISM) in the interacting region. As one of the most luminous star-forming dusty high-redshift galaxies, G09v1.97 is an exceptional source for understanding the ISM in gas-rich starbursting major merging systems at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {1903.00273}, -author = {Yang, C. and Gavazzi, R. and Beelen, A. and Cox, P. and Omont, A. and Lehnert, M. D. and Gao, Y. and Ivison, R. J. and Swinbank, A. M. and Barcos-Mu{\~{n}}oz, L. and Neri, R. and Cooray, A. and Dye, S. and Eales, S. and Fu, H. and Gonz{\'{a}}lez-Alfonso, E. and Ibar, E. and Micha{\l}owski, M. J. and Nayyeri, H. and Negrello, M. and Nightingale, J. and P{\'{e}}rez-Fournon, I. and Riechers, D. A. and Smail, I. and {Van Der Werf}, P.}, -doi = {10.1051/0004-6361/201833876}, -eprint = {1903.00273}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yang et al. - 2019 - CO, H2O, H2O line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales.pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: ISM,Galaxies: high-redshift,Gravitational lensing: strong,ISM: molecules,Radio lines: ISM,Submillimeter: galaxies}, -title = {{CO, H2O, H2O+ line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales}}, -volume = {624}, -year = {2019} -} -@article{Alexander2019, -abstract = {Dark matter substructure has the potential to discriminate between broad classes of dark matter models. With this in mind, we construct novel solutions to the equations of motion governing condensate dark matter candidates, namely axion Bose-Einstein condensates and superfluids. These solutions are highly compressed along one axis and thus have a disk-like geometry. We discuss linear stability of these solutions, consider the astrophysical implications as a large-scale dark disk or as small scale substructure, and find a characteristic signal in strong gravitational lensing. This adds to the growing body of work that indicates that the morphology of dark matter substructure is a powerful probe of the nature of dark matter.}, -archivePrefix = {arXiv}, -arxivId = {1901.03694}, -author = {Alexander, Stephon and Bramburger, Jason J. and McDonough, Evan}, -doi = {10.1016/j.physletb.2019.134871}, -eprint = {1901.03694}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Alexander, Bramburger, McDonough - 2019 - Dark disk substructure and superfluid dark matter.pdf:pdf}, -issn = {03702693}, -journal = {Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics}, -pages = {1--7}, -title = {{Dark disk substructure and superfluid dark matter}}, -url = {http://arxiv.org/abs/1901.03694}, -volume = {797}, -year = {2019} -} -@article{Sales2012a, -abstract = {In the simplest scenario, disk galaxies form predominantly in halos with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly-rotating remnants of repeated merging events. We explore these assumptions using one hundred systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations GIMIC. At z=0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disk galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: disks form in halos with high and low net spin, and mergers play a negligible role in the formation of spheroid stars, most of which form in-situ. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly-accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Disks, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier-accreted material. Gas accretion from a hot corona thus favours disk formation, whereas gas that flows "cold", often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, most spheroids consist of superpositions of stellar components with distinct kinematics, age, and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology is imprinted early by the interplay of the tidal field and the shape of the material destined to form the galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Hall2014, -abstract = {The science goals of space missions from the Hubble Space Telescope through to Gaia and Euclid require ultraprecise positional, photometric, and shape measurement information. However, in the radiation environment of the space telescopes, damage to the focal plane detectors through high-energy protons leads to the creation of traps, a loss of charge transfer efficiency, and a consequent deterioration in measurement accuracy. An understanding of the traps produced and their properties in the CCD during operation is essential to allow optimization of the devices and suitable modeling to correct the effect of the damage through the postprocessing of images. The technique of 'pumping single traps' has allowed the study of individual traps in high detail that cannot be achieved with other techniques, such as deep level transient spectroscopy, whilst also locating each trap to the subpixel level in the device. Outlining the principles used, we have demonstrated the technique for the A-center, the most influential trap in serial readout, giving results consistent with the more general theoretical values, but here showing new results indicating the spread in the emission times achieved and the variation in capture probability of individual traps with increasing signal levels. This technique can now be applied to other time and temperature regimes in the CCD to characterize individual traps in situ under standard operating conditions such that dramatic improvements can be made to optimization processes and modeling techniques. {\textcopyright} 2013 IEEE.}, -author = {Hall, David J. and Murray, Neil J. and Holland, Andrew D. and Gow, Jason and Clarke, Andrew and Burt, David}, -doi = {10.1109/TNS.2013.2295941}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hall et al. - 2014 - Determination of in situ trap properties in CCDs using a single-trap pumping technique.pdf:pdf}, -isbn = {9781467350570}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {A-centre,CCD image sensors,Euclid,Si-A,defect,pocket pumping,radiation damage,trap pumping}, -number = {4}, -pages = {1826--1833}, -title = {{Determination of in situ trap properties in CCDs using a "single-trap pumping" technique}}, -volume = {61}, -year = {2014} -} -@article{Li2017, -abstract = {We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier {\$}\backslashrm ATLAS{\^{}}{\{}3D{\}}{\$} results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients.}, -archivePrefix = {arXiv}, -arxivId = {1703.04894}, -author = {Li, Hongyu and Ge, Junqiang and Mao, Shude and Cappellari, Michele and Long, R J and Li, Ran and Emsellem, Eric and Dutton, Aaron A and Li, Cheng and Bundy, Kevin and Thomas, Daniel and Drory, Niv and Lopes, Alexandre Roman}, -doi = {10.3847/1538-4357/aa662a}, -eprint = {1703.04894}, -isbn = {0004-637X}, -issn = {1538-4357}, -pages = {1--9}, -title = {{SDSS-IV MaNGA: variation of the stellar initial mass function in spiral and early-type galaxies}}, -url = {http://arxiv.org/abs/1703.04894%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa662a}, -year = {2017} -} -@article{Sonnenfeld2021, -abstract = {Context. Time-delay lensing is a powerful tool for measuring the Hubble constant H0. However, in order to obtain an accurate estimate of H0 from a sample of time-delay lenses, very good knowledge of the mass structure of the lens galaxies is needed. Strong lensing data on their own are not sufficient to break the degeneracy between H0 and the lens model parameters on a single object basis. Aims. The goal of this study is to determine whether it is possible to break the H0-lens structure degeneracy with the statistical combination of a large sample of time-delay lenses, relying purely on strong lensing data with no stellar kinematics information. Methods. I simulated a set of 100 lenses with doubly imaged quasars and related time-delay measurements. I fitted these data with a Bayesian hierarchical method and a flexible model for the lens population, emulating the lens modelling step. Results. The sample of 100 lenses on its own provides a measurement of H0 with 3% precision, but with a -4% bias. However, the addition of prior information on the lens structural parameters from a large sample of lenses with no time delays, such as that considered in Paper I, allows for a 1% level inference. Moreover, the 100 lenses allow for a 0.03 dex calibration of galaxy stellar masses, regardless of the level of prior knowledge of the Hubble constant. Conclusions. Breaking the H0-lens model degeneracy with lensing data alone is possible, but 1% measurements of H0 require either many more than 100 time-delay lenses or knowledge of the structural parameter distribution of the lens population from a separate sample of lenses.}, -archivePrefix = {arXiv}, -arxivId = {2109.00009}, -author = {Sonnenfeld, Alessandro}, -doi = {10.1051/0004-6361/202142062}, -eprint = {2109.00009}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnenfeld2021StatsII.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Cosmological parameters,Galaxies: fundamental parameters,Gravitational lensing: strong}, -pages = {1--12}, -title = {{Statistical strong lensing: II. Cosmology and galaxy structure with time-delay lenses}}, -volume = {656}, -year = {2021} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Dynesty, -abstract = {We present dynesty, a public, open-source, python package to estimate Bayesian posteriors and evidences (marginal likelihoods) using the dynamic nested sampling methods developed by Higson et al. By adaptively allocating samples based on posterior structure, dynamic nested sampling has the benefits of Markov chain Monte Carlo (MCMC) algorithms that focus exclusively on posterior estimation while retaining nested sampling's ability to estimate evidences and sample from complex, multimodal distributions. We provide an overview of nested sampling, its extension to dynamic nested sampling, the algorithmic challenges involved, and the various approaches taken to solve them in this and previous work. We then examine dynesty's performance on a variety of toy problems along with several astronomical applications. We find in particular problems dynesty can provide substantial improvements in sampling efficiency compared to popular MCMC approaches in the astronomical literature. More detailed statistical results related to nested sampling are also included in the appendix.}, -archivePrefix = {arXiv}, -arxivId = {1904.02180}, -author = {Speagle, Joshua S}, -doi = {10.1093/mnras/staa278}, -eprint = {1904.02180}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {data analysis,methods,statistical}, -number = {3}, -pages = {3132--3158}, -title = {{dynesty: a dynamic nested sampling package for estimating Bayesian posteriors and evidences}}, -volume = {493}, -year = {2020} -} -@article{Wang2018c, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}} \backslashleqslant M{\_}{\{}\backslashast{\}} \backslashleqslant 10{\^{}}{\{}11.9{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashlangle\backslashgamma{\^{}}{\{}\backslashprime{\}}\backslashrangle = 2.003 \backslashpm 0.008{\$} and a standard deviation of {\$}\backslashsigma{\_}{\{}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashgamma{\_}{\{}\backslashmathrm{\{}mw{\}}{\}}{\^{}}{\{}\backslashprime{\}}-f{\_}{\{}\backslashmathrm{\{}DM{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {1}, -year = {2018} -} -@article{Cautun2015, -abstract = {The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model ($\Lambda$ cold dark matter - $\Lambda$CDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of theMWand M31 planes in $\Lambda$CDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high-resolution cosmological simulations. We find that planar structures are very common, and that {\$\sim${}}10 per cent of $\Lambda$CDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small-scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and $\Lambda$CDM predictions. In fact, {\$\sim${}}10 per cent of $\Lambda$CDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1506.04151}, -author = {Cautun, Marius and Bose, Sownak and Frenk, Carlos S and Guo, Qi and Han, Jiaxin and Hellwing, Wojciech A and Sawala, Till and Wang, Wenting}, -doi = {10.1093/mnras/stv1557}, -eprint = {1506.04151}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {4}, -pages = {3838--3852}, -title = {{Planes of satellite galaxies: When exceptions are the rule}}, -volume = {452}, -year = {2015} -} -@article{Alexander2019a, -abstract = {Strong gravitational lensing is a promising probe of the substructure of dark matter halos. Deep learning methods have the potential to accurately identify images containing substructure, and differentiate WIMP dark matter from other well motivated models, including vortex substructure of dark matter condensates and superfluids. This is crucial in future efforts to identify the true nature of dark matter. We implement, for the first time, a classification approach to identifying dark matter substructure based on simulated strong lensing images with different substructure. Utilizing convolutional neural networks trained on sets of simulated images, we demonstrate the feasibility of deep neural networks to reliably distinguish among different types of dark matter substructure. With thousands of strong lensing images anticipated with the coming launch of LSST, we expect that supervised and unsupervised deep learning models will play a crucial role in determining the nature of dark matter.}, -archivePrefix = {arXiv}, -arxivId = {1909.07346}, -author = {Alexander, Stephon and Gleyzer, Sergei and McDonough, Evan and Toomey, Michael W and Usai, Emanuele}, -eprint = {1909.07346}, -pages = {1--10}, -title = {{Deep Learning the Morphology of Dark Matter Substructure}}, -url = {http://arxiv.org/abs/1909.07346}, -year = {2019} -} -@article{Lacerna2020, -abstract = {We study the spatially resolved properties of 333 elliptical galaxies with the MaNGA/SDSS-IV survey. The aim is to understand the fundamental processes of formation and quenching of elliptical galaxies. We used the DESI Legacy Imaging Surveys for accurate morphological classification. Based on integrated spectroscopic properties and colors, we classified galaxies into classical "red and dead", recently quenched, and blue star-forming ellipticals (CLEs, RQEs, and BSFs corresponding to 75{\%}, 10{\%}, and 4{\%} of the sample, respectively). We inferred their stellar age and stellar metallicity gradients out to 1.5 effective radius, and reconstructed their global and radial histories of mass growth and star formation. We find the mass- and light-weighted age gradients of CLEs are nearly flat or mildly negative, with small differences between both ages. The respective metallicity gradients are negative, being flatter as less massive are the CLEs. The more massive CLEs assembled earlier and quenched faster than the less massive ones. The CLEs show a weak inside-out growth and a clear inside-out quenching. At masses {\textless} {\$}10{\^{}}{\{}11{\}}{\$} {\$}M{\_}{\{}\backslashbigodot{\}}{\$}, the age and {\$}Z{\$} gradients of the RQEs and BSFs are flatter than those of the CLEs but with larger scatters. They show very weak inside-out growth and quenching, being the quenching slow and even not completed at {\$}z\backslashsim{\$} 0 for the BSFs. Instead, the massive RQEs show an outside-in quenching, and positive gradients in the light-weighted age and stellar metallicities. Our results are consistent with a scenario where the inner parts of CLEs formed by an early and coeval dissipative collapse with a consequent burst of star formation and further quenching, whereas the outer parts continued their assembly likely by dry mergers. We also discuss some evolutionary scenarios for the RQE and BSF galaxies that would agree with their generic results presented here.}, -archivePrefix = {arXiv}, -arxivId = {2001.05506}, -author = {Lacerna, I and Ibarra-Medel, H and Avila-Reese, V and Hern{\'{a}}ndez-Toledo, H M and V{\'{a}}zquez-Mata, J A and S{\'{a}}nchez, S F}, -eprint = {2001.05506}, -keywords = {cd - galaxies,elliptical and lenticular,evolution - galaxies,formation - galaxies,galaxies,star formation,stellar content - galaxies,structure - galaxies}, -title = {{SDSS-IV MaNGA: global and local stellar population properties of elliptical galaxies and their assembly histories}}, -url = {http://arxiv.org/abs/2001.05506}, -year = {2020} -} -@article{Morishita2018a, -abstract = {Observations have revealed massive (logM*/Msun>11) galaxies that were already dead when the universe was only $\sim$2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6 50% of their extant masses by $\sim$1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of $\sim$0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z$\sim$5.5 to $\sim$2.2 at a rate of $\sim$0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, $\sim$0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T. and Abramson, L. E. and Treu, T. and Brammer, G. B. and Jones, T. and Kelly, P. and Stiavelli, M. and Trenti, M. and Vulcani, B. and Wang, X.}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Morishita et al. - 2019 - Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enr(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {evolution,formation,galaxies,star formation}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Milosavljevic2001, -abstract = {We investigate a model in which galactic nuclei form via the coalescence of pre-existing stellar systems containing supermassive black holes. Merger simulations are carried out using N-body algorithms that can follow the formation and decay of a black-hole binary and its effect on the surrounding stars down to sub-parsec scales. Our initial stellar systems have steep central density cusps similar to those in low-luminosity elliptical galaxies. Formation of a black-hole binary transfers energy to the stars and lowers the central density; continued decay of the binary creates a $\sim$1/r density cusp similar to those observed in bright elliptical galaxies, with a break radius that extends well beyond the sphere of gravitational influence of the black holes. The decay of the black hole binary is followed over a factor of $\sim$20 in separation after formation of a hard binary, considerably farther than in previous simulations. We see almost no dependence of the binary's decay rate on number of particles in the simulation, contrary to earlier studies in which a lower initial density of stars led to a more rapid depletion of the binary's loss cone. We nevertheless argue that the decay of a black hole binary in a real galaxy would be expected to stall at separations of 0.01-1 pc unless some additional mechanism is able to extract energy from the binary. Our results support a picture in which the observed dependence of nuclear cusp slope on galaxy luminosity is a consequence of galaxy interactions. We also discuss the implications of our results for the survivability of dark-matter cusps.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103350}, -author = {Milosavljevi{\'{c}}, Milo{\v{s}} and Merritt, David}, -doi = {10.1086/323830}, -eprint = {0103350}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {34--62}, -primaryClass = {astro-ph}, -title = {{Formation of Galactic Nuclei}}, -url = {http://arxiv.org/abs/astro-ph/0103350%0Ahttp://dx.doi.org/10.1086/323830}, -volume = {563}, -year = {2001} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a $\Lambda$CDM concordance cosmology. To that extent we use a large N-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as a function of halo mass and galaxy colour. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by ∼40° (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the colour of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the colour of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion. {\textcopyright}2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X and {Van Den Bosch}, Frank C and Yang, Xiaohu and Mao, Shude and Mo, H J and Li, Cheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@article{Goerdt2010, -abstract = {We perform a detailed investigation into the disruption of central cusps via the transfer of energy from sinking massive objects. Constant density inner regions form at the radius where the enclosed mass approximately matches the mass of the infalling body. We explore parameter space using numerical simulations and give an empirical relation for the size of the resulting core within structures that have different initial cusp slopes. We find that infalling bodies always stall at the edge of these newly formed cores, experiencing no dynamical friction over many dynamical times. As applications, we consider the resulting decrease in the dark matter annihilation flux due to centrally destroyed cusps, and we present a new theory for the formation of close binary nuclei-the "stalled binary" model.We focus on one particularly interesting binary nucleus system, the dwarf spheroidal galaxy VCC 128 which is darkmatter dominated at all radii.We showthat its nucleiwould rapidly coalesce within a fewmillion years if it has a central dark matter cusp slope steeper than r-1. However, if its initial dark matter cusp is slightly shallower than a logslope of-0.75 at∼0.1% of the virial radius, then the sinking nuclei naturally create a core equal to their observed separation and stall. This is close to the logslope measured in a recent billion particle cold darkmatter halo simulation. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0806.1951}, -author = {Goerdt, Tobias and Moore, Ben and Read, J. I. and Stadel, Joachim}, -doi = {10.1088/0004-637X/725/2/1707}, -eprint = {0806.1951}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Cosmology: theory,Dark matter,Galaxies: dwarf,Galaxies: individual (VCC 128),Methods: numerical}, -month = {dec}, -number = {2}, -pages = {1707--1716}, -title = {{Core creation in galaxies and halos via sinking massive objects}}, -url = {http://stacks.iop.org/0004-637X/725/i=2/a=1707?key=crossref.f1a39f421687694dc69519d38297f745}, -volume = {725}, -year = {2010} -} -@article{Li2018a, -abstract = {We investigate the discrepancy between the two-dimensional projected lensing mass and the dynam- ical mass for an ensemble of 97 strong gravitational lensing systems discovered by the Sloan Lens ACS (SLACS) Survey, the BOSS Emission-Line Lens Survey (BELLS), and the BELLS for GALaxy-Ly{\{}$\backslash$alpha{\}} EmitteR sYs- tems (BELLS GALLERY) Survey. We fit the lensing data to obtain the Einstein mass, and use the velocity dispersion of the lensing galaxies provided by the Sloan Digital Sky Survey (SDSS) to get the projected dynamical mass within the Einstein radius by assuming the power-law mass approximation. The discrepancy is found to be obvious and quantified by Bayesian analysis. For the singular isothermal sphere (SIS) mass model, we obtain that the Einstein mass is 20.7{\%} more than the dynamical mass, and the discrepancy increases with the redshift of the lensing galaxies. For more general power-law mass model, the discrepancy still exists within 1{\{}$\backslash$sigma{\}} credible region. The main reason of the the discrepancy could be mass contamination, including all invisible masses along the line of sight. In addition, the measurement errors and the approximation of the mass models could lead to part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1803.00819}, -author = {Li, Rui and Wang, Jiancheng and Shu, Yiping and Xu, Zhaoyi}, -doi = {10.3847/1538-4357/aaab50}, -eprint = {1803.00819}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {64}, -title = {{The Discrepancy between Einstein Mass and Dynamical Mass for SIS and Power-law Mass Models}}, -url = {http://arxiv.org/abs/1803.00819%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaab50}, -volume = {855}, -year = {2018} -} -@article{Mendez-Abreu2010a, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Vegetti2009, -abstract = {We introduce a new adaptive and fully Bayesian grid-based method to model strong gravitational lenses with extended images. The primary goal of this method is to quantify the level of luminous and dark mass substructure in massive galaxies, through their effect on highly magnified arcs and Einstein rings. The method is adaptive on the source plane, where a Delaunay tessellation is defined according to the lens mapping of a regular grid on to the source plane. The Bayesian penalty function allows us to recover the best non-linear potential-model parameters and/or a grid-based potential correction and to objectively quantify the level of regularization for both the source and potential. In addition, we implement a Nested-Sampling technique to quantify the errors on all non-linear mass model parameters - marginalized over all source and regularization parameters - and allow an objective ranking of different potential models in terms of the marginalized evidence. In particular, we are interested in comparing very smooth lens mass models with ones that contain mass substructures. The algorithm has been tested on a range of simulated data sets, created from a model of a realistic lens system. One of the lens systems is characterized by a smooth potential with a power-law density profile, 12 include a Navarro, Frenk and White (NFW) dark matter substructure of different masses and at different positions and one contains two NFW dark substructures with the same mass but with different positions. Reconstruction of the source and lens potential for all of these systems shows the method is able, in a realistic scenario, to identify perturbations with masses ≳107 M ⊙ when located on the Einstein ring. For positions both inside and outside of the ring, masses of at least 109 M⊙ are required (i.e. roughly the Einstein ring of the perturber needs to overlap with that of the main lens). Our method provides a fully novel and objective test of mass substructure in massive galaxies. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0805.0201}, -author = {Vegetti, S. and Koopmans, L. V.E.}, -doi = {10.1111/j.1365-2966.2008.14005.x}, -eprint = {0805.0201}, -isbn = {0892-0915 (Print)\r0892-0915 (Linking)}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing}, -month = {jan}, -number = {3}, -pages = {945--963}, -pmid = {20829068}, -title = {{Bayesian strong gravitational-lens modelling on adaptive grids: Objective detection of mass substructure in Galaxies}}, -volume = {392}, -year = {2009} -} -@article{Chirivi2017, -abstract = {Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we aim to present the first attempt at modelling line-of-sight (LOS) mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We have focussed on the Hubble Frontier Field cluster MACS J0416.1-2403, and our multi-plane model reproduces the observed image positions with a rms offset of $\sim$0.′′53. Starting from this best-fitting model, we simulated a mock cluster that resembles MACS J0416.1-2403 in order to explore the effects of LOS structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms $\sim$0.′′3); accounting for LOS galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factor of the lensed multiple images are recovered within $\sim$10% for $\sim$95% of them, those $\sim$5% that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models. In addition, LOS galaxies cannot explain the apparent discrepancy in the properties of massive sub-halos between MACS J0416.1-2403 and N-body simulated clusters. Since our model of MACS J0416.1-2403 with LOS galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities would be needed in future models of MACS J0416.1-2403.}, -archivePrefix = {arXiv}, -arxivId = {1706.07815}, -author = {Chiriv{\`{i}}, G. and Suyu, S. H. and Grillo, C. and Halkola, A. and Balestra, I. and Caminha, G. B. and Mercurio, A. and Rosati, P.}, -doi = {10.1051/0004-6361/201731433}, -eprint = {1706.07815}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Chiriv{\`{i}} et al. - 2018 - MACS J0416.1-2403 Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy cluster.pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Dark matter,Galaxies: clusters: general,Galaxies: clusters: individual: MACS J0416.1-2403,Gravitational lensing: strong}, -pages = {1--29}, -title = {{MACS J0416.1-2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters}}, -url = {http://arxiv.org/abs/1706.07815%0Ahttp://dx.doi.org/10.1051/0004-6361/201731433}, -volume = {614}, -year = {2018} -} -@article{Schaye2014, -abstract = {We introduce the Virgo Consortium's Evolution and Assembly of GaLaxies and their Environments (EAGLE) project, a suite of hydrodynamical simulations that follow the formation of galaxies and supermassive black holes in cosmologically representative volumes of a standard $\Lambda$ cold dark matter universe. We discuss the limitations of such simulations in light of their finite resolution and poorly constrained subgrid physics, and how these affect their predictive power. One major improvement is our treatment of feedback from massive stars and active galactic nuclei (AGN) in which thermal energy is injected into the gas without the need to turn off cooling or decouple hydrodynamical forces, allowing winds to develop without predetermined speed or mass loading factors. Because the feedback efficiencies cannot be predicted from first principles, we calibrate them to the present-day galaxy stellar mass function and the amplitude of the galaxy-central black hole mass relation, also taking galaxy sizes into account. The observed galaxy stellar mass function is reproduced to ≲0.2 dex over the full resolved mass range, 108 < M*/M⊙ ≲ 1011, a level of agreement close to that attained by semi-analytic models, and unprecedented for hydrodynamical simulations. We compare our results to a representative set of low-redshift observables not considered in the calibration, and find good agreement with the observed galaxy specific star formation rates, passive fractions, Tully-Fisher relation, total stellar luminosities of galaxy clusters, and column density distributions of intergalactic C IV and O VI. While the mass-metallicity relations for gas and stars are consistent with observations for M* ≳ 109 M⊙ (M* ≳ 1010 M⊙ at intermediate resolution), they are insufficiently steep at lower masses. For the reference model, the gas fractions and temperatures are too high for clusters of galaxies, but for galaxy groups these discrepancies can be resolved by adopting a higher heating temperature in the subgrid prescription for AGN feedback. The EAGLE simulation suite, which also includes physics variations and higher resolution zoomed-in volumes described elsewhere, constitutes a valuable new resource for studies of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1407.7040}, -author = {Schaye, Joop and Crain, Robert A. and Bower, Richard G. and Furlong, Michelle and Schaller, Matthieu and Theuns, Tom and {Dalla Vecchia}, Claudio and Frenk, Carlos S. and Mccarthy, I. G. and Helly, John C. and Jenkins, Adrian and Rosas-Guevara, Y. M. and White, Simon D.M. and Baes, Maarten and Booth, C. M. and Camps, Peter and Navarro, Julio F. and Qu, Yan and Rahmati, Alireza and Sawala, Till and Thomas, Peter A. and Trayford, James}, -doi = {10.1093/mnras/stu2058}, -eprint = {1407.7040}, -isbn = {047149870X}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {jan}, -number = {1}, -pages = {521--554}, -title = {{The EAGLE project: Simulating the evolution and assembly of galaxies and their environments}}, -volume = {446}, -year = {2015} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the TIGER principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper will report on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R and Copin, Y and Monnet, G and Miller, Bryan W and Allington-Smith, J R and Bureau, M and Carollo, C Marcella and Davies, Roger L and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F and Verolme, E K and {De Zeeuw}, P Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs,cD}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{James2018, -abstract = {We present the first spatially-resolved rest-frame UV study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z=2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each {\$\sim${}}4-8 kpc{\^{}}2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with CIII] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. The mapped CIII] emission shows distinct kinematical structure, with velocity offsets of {\$\sim${}}+/-50 km/s between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionisation parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing between -200{\textless}v(km/s){\textless}-50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star-formation rates remain relatively constant ({\$\sim${}}8-16 M{\_}sol/yr), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced. We measure electron densities with a range of log(Ne)=3.92-4.36 cm{\^{}}-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially-resolved rest-frame UV studies expected with future observatories, such as JWST.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L and Auger, Matt and Pettini, Max and Stark, Daniel P and Belokurov, V and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Morishita2018, -abstract = {Observations have revealed log M*/Msun {\textgreater}11 galaxies that were already dead when the universe was only {\$\sim${}}2Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interests. In this paper, we study star formation and metallicity enrichment histories of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple HST surveys allows robust determination of their SEDs. Our new SED modeling provides mass accumulation/stellar metallicity enrichment histories of those galaxies over the past {\$\sim${}}3Gyr, with no functional assumptions on their star formation histories. We find that most of our massive galaxies have formed {\textgreater}50{\%} of their extant masses by {\$\sim${}}1.5Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Most of our galaxies already have stellar metallicities compatible with, or even higher than, those of local early-type galaxies, with a median value of log Z*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. By using reconstructed star formation history, we reveal their rapid metallicity enrichment history from z{\$\sim${}}5.5 to 2.2 at a rate of {\$\sim${}}0.2dex/Gyr in logZ*/Zsun. The inferred metallicities are on average {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies at the time of formation. This supports a view where quenched galaxies continue to form stars at low-level until recently, rather than abrupt termination of star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -eprint = {1812.06980}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {February}, -pages = {1--13}, -title = {{Massive Dead Galaxies at z{\$\sim${}}2 with HST Grism Spectroscopy I. Star Formation and Metallicity Enrichment Histories}}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {13}, -year = {2018} -} -@article{Lilly2016, -abstract = {There are very strong observed correlations between the specific star-formation rates (sSFR) of galaxies and their mean surface mass densities, {\{}$\backslash$Sigma{\}}, as well as other aspects of their internal structure. These strong correlations have often been taken to indicate that the internal structure of a galaxy must play a major physical role, directly or indirectly, in the control of star-formation. In this paper we show by means of a very simple toy model that these correlations can arise naturally without any such physical role once the observed evolution of the size-mass relation for star-forming galaxies is taken into account. In particular, the model reproduces the sharp threshold in {\{}$\backslash$Sigma{\}} between galaxies that are star-forming and those that are quenched, and the evolution of this threshold with redshift. Similarly, it produces iso-quenched-fraction contours in the {\$}{\{}f{\_}Q(m,R{\_}e){\}}{\$} plane that are almost exactly parallel to lines of constant {\{}$\backslash$Sigma{\}} for centrals and shallower for satellites. It does so without any dependence on quenching on size or {\{}$\backslash$Sigma{\}}, and without invoking any differences between centrals and satellites, beyond the different mass-dependences of their quenching laws. The toy-model also reproduces several other observations, including the sSFR gradients within galaxies and the appearance of inside-out build-up of passive galaxies. Finally, it is shown that curvature in the Main Sequence sSFR-mass relation can produce curvature in the apparent B/T ratios with mass. Our analysis therefore suggests that many of the strong correlations that are observed between galaxy structure and sSFR may well be a consequence of things unrelated to quenching and should not be taken as evidence of the physical processes that drive quenching.}, -archivePrefix = {arXiv}, -arxivId = {1604.06459}, -author = {Lilly, Simon J and Carollo, C Marcella}, -doi = {10.3847/0004-637X/833/1/1}, -eprint = {1604.06459}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {1}, -pmid = {15540530}, -title = {{Surface density effects in quenching: cause or effect?}}, -url = {http://arxiv.org/abs/1604.06459%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/833/1/1}, -volume = {833}, -year = {2016} -} -@article{Yang2006, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd (2005), but inconsistent with several previous studies who detected a preferential minor axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful number of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag limit of ∼24. However, gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z ∼ 5–7 for LSST. We find that the LSST Wide Fast Deep survey could detect up to 120 lensed Population (Pop) I and II SNe but no lensed Pop III SNe. Deep-drilling programs in 10 deg2 fields could detect Pop I and II core-collapse SNe at AB magnitudes of 27–28 and 26, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes-Erik and Whalen, Daniel J and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S}, -doi = {10.1093/mnras/stz3203}, -eprint = {1805.02662}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cos-,cosmology,dark ages,early universe,first stars,galaxies,gravitational lensing,high-redshift,mology,observations,population iii,reionization,stars,strong}, -number = {2}, -pages = {2447--2459}, -title = {{Detecting strongly lensed supernovae at z ∼ 5–7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {491}, -year = {2020} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print){\$}\backslash{\$}r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Metcalf2018, -abstract = {Large scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100,000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. (abridged)}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R Benton and Meneghetti, M and Avestruz, Camille and Bellagamba, Fabio and Bom, Cl{\'{e}}cio R and Bertin, Emmanuel and Cabanac, R{\'{e}}mi and Davies, Andrew and Decenci{\`{e}}re, Etienne and Flamary, R{\'{e}}mi and Gavazzi, Raphael and Geiger, Mario and Hartley, Philippa and Huertas-Company, Marc and Jackson, Neal and Jullo, Eric and Kneib, Jean-Paul and Koopmans, L{\'{e}}on V E and Lanusse, Fran{\c{c}}ois and Li, Chun-Liang and Ma, Quanbin and Makler, Martin and Li, Nan and Lightman, Matthew and Petrillo, Carlo Enrico and Serjeant, Stephen and Sch{\"{a}}fer, Christoph and Sonnenfeld, Alessandro and Tagore, Amit and Tortora, Crescenzo and Tuccillo, Diego and Valent{\'{i}}n, Manuel B and Velasco-Forero, Santiago and Kleijn, Gijs A Verdoes and Vernardos, Georgios}, -eprint = {1802.03609}, -title = {{The Strong Gravitational Lens Finding Challenge}}, -url = {http://arxiv.org/abs/1802.03609}, -year = {2018} -} -@article{Greene2013, -abstract = {We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions $\sigma$* ≳ 150 km s-1. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼ 10 Gyr), relatively metal-poor ([Fe/H] ≈ -0.5), and $\alpha$-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z ≈ 1.5-2). {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1308.2682}, -author = {Greene, Jenny E. and Murphy, Jeremy D. and Graves, Genevieve J. and Gunn, James E. and Raskutti, Sudhir and Comerford, Julia M. and Gebhardt, Karl}, -doi = {10.1088/0004-637X/776/2/64}, -eprint = {1308.2682}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2013 - The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: abundances,galaxies: elliptical and lenticular, cD,galaxies: evolution}, -number = {2}, -title = {{The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius}}, -volume = {776}, -year = {2013} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the TIGER principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper will report on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R and Copin, Y and Monnet, G and Miller, Bryan W and Allington-Smith, J R and Bureau, M and Carollo, C Marcella and Davies, Roger L and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F and Verolme, E K and {De Zeeuw}, P Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs,cD}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{Lee2016, -abstract = {We study how properties of discrete dark matter haloes depend on halo environment, characterized by the mass density around the haloes on scales from 0.5 to 16 h−1 Mpc. We find that low-mass haloes (those less massive than the characteristic mass MC of haloes collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations and rounder shapes than haloes in median density environments. Haloes in median- and low-density environments have similar accretion rates and concentrations, but haloes in low-density environments have lower spins and are more elongated. Haloes of a given mass in high-density regions accrete material earlier than haloes of the same mass in lower density regions. All but the most massive haloes in high-density regions are losing mass (i.e. being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low-mass haloes in high-density regions at low redshifts z < 1, by preferentially removing higher angular momentum material from haloes. Haloes in low-density regions have lower than average spins because they lack nearby haloes whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an extreme value distribution, and that the density distribution becomes broader with cosmic time.}, -archivePrefix = {arXiv}, -arxivId = {1610.02108}, -author = {Lee, Christoph T. and Primack, Joel R. and Behroozi, Peter and Rodr{\'{i}}guez-Puebla, Aldo and Hellinger, Doug and Dekel, Avishai}, -doi = {10.1093/mnras/stw3348}, -eprint = {1610.02108}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lee et al. - 2017 - Properties of dark matter haloes as a function of local environment density.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Large-scale structure of Universe,Methods: numerical}, -number = {4}, -pages = {3834--3858}, -title = {{Properties of dark matter haloes as a function of local environment density}}, -url = {http://arxiv.org/abs/1610.02108%0Ahttp://dx.doi.org/10.1093/mnras/stw3348}, -volume = {466}, -year = {2017} -} -@article{Khochfar2011, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}R{\$}. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the {\$}\backslash{\$}atl survey, assuming that fast rotating ETGs have at least 10{\%} of their total stellar mass in a disc component. In agreement with {\$}\backslash{\$}atl observations we find that slow rotators are predominantly galaxies with {\$} M{\_}* {\textgreater}10{\^{}}{\{}10.5{\}}{\$} M{\$}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} contributing {\$}\backslashbackslashsim 20{\%}{\$} to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between {\$}\backslashbackslashsim 50{\%} -90{\%}{\$} of their stellar mass from satellites and their most massive progenitors have on average up to 3 major mergers during their evolution. Fast rotators in contrast, accrete less than 50{\%} and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stops, galaxies grow via infall from satellites. Frequent minor mergers thereby, destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}R{\$} into the slow rotator regime. Abridged...}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M and Cappellari, Michele and Davies, Roger L and Davis, Timothy A and de Zeeuw, P T and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: structure,cD}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3Dproject - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within {\$}\Lambda{\$}CDM}}, -volume = {417}, -year = {2011} -} -@article{Nightingale2024a, -author = {Nightingale, James. W. and Massey, Richard J. and Kegerreis, Jacob and Hayes, Richard G.}, -doi = {10.21105/joss.04904}, -file = {:C\:/Users/Jammy/Documents/Papers/CTI/Nightingale2024PyAutoCTI.pdf:pdf}, -issn = {2475-9066}, -journal = {J. Open Source Softw.}, -number = {98}, -pages = {4904}, -publisher = {Open Journals}, -title = {{PyAutoCTI: Open-Source Charge Transfer Inefficiency Calibration}}, -volume = {9}, -year = {2024} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/9602085v1}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085v1}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {arXiv:astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{Mukherjee2018, -abstract = {In this paper we introduce the SEAGLE (i.e. Simulating EAGLE LEnses) programme, which approaches the study of galaxy formation through strong gravitational lensing, using a suite of high-resolution hydrodynamic simulations, Evolution and Assembly of GaLaxies and their Environments (EAGLE) project.We introduce the simulation and analysis pipeline and present the first set of results from our analysis of early-type galaxies. We identify and extract an ensemble of simulated lens galaxies and use the GLAMER ray-tracing lensing code to create mock lenses similar to those observed in the Sloan Lens ACS Survey (SLACS) and SL2S surveys, using a range of source parameters and galaxy orientations, including observational effects such as the point spread function, pixelization, and noise levels, representative of single-orbit observations with the Hubble Space Telescope (HST) using the ACS-F814W filter. We subsequently model these mock lenses using the code LENSED, treating them in the same way as observed lenses. We also estimate the mass model parameters directly from the projected surface mass density of the simulated galaxy, using an identical mass model family. We perform a three-way comparison of all the measured quantities with real lenses. We find the average total density slope of EAGLE lenses, t = 2.26 (0.25 rms) to be higher than SL2S, t = 2.16 or SLACS, t = 2.08. We find a very strong correlation between the external shear ($\gamma$ ) and the complex ellipticity ($\epsilon$), with $\gamma$ $\sim$ $\epsilon$/4. This correlation indicates a degeneracy in the lens mass modelling. We also see a dispersion between lens modelling and direct fitting results, indicating systematical biases. {\textcopyright} 2018 The Author(s) Published by Oxford University Press on behalf of The Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1802.06629}, -author = {Mukherjee, Sampath and Koopmans, L{\'{e}}on V.E. and {Benton Metcalf}, R. and Tessore, Nicolas and Tortora, Crescenzo and Schaller, Matthieu and Schaye, Joop and Crain, Robert A. and Vernardos, Georgios and Bellagamba, Fabio and Theuns, Tom}, -doi = {10.1093/mnras/sty1741}, -eprint = {1802.06629}, -file = {:C\:/Users/Jammy/Documents/Papers/Simulation/Mukherjee2019SEGLE1.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: evolution,Galaxies: formation,Gravitational lensing: strong,Methods: numerical}, -number = {3}, -pages = {4108--4125}, -title = {{SEAGLE - I. A pipeline for simulating and modelling strong lenses from cosmological hydrodynamic simulations}}, -volume = {479}, -year = {2018} -} -@article{Zibetti2020, -abstract = {We perform spatially resolved stellar population analysis for a sample of 69 early-type galaxies (ETGs) from the CALIFA integral field spectroscopic survey, including 48 ellipticals and 21 S0's. We generate and quantitatively characterize profiles of light-weighted mean stellar age and metallicity within ≲2Re, as a function of radius and stellar-mass surface density $\mu$*. We study in detail the dependence of profiles on galaxies' global properties, including velocity dispersion $\sigma$e, stellar mass, morphology. ETGs are universally characterized by strong, negative metallicity gradients ({\$}\backslashsim \backslash!-0.3\backslash, \backslashtext{\{}dex{\}}{\$} per Re) within 1Re, which flatten out moving towards larger radii. A quasi-universal local $\mu$*–metallicity relation emerges, which displays a residual systematic dependence on $\sigma$e, whereby higher $\sigma$e implies higher metallicity at fixed $\mu$*. Age profiles are typically U-shaped, with minimum around 0.4 Re, asymptotic increase to maximum ages beyond {\$}\backslashsim 1.5\backslash, {\$}Re, and an increase towards the centre. The depth of the minimum and the central increase anticorrelate with $\sigma$e. A possible qualitative interpretation of these observations is a two-phase scenario. In the first phase, dissipative collapse occurs in the inner 1Re, establishing a negative metallicity gradient. The competition between the outside-in quenching due to feedback-driven winds and some form of inside-out quenching, possibly caused by central AGN feedback or dynamical heating, determines the U-shaped age profiles. In the second phase, the accretion of ex-situ stars from quenched and low-metallicity satellites shapes the flatter stellar population profiles in the outer regions.}, -archivePrefix = {arXiv}, -arxivId = {1906.02209}, -author = {Zibetti, Stefano and Gallazzi, Anna R and Hirschmann, Michaela and Consolandi, Guido and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and van de Ven, Glenn and Lyubenova, Mariya}, -doi = {10.1093/mnras/stz3205}, -eprint = {1906.02209}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {abundances,cd,elliptical and lenticular,evolution,formation,galax-,galaxies,ies,imaging,stellar content,techniques}, -number = {3}, -pages = {3562--3585}, -title = {{Insights into formation scenarios of massive early-type galaxies from spatially resolved stellar population analysis in CALIFA}}, -volume = {491}, -year = {2020} -} -@article{Lanusse2017a, -abstract = {Galaxy-scale strong gravitational lensing can not only provide a valuable probe of the dark matter distribution of massive galaxies, but also provide valuable cosmological constraints, either by studying the population of strong lenses or by measuring time delays in lensed quasars. Due to the rarity of galaxy-scale strongly lensed systems, fast and reliable automated lens finding methods will be essential in the era of large surveys such as Large Synoptic Survey Telescope, Euclid and Wide-Field Infrared Survey Telescope. To tackle this challenge, we introduce CMU DeepLens, a new fully automated galaxy-galaxy lens finding method based on deep learning. This supervised machine learning approach does not require any tuning after the training step which only requires realistic image simulations of strongly lensed systems. We train and validate our model on a set of 20 000 LSST-like mock observations including a range of lensed systems of various sizes and signal-to-noise ratios (S/N).We find on our simulated data set that for a rejection rate of non-lenses of 99 per cent, a completeness of 90 per cent can be achieved for lenses with Einstein radii larger than 1.4 arcsec and S/N larger than 20 on individual g-band LSST exposures. Finally, we emphasize the importance of realistically complex simulations for training such machine learning methods by demonstrating that the performance of models of significantly different complexities cannot be distinguished on simpler simulations.}, -archivePrefix = {arXiv}, -arxivId = {1703.02642}, -author = {Lanusse, Fran{\c{c}}ois and Ma, Quanbin and Li, Nan and Collett, Thomas E and Li, Chun Liang and Ravanbakhsh, Siamak and Mandelbaum, Rachel and P{\'{o}}czos, Barnab{\'{a}}s}, -doi = {10.1093/mnras/stx1665}, -eprint = {1703.02642}, -isbn = {0021-9258 (Print)$\backslash$r0021-9258 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: statistical,gravitational lensing: strong}, -number = {3}, -pages = {3895--3906}, -pmid = {10913147}, -title = {{CMU DeepLens: Deep learning for automatic image-based galaxy-galaxy strong lens finding}}, -url = {http://arxiv.org/abs/1703.02642}, -volume = {473}, -year = {2018} -} -@article{Richard2014, -abstract = {Extending over three Hubble Space Telescope (HST) cycles, the Hubble Frontier Fields (HFF) initiative constitutes the largest commitment ever of HST time to the exploration of the distant Universe via gravitational lensing by massive galaxy clusters. Here, we present models of the mass distribution in the six HFF cluster lenses, derived from a joint strong- and weak-lensing analysis anchored by a total of 88 multiple-image systems identified in existing HST data. The resulting maps of the projected mass distribution and of the gravitational magnification effectively calibrate the HFF clusters as gravitational telescopes. Allowing the computation of search areas in the source plane, these maps are provided to the community to facilitate the exploitation of forthcoming HFF data for quantitative studies of the gravitationally lensed population of background galaxies. Our models of the gravitational magnification afforded by the HFF clusters allow us to quantify the lensing-induced boost in sensitivity over blank-field observations and predict that galaxies at z {\textgreater} 10 and as faint as m(AB) = 32 will be detectable, up to 2 mag fainter than the limit of the Hubble Ultra Deep Field.}, -author = {Richard, Johan and Jauzac, Mathilde and Limousin, Marceau and Jullo, Eric and Cl{\'{e}}ment, Benjamin and Ebeling, Harald and Kneib, Jean Paul and Atek, Hakim and Natarajan, Priya and Egami, Eiichi and Livermore, Rachael and Bower, Richard}, -doi = {10.1093/mnras/stu1395}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies clusters: individual: A1063S,Galaxies clusters: individual: Abell 370,Galaxies clusters: individual: MACS J0416.1-2403,Galaxies clusters: individual: MACS J0717.5+3745,Galaxies clusters: individual: MACS J1149.5+2223,galaxies clusters: individual: Abell 2744}, -number = {1}, -pages = {268--289}, -title = {{Mass and magnification maps for the hubble space telescope frontier fields clusters: Implications for high-redshift studies}}, -volume = {444}, -year = {2014} -} -@article{Geometryei, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N. J. and Holland, A. D. and Gow, J. P. D. and Hall, D. J. and Tutt, James H. and Burt, D. and Endicott, J.}, -doi = {10.1117/12.926804}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2012 - Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps(2).pdf:pdf}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{PyLops, -abstract = {Linear operators and optimisation are at the core of many algorithms used in signal and image processing, remote sensing, and inverse problems. For small to medium-scale problems, existing software packages (e.g., MATLAB, Python numpy and scipy) allow for explicitly building dense (or sparse) matrices and performing algebraic operations (e.g., computation of matrix-vector products and manipulation of matrices) with syntax that closely represents their corresponding analytical forms. However, many real application, large-scale operators do not lend themselves to explicit matrix representations, usually forcing practitioners to forego of the convenient linear-algebra syntax available for their explicit-matrix counterparts. PyLops is an open-source Python library providing a flexible and scalable framework for the creation and combination of so-called linear operators, class-based entities that represent matrices and inherit their associated syntax convenience, but do not rely on the creation of explicit matrices. We show that PyLops operators can dramatically reduce the memory load and CPU computations compared to explicit-matrix calculations, while still allowing users to seamlessly use their existing knowledge of compact matrix-based syntax that scales to any problem size because no explicit matrices are required.}, -archivePrefix = {arXiv}, -arxivId = {1907.12349}, -author = {Ravasi, Matteo and Vasconcelos, Ivan}, -eprint = {1907.12349}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ravasi, Vasconcelos - 2019 - PyLops -- A Linear-Operator Python Library for large scale optimization.pdf:pdf}, -title = {{PyLops -- A Linear-Operator Python Library for large scale optimization}}, -url = {http://arxiv.org/abs/1907.12349}, -year = {2019} -} -@article{Metcalf2018, -abstract = {Large-scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images, and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects, reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100 000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. Having multi-band, ground based data is found to be better for this purpose than single-band space based data with lower noise and higher resolution, suggesting that multi-colour data is crucial. Multi-band space based data will be superior to ground based data. The most difficult challenge for a lens finder is differentiating between rare, irregular and ring-like face-on galaxies and true gravitational lenses. The degree to which the efficiency and biases of lens finders can be quantified largely depends on the realism of the simulated data on which the finders are trained.}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R B and Meneghetti, M and Avestruz, C and Bellagamba, F and Bom, C R and Bertin, E and Cabanac, R and Courbin, F and Davies, A and Decenci{\`{e}}re, E and Flamary, R and Gavazzi, R and Geiger, M and Hartley, P and Huertas-Company, M and Jackson, N and Jacobs, C and Jullo, E and Kneib, J P and Koopmans, L V E and Lanusse, F and Li, C L and Ma, Q and Makler, M and Li, N and Lightman, M and Petrillo, C E and Serjeant, S and Sch{\"{a}}fer, C and Sonnenfeld, A and Tagore, A and Tortora, C and Tuccillo, D and Valent{\'{i}}n, M B and Velasco-Forero, S and {Verdoes Kleijn}, G A and Vernardos, G}, -doi = {10.1051/0004-6361/201832797}, -eprint = {1802.03609}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Gravitational lensing: strong - methods: data anal}, -title = {{The strong gravitational lens finding challenge}}, -url = {http://arxiv.org/abs/1802.03609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201832797}, -volume = {625}, -year = {2019} -} -@article{Schombert2013, -abstract = {Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the S{\'{e}}rsic r 1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the S{\'{e}}rsic r 1/n model produces good fits to the core regions of ellipticals (r{\textless}r half), but is an inadequate function for the entire profile of an elliptical from core to halo due to competing effects on the S{\'{e}}rsic n index and the fact that the interior shape of an elliptical is only weakly correlated with its halo shape. In addition, there are a wide range of S{\'{e}}rsic parameters that will equally describe the shape of the outer profile, degrading the S{\'{e}}rsic model's usefulness as a describer of the entire profile. Empirically determined parameters, such as half-light radius and total luminosity, have less scatter than fitting function variables. The scaling relations for ellipticals are often non-linear, but for ellipticals brighter than MJ {\textless}-23 the following structural relations are found: L ∞ r 0.8±0.1, L ∞ $\Sigma$-0.5±0.1, and $\Sigma$ ∞ r -1.5±0.1. {\textcopyright}2013 Astronomical Society of Australia.}, -archivePrefix = {arXiv}, -arxivId = {1303.4710}, -author = {Schombert, J M}, -doi = {10.1017/pas.2013.010}, -eprint = {1303.4710}, -issn = {13233580}, -journal = {Publications of the Astronomical Society of Australia}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: star formation,galaxies: structure}, -number = {1}, -title = {{The structure of galaxies: II. Fitting functions and scaling relations for ellipticals}}, -url = {http://arxiv.org/abs/1303.4710%7B%5C%25%7D0Ahttp://dx.doi.org/10.1017/pas.2013.010}, -volume = {30}, -year = {2013} -} -@article{Ma2014, -abstract = {Massive early-type galaxies represent the modern day remnants of the earliest major star formation episodes in the history of the universe. These galaxies are central to our understanding of the evolution of cosmic structure, stellar populations, and supermassive black holes, but the details of their complex formation histories remain uncertain. To address this situation, we have initiated the MASSIVE Survey, a volume-limited, multi-wavelength, integral-field spectroscopic (IFS) and photometric survey of the structure and dynamics of the {\$\sim${}}100 most massive early-type galaxies within a distance of 108 Mpc. This survey probes a stellar mass range M* {\textgreater}{\$\sim${}} 1011.5 M ⊙ and diverse galaxy environments that have not been systematically studied to date. Our wide-field IFS data cover about two effective radii of individual galaxies, and for a subset of them, we are acquiring additional IFS observations on sub-arcsecond scales with adaptive optics. We are also acquiring deep K-band imaging to trace the extended halos of the galaxies and measure accurate total magnitudes. Dynamical orbit modeling of the combined data will allow us to simultaneously determine the stellar, black hole, and dark matter halo masses. The primary goals of the project are to constrain the black hole scaling relations at high masses, investigate systematically the stellar initial mass function and dark matter distribution in massive galaxies, and probe the late-time assembly of ellipticals through stellar population and kinematical gradients. In this paper, we describe the MASSIVE sample selection, discuss the distinct demographics and structural and environmental properties of the selected galaxies, and provide an overview of our basic observational program, science goals and early survey results.}, -archivePrefix = {arXiv}, -arxivId = {1407.1054}, -author = {Ma, Chung Pei and Greene, Jenny E and McConnell, Nicholas and Janish, Ryan and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/795/2/158}, -eprint = {1407.1054}, -isbn = {0000000000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content,galaxies: structure}, -number = {2}, -pages = {158}, -pmid = {28562576}, -title = {{The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...795..158M}, -volume = {795}, -year = {2014} -} -@article{VanDerWel2012, -abstract = {We present global structural parameter measurements of 109,533 unique, H F160W-selected objects from the CANDELS multi-cycle treasury program. S{\'{e}}rsic model fits for these objects are produced with GALFIT in all available near-infrared filters (H F160W, J F125W and, for a subset, Y F105W). The parameters of the best-fitting S{\'{e}}rsic models (total magnitude, half-light radius, S{\'{e}}rsic index, axis ratio, and position angle) are made public, along with newly constructed point-spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties, we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements - to 10{\%} or better - of all structural parameters can typically be obtained for galaxies with H F160W {\textless} 23, with comparable fidelity for basic size and shape measurements for galaxies to H F160W ∼ 24.5. {\textcopyright}2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1211.6954}, -author = {{Van Der Wel}, A and Bell, E F and H{\"{a}}ussler, B and McGrath, E J and Chang, Yu Yen and Guo, Yicheng and McIntosh, D H and Rix, H W and Barden, M and Cheung, E and Faber, S M and Ferguson, H C and Galametz, A and Grogin, N A and Hartley, W and Kartaltepe, J S and Kocevski, D D and Koekemoer, A M and Lotz, J and Mozena, M and Peth, M A and Peng, Chien Y}, -doi = {10.1088/0067-0049/203/2/24}, -eprint = {1211.6954}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: high-redshift,galaxies: statistics,galaxies: structure surveys}, -number = {2}, -title = {{Structural parameters of galaxies in candels}}, -volume = {203}, -year = {2012} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 {\textless} z {\textless} 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J{\textless}inf{\textgreater}125{\textless}/inf{\textgreater}, i{\textless}inf{\textgreater}814{\textless}/inf{\textgreater}, v{\textless}inf{\textgreater}606{\textless}/inf{\textgreater} HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{Murray2013a, -abstract = {Pocket-pumping is an established technique for identifying the locations of charge trapping sites within the transport channels of CCDs. Various parameters of the pumping process can be manipulated to increase the efficiency, or allow characterisation of the trap sites effective during nominal operating modes. A CCD273 was irradiated in a triangular region by protons to a 10 MeV equivalent fluence of 1.2E9 p.cm-2, ensuring a suitably low trap density for the development of an automated trap recognition algorithm. X-rays of 5, 898 eV were incident on the CCD above the region irradiated with the triangle, such that events could be analysed having passed through an increasing length of irradiated silicon and hence number of trapping sites as a function of column number. Here we present the relationship between the number of traps identified by pocket pumping within the parallel transport channels of a CCD273 and the amount of signal that is deferred by the trapping process during readout. {\textcopyright}2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Hall, David and Holland, Andrew D}, -doi = {10.1117/12.2024826}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {ccd,cic,cte,eper,euclid vis,fpr,multi-level,pocket pumping,trap pumping,tri-level}, -number = {0}, -pages = {88600H}, -title = {{The relationship between pumped traps and signal loss in buried channel CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024826}, -volume = {8860}, -year = {2013} -} -@book{Janesick2001, -abstract = {Predicting the binding mode of flexible polypeptides to proteins is an important task that falls outside the domain of applicability of most small molecule and protein−protein docking tools. Here, we test the small molecule flexible ligand docking program Glide on a set of 19 non-$\alpha$-helical peptides and systematically improve pose prediction accuracy by enhancing Glide sampling for flexible polypeptides. In addition, scoring of the poses was improved by post-processing with physics-based implicit solvent MM- GBSA calculations. Using the best RMSD among the top 10 scoring poses as a metric, the success rate (RMSD ≤ 2.0 {\AA} for the interface backbone atoms) increased from 21% with default Glide SP settings to 58% with the enhanced peptide sampling and scoring protocol in the case of redocking to the native protein structure. This approaches the accuracy of the recently developed Rosetta FlexPepDock method (63% success for these 19 peptides) while being over 100 times faster. Cross-docking was performed for a subset of cases where an unbound receptor structure was available, and in that case, 40% of peptides were docked successfully. We analyze the results and find that the optimized polypeptide protocol is most accurate for extended peptides of limited size and number of formal charges, defining a domain of applicability for this approach.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {Janesick, James R.}, -booktitle = {Scientific Charge-Coupled Devices}, -doi = {10.1117/3.374903}, -eprint = {arXiv:1011.1669v3}, -isbn = {9780819436986}, -issn = {00913286}, -keywords = {CHARGE COUPLED DEVICES,OPTICAL INSTRUMENTS}, -number = {8}, -pmid = {25246403}, -publisher = {SPIE}, -title = {{Scientific Charge-Coupled Devices}}, -url = {http://opticalengineering.spiedigitallibrary.org/article.aspx?doi=10.1117/12.7974139}, -volume = {26}, -year = {2009} -} -@article{Costantin2017, -abstract = {The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. We intended to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the {\$}i{\$}-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new ({\$}B/A{\$}, {\$}C/A{\$}) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations {\$}25{\^{}}{\{}\backslashbackslashcirc{\{}\backslash{\}}{\}} {\textless}\backslashbackslashtheta {\textless}65{\^{}}{\{}\backslashbackslashcirc{\{}\backslash{\}}{\}}{\$} we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66{\%}), with a smaller fraction of prolate spheroids (19{\%}) and triaxial ellipsoids (15{\%}). The majority of triaxial bulges are in barred galaxies (75{\%}). Moreover, we found that bulges with low S{\$}\backslash{\$}'ersic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, also bulges in late-type galaxies or in less massive galaxies have no preference in being oblate, prolate, or triaxial. On the contrary, bulges with high S{\$}\backslash{\$}'ersic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L and M{\'{e}}ndez-Abreu, J and Corsini, E M and Eliche-Moral, M C and Tapia, T and Morelli, L and Bont{\`{a}}, E Dalla and Pizzella, A}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -issn = {0004-6361}, -keywords = {bulges - galaxies,evolution - galaxies,formation - galaxies,fundamental parameters - galaxies,galaxies,photometry -}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -year = {2017} -} -@article{Vika2014, -abstract = {Bulge-disc decomposition is a valuable tool for understanding galaxies. However, achieving robust measurements of component properties is difficult, even with high-quality imaging, and it becomes even more so with the imaging typical of large surveys. In this paper, we consider the advantages of a new, multiband approach to galaxy fitting. We perform automated bulge-disc decompositions for 163 nearby galaxies, by simultaneously fitting multiple images taken in five photometric filters. We show that we are able to recover structural measurements that agree well with various other works, and confirm a number of key results. We additionally use our results to illustrate the link between total S{\'{e}}rsic index and bulge-disc structure, and demonstrate that the visually classification of lenticular galaxies is strongly dependent on the inclination of their disc component. By simulating the same set of galaxies as they would appear if observed at a range of redshifts, we are able to study the behaviour of bulge-disc decompositions as data quality diminishes. We examine how our multiband fits perform, and compare to the results of more conventional, single-band methods.Multiband fitting improves the measurement of all parameters, but particularly the bulge-to-total flux ratio and component colours. We therefore encourage the use of this approach with future surveys.}, -archivePrefix = {arXiv}, -arxivId = {1408.4070}, -author = {Vika, Marina and Bamford, Steven P. and H{\"{a}}u{\ss}ler, Boris and Rojas, Alex L.}, -doi = {10.1093/mnras/stu1696}, -eprint = {1408.4070}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure,Methods: data analysis,Techniques: image processing}, -number = {4}, -pages = {3603--3621}, -title = {{MegaMorph - multiwavelength measurement of galaxy structure: Physically meaningful bulge-disc decomposition of galaxies near and far}}, -volume = {444}, -year = {2014} -} -@article{Rest2001, -author = {Rest, Armin and Bosch, Frank C V A N D E N and Tran, Hien and Tsvetanov, Zlatan and Ford, Holland C and Davies, James and Schafer, Joanna}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rest et al. - 2001 - WFPC2 IMAGES OF THE CENTRAL REGIONS OF EARLY-TYPE GALAXIES . I . THE DATA AND We present high-resolution R-band ima.pdf:pdf}, -journal = {Database}, -keywords = {cd {\`{e}} galaxies,elliptical and lenticular,galaxies,nuclei {\`{e}} galaxies,structure}, -number = {1995}, -title = {{WFPC2 IMAGES OF THE CENTRAL REGIONS OF EARLY-TYPE GALAXIES . I . THE DATA AND We present high-resolution R-band images of the central regions of 67 early-type galaxies obtained with the Wide Field and Planetary Camera 2 ( WFPC2 ) aboard the Hubble Space T}}, -year = {2001} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of stellar parameters and abundances ("stellar labels") for hundreds of thousands of stars; this poses a formidable spectral modeling challenge. In many cases, there is a subset of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the "known" labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with and as the labels, and then applying it to the spectra of 55,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one-ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ness, M and Hogg, David W and Rix, H W and Ho, Anna Y Q and Zasowski, G}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{THE CANNON: A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION}}, -volume = {808}, -year = {2015} -} -@article{Agertz2011, -abstract = {We study the formation of disc galaxies in a fully cosmological framework using adaptive mesh refinement simulations. We perform an extensive parameter study of the main subgrid processes that control how gas is converted into stars and the coupled effect of supernovae feedback. We argue that previous attempts to form disc galaxies have been unsuccessful because of the universal adoption of strong feedback combined with high star formation efficiencies. Unless extreme amounts of energy are injected into the interstellar medium during supernovae events, these star formation parameters result in bulge dominated S0/Sa galaxies as star formation is too efficient at z$\sim$3. We show that a low efficiency of star-formation more closely models the subparsec physical processes, especially at high redshift. We highlight the successful formation of extended disc galaxies with scale lengths r_d=4-5 kpc, flat rotation curves and bulge to disc ratios of B/D$\sim$1/4. Not only do we resolve the formation of a Milky Way-like spiral galaxy, we also observe the secular evolution of the disc as it forms a pseudo-bulge. The disc properties agree well with observations and are compatible with the photometric and baryonic Tully-Fisher relations, the Kennicutt-Schmidt relation and the observed angular momentum content of spiral galaxies. We conclude that underlying small-scale star formation physics plays a larger role than previously considered in simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1004.0005}, -author = {Agertz, Oscar and Teyssier, Romain and Moore, Ben}, -doi = {10.1111/j.1365-2966.2010.17530.x}, -eprint = {1004.0005}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes,Galaxies: spiral,Methods: numerical}, -month = {jan}, -number = {2}, -pages = {1391--1408}, -title = {{The formation of disc galaxies in a ??CDM universe}}, -volume = {410}, -year = {2011} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G.}, -doi = {10.1086/507084}, -eprint = {0505272}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Agustsson, Brainerd - 2006 - The Locations of Satellite Galaxies in a $\Lambda$CDM Universe(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M_*/M_sun) > 11.5 (M_K < -25.3 mag) and distance D < 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38\pm6% down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80\pm10% and 28\pm6%, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R_e), and the gas morphologies are diverse, with 17/28 = 61\pm9% being centrally concentrated, 8/28 = 29\pm9% exhibiting clear rotation out to several kpc, and 3/28 = 11\pm6% being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly $\sim$10^5M_sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E. and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A. and Blakeslee, John P. and Goulding, Andy D. and McConnell, Nicholas J. and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pandya et al. - 2017 - The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Ear.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{Messias2014, -abstract = {[Abridged] Aims: This work focuses on one lensed system, HATLAS J142935.3-002836 (H1429-0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation. Methods: Multi-wavelength high-resolution data is utilised to assess the nature of the system. A lensing-analysis algorithm which simultaneously fits different wavebands is adopted to characterise the lens. The background galaxy dynamical information is studied by reconstructing the 3-D source-plane of the ALMA CO(J:4-3) transition. Near-IR imaging from HST and Keck-AO allows to constrain rest-frame optical photometry independently for the foreground and background systems. Physical parameters (such as stellar and dust masses) are estimated via modelling of the spectral energy distribution taking into account source blending, foreground obscuration, and differential magnification. Results: The system comprises a foreground edge-on disk galaxy (at z{\_}sp=0.218) with an almost complete Einstein ring around it. The background source (at z{\_}sp=1.027) is magnified by a factor of {\$\sim${}}8-10 depending on wavelength. It is comprised of two components and a tens of kpc long tidal tail resembling the Antennae merger. As a whole, the system is a massive stellar system (1.32[-0.41,+0.63] x1E11 Mo) forming stars at a rate of 394+-90 Mo/yr, and has a significant gas reservoir M{\_}ISM = 4.6+-1.7 x1E10 Mo. Its depletion time due to star formation alone is thus expected to be tau{\_}SF=M{\_}ISM/SFR=117+-51 Myr. The dynamical mass of one of the components is estimated to be 5.8+-1.7 x1E10 Mo, and, together with the photometric total mass estimate, it implies that H1429-0028 is a major merger system (1:2.8[-1.5,+1.8]).}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1406.4859v1}, -author = {Messias, Hugo and Dye, Simon and Nagar, Neil and Orellana, Gustavo and {Shane Bussmann}, R and Calanog, Jae and Dannerbauer, Helmut and Fu, Hai and Ibar, Edo and Inohara, Andrew and Ivison, R J and Negrello, Mattia and Riechers, Dominik A and Sheen, Yun-Kyeong and Aguirre, James E and Amber, Simon and Birkinshaw, Mark and Bourne, Nathan and Bradford, Charles M and Clements, Dave L and Cooray, Asantha and {De Zotti}, Gianfranco and Demarco, Ricardo and Dunne, Loretta and Eales, Stephen and Fleuren, Simone and Kamenetzky, Julia and Lupu, Roxana E and Maddox, Steve J and Marrone, Daniel P and Micha{\l}owski, Micha{\l}J. and Murphy, Eric J and Nguyen, Hien T and Omont, Alain and Rowlands, Kate and Smith, Dan and Smith, Matt and Valiante, Elisabetta and Vieira, Joaquin D}, -doi = {10.1051/0004-6361/201424410}, -eprint = {arXiv:1406.4859v1}, -issn = {0004-6361}, -journal = {Astronomy {\&} Astrophysics}, -keywords = {Blood pressure,Borderline hypertension,Normotensive}, -number = {3}, -pages = {A92}, -pmid = {18274343}, -title = {{Herschel -ATLAS and ALMA }}, -url = {http://www.aanda.org/10.1051/0004-6361/201424410}, -volume = {568}, -year = {2014} -} -@article{2001ev, -author = {عامر, د. وفاء محروس}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/عامر - 2001 - No Title المعالجة الحيوية للمولوثات البيئية(11).pdf:pdf}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{More2016, -abstract = {We report the discovery of 29 promising (and 59 total) new lens candidates from the Canada- France-Hawaii Telescope Legacy Survey (CFHTLS) based on about 11 million classifications performed by citizen scientists as part of the first SPACEWARPS lens search. The goal of the blind lens search was to identify lens candidates missed by robots (the RINGFINDER on galaxy scales and ARCFINDER on group/cluster scales) which had been previously used to mine the CFHTLS for lenses. We compare some properties of the samples detected by these algorithms to the SPACE WARPS sample and find them to be broadly similar. The image separation distribution calculated from the SPACE WARPS sample shows that previous constraints on the average density profile of lens galaxies are robust. SPACE WARPS recovers about 65 per cent of known lenses, while the new candidates show a richer variety compared to those found by the two robots. This detection rate could be increased to 80 per cent by only using classifications performed by expert volunteers (albeit at the cost of a lower purity), indicating that the training and performance calibration of the citizen scientists is very important for the success of SPACE WARPS. In this work we present the SIMCT pipeline, used for generating in situ a sample of realistic simulated lensed images. This training sample, along with the false positives identified during the search, has a legacy value for testing future lens-finding algorithms. We make the pipeline and the training set publicly available.}, -archivePrefix = {arXiv}, -arxivId = {1504.05587}, -author = {More, Anupreeta and Verma, Aprajita and Marshall, Philip J. and More, Surhud and Baeten, Elisabeth and Wilcox, Julianne and Macmillan, Christine and Cornen, Claude and Kapadia, Amit and Parrish, Michael and Snyder, Chris and Davis, Christopher P. and Gavazzi, Raphael and Lintott, Chris J. and Simpson, Robert and Miller, David and Smith, Arfon M. and Paget, Edward and Saha, Prasenjit and K{\"{u}}ng, Rafael and Collett, Thomas E.}, -doi = {10.1093/mnras/stv1965}, -eprint = {1504.05587}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: strong,Methods: statistical}, -month = {jan}, -number = {2}, -pages = {1191--1210}, -title = {{SPACEWARPS- II. New gravitational lens candidates from the CFHTLS discovered through citizen science}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stv1965}, -volume = {455}, -year = {2016} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified {\$\sim${}}17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M {\textless}10{\^{}}9 M*), low-metallicity (Z{\$\sim${}}1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He $\backslash$ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A and Erb, Dawn K and Auger, Matthew W and Pettini, Max and Brammer, Gabriel B}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {164}, -title = {{ A Window on the Earliest Star Formation: Extreme Photoionization Conditions of a High-ionization, Low-metallicity Lensed Galaxy at z ∼ 2* }}, -url = {http://arxiv.org/abs/1803.02340}, -volume = {859}, -year = {2018} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{Pontzen2014, -abstract = {A principal discovery in modern cosmology is that standard model particles comprise only 5 per cent of the mass-energy budget of the Universe. In the $\Lambda$CDM paradigm, the remaining 95 per cent consists of dark energy ($\Lambda$) and cold dark matter. $\Lambda$CDM is being challenged by its apparent inability to explain the low-density 'cores' of dark matter measured at the centre of galaxies, where centrally concentrated high-density 'cusps' were predicted. But before drawing conclusions, it is necessary to include the effect of gas and stars, historically seen as passive components of galaxies. We now understand that these can inject heat energy into the cold dark matter through a coupling based on rapid gravitational potential fluctuations, explaining the observed low central densities. {\textcopyright}2014 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1402.1764}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1038/nature12953}, -eprint = {1402.1764}, -isbn = {1476-4687 (Electronic)$\backslash$r0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -number = {7487}, -pages = {171--178}, -pmid = {24522596}, -title = {{Cold dark matter heats up}}, -volume = {506}, -year = {2014} -} -@article{Wertz2018, -abstract = {Modern time-delay cosmography aims to infer the cosmological parameters with a competitive precision from observing a multiply imaged quasar. The success of this technique relies upon a robust modeling of the lens mass distribution. Unfortunately strong degeneracies between density profiles that lead to almost the same lensing observables may bias precise estimates of the Hubble constant. The source position transformation (SPT), which covers the well-known mass-sheet transformation (MST) as a special case, defines a new framework to investigate these degeneracies. In this paper, we present pySPT, a python package dedicated to the SPT. We describe how it can be used to evaluate the impact of the SPT on lensing observables. We review most of its capabilities and elaborate on key features that we used in a companion paper regarding SPT and time delays. The pySPT program also comes with a subpackage dedicated to simple lens modeling. This can be used to generate lensing related quantities for a wide variety of lens models independent of any SPT analysis. As a first practical application, we present a correction to the first estimate of the impact on time delays of the SPT, which has been experimentally found in a previous work between a softened power law and composite (baryons + dark matter) lenses. We find that the large deviations previously predicted have been overestimated because of a minor bug in the public lens modeling code lensmodel (v1.99), which is now fixed. We conclude that the predictions for the Hubble constant deviate by ∼7{\%}, first and foremost as a consequence of an MST. The latest version of pySPT is available on Github, a software development platform, along with some tutorials to describe in detail how making the best use of pySPT.}, -archivePrefix = {arXiv}, -arxivId = {1801.04151}, -author = {Wertz, Olivier and Orthen, Bastian}, -doi = {10.1051/0004-6361/201732242}, -eprint = {1801.04151}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Cosmological parameters,Gravitational lensing: Strong}, -pages = {A117}, -title = {{A dedicated source-position transformation package: PySPT}}, -url = {http://arxiv.org/abs/1801.04151%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201732242}, -volume = {619}, -year = {2018} -} -@article{Birrer2018a, -abstract = {We present lenstronomy, a multi-purpose open-source gravitational lens modelling pythonpackage. lenstronomy is able to reconstruct the lens mass and surface brightness distributions of strong lensing systems using forward modelling. lenstronomy supports a wide range of analytic lens and light models in arbitrary combination. The software is also able to reconstruct complex extended sources (Birrer et. al 2015) as well as being able to model point sources. We designed lenstronomy to be stable, flexible and numerically accurate, with a clear user interface that could be deployed across different platforms. Throughout its development, we have actively used lenstronomy to make several measurements including deriving constraints on dark matter properties in strong lenses, measuring the expansion history of the universe with time-delay cosmography, measuring cosmic shear with Einstein rings and decomposing quasar and host galaxy light. The software is distributed under the MIT license. The documentation, starter guide, example notebooks, source code and installation guidelines can be found at https://lenstronomy.readthedocs.io.}, -archivePrefix = {arXiv}, -arxivId = {1803.09746}, -author = {Birrer, Simon and Amara, Adam}, -doi = {10.1016/j.dark.2018.11.002}, -eprint = {1803.09746}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Birrer, Amara - 2018 - lenstronomy Multi-purpose gravitational lens modelling software package.pdf:pdf}, -issn = {22126864}, -journal = {Physics of the Dark Universe}, -keywords = {Gravitational lensing,Image simulations,Software}, -pages = {189--201}, -title = {{lenstronomy: Multi-purpose gravitational lens modelling software package}}, -volume = {22}, -year = {2018} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M{\textgreater}10{\^{}}11 M{\_}sun) galaxies at 1.7{\textless}z{\textless}3 utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our sample is almost an order of magnitude larger than previous studies at these redshifts, providing the first statistical study of massive galaxy sizes at z{\textgreater}2, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n{\textless}2) and spheroid-like (n{\textgreater}2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z{\$\sim${}}2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z{\textgreater}2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ({\$\sim${}}2x10{\^{}}10 M{\_}sun kpc{\^{}}-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J and Bouwens, Rychard J and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61----L64}, -title = {{ Size Evolution of the Most Massive Galaxies at 1.7 {\textless} z {\textless} 3 from GOODS NICMOS Survey Imaging }}, -url = {http://arxiv.org/abs/0807.4141%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Bullock2001, -abstract = {We study dark matter halo density profiles in a high-resolution N-body simulation of a $\Lambda$CDM cosmology. Our statistical sample contains ∼5000 haloes in the range 1011-1014 h-1 M⊙, and the resolution allows a study of subhaloes inside host haloes. The profiles are parametrized by an NFW form with two parameters, an inner radius rs and a virial radius Rvir, and we define the halo concentration cvir ≡ Rvir/rs. First, we find that, for a given halo mass, the redshift dependence of the median concentration is cvir ∝ (1 + z)-1. This corresponds to rs(z) ∼ constant, and is contrary to earlier suspicions that cvir does not vary much with redshift. The implications are that high-redshift galaxies are predicted to be more extended and dimmer than expected before. Secondly, we find that the scatter in halo profiles is large, with a 1$\sigma$ $\Delta$(log cvir) = 0.18 at a given mass, corresponding to a scatter in maximum rotation velocities of $\Delta$Vmax/Vmax = 0.12. We discuss implications for modelling the Tully-Fisher relation, which has a smaller reported intrinsic scatter. Thirdly, subhaloes and haloes in dense environments tend to be more concentrated than isolated haloes, and show a larger scatter. These results suggest that cvir is an essential parameter for the theory of galaxy modelling, and we briefly discuss implications for the universality of the Tully-Fisher relation, the formation of low surface brightness galaxies, and the origin of the Hubble sequence. We present an improved analytic treatment of halo formation that fits the measured relations between halo parameters and their redshift dependence, and can thus serve semi-analytic studies of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9908159}, -author = {Bullock, J. S. and Kolatt, T. S. and Sigad, Y. and Somerville, R. S. and Kravtsov, A. V. and Klypin, A. A. and Primack, J. R. and Dekel, A.}, -doi = {10.1046/j.1365-8711.2001.04068.x}, -eprint = {9908159}, -isbn = {978-1-4244-6023-6}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: formation,Galaxies: structure}, -month = {mar}, -number = {3}, -pages = {559--575}, -pmid = {25246403}, -primaryClass = {astro-ph}, -title = {{Profiles of dark haloes: Evolution, scatter and environment}}, -volume = {321}, -year = {2001} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for $\sim$20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J. and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Coenda, Mart{\'{i}}nez, Muriel - 2018 - Green valley galaxies as a transition population in different environments.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Enia2018, -abstract = {We perform lens modelling and source reconstruction of Submillimeter Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500{\$}\backslashmu{\$}m in the Herschel Astrophysical Terahertz Large Area Survey H-ATLAS. A previous analysis of the same dataset used a single S$\backslash$`ersic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from the H-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission. We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5{\$}\backslashsigma{\$}. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value {\$}r{\_}{\{}eff{\}}\backslash,\backslashsim 1.77\backslash,{\$}kpc and a median Gaussian full width at half maximum {\$}\backslashsim1.47\backslash,{\$}kpc. After correction for magnification, our sources have intrinsic star formation rates SFR{\$}\backslash,\backslashsim900-3500\backslash,M{\_}{\{}\backslashodot{\}}yr{\^{}}{\{}-1{\}}{\$}, resulting in a median star formation rate surface density {\$}\backslashSigma{\_}{\{}SFR{\}}\backslashsim132\backslash,M{\_}{\{}\backslashodot{\}}{\$} yr{\$}{\^{}}{\{}-1{\}}{\$} kpc{\$}{\^{}}{\{}-2{\}}{\$} (or {\$}\backslashsim 218\backslash,M{\_}{\{}\backslashodot{\}}{\$} yr{\$}{\^{}}{\{}-1{\}}{\$} kpc{\$}{\^{}}{\{}-2{\}}{\$} for the Gaussian fit). This is consistent with what observed for other star forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst.}, -archivePrefix = {arXiv}, -arxivId = {1801.01831}, -author = {Enia, A and Negrello, M and Gurwell, M and Dye, S and Rodighiero, G and Massardi, M and {De Zotti}, G and Franceschini, A and Cooray, A and van der Werf, P and Birkinshaw, M and Michalowski, M J and Oteo, I}, -doi = {10.1093/mnras/sty021}, -eprint = {1801.01831}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong,Instrumentation: interferometers}, -number = {3}, -pages = {3467--3484}, -title = {{The Herschel-ATLAS: Magnifications and physical sizes of 500-$\mu$m-selected strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1801.01831}, -volume = {475}, -year = {2018} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kremer et al. - 2017 - Big Universe, Big Data Machine Learning and Image Analysis for Astronomy.pdf:pdf}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Read2005, -abstract = {Dwarf spheroidal galaxies have shallow central dark matter density profiles, low angular momentum and approximately exponential surface brightness distributions. Through N-body simulations and analytic calculations we investigate the extent to which these properties can be generated from 'typical' ACDM galaxies, which differ in all of these properties, by the dynamical consequences of feedback. We find that, for a wide range of initial conditions, one impulsive mass-loss event will naturally produce a surface brightness profile in the remaining stellar component of a dwarf spheroidal galaxy (dSph) which is well-fitted over many scalelengths by an exponential, in good qualitative agreement with observations of Local Group dSphs. Furthermore, two impulsive mass-loss phases, punctuated by significant gas re-accretion, are found to be sufficient to transform a central density cusp in the dark matter profile into a near-constant density core. This may then provide the missing link between current cosmological simulations, which predict a central cusp in the dark matter density profile, and current observations, which find much shallower central density profiles. We also look at the angular momentum history of dSphs and demonstrate that if these galaxies have spent most of their lifetime in tidal isolation from massive galaxies then they cannot have formed from high angular momentum gas discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0409565}, -author = {Read, J. I. and Gilmore, G.}, -doi = {10.1111/j.1365-2966.2004.08424.x}, -eprint = {0409565}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Evolution,Galaxies,Galaxies: dwarf,Galaxies: haloes,Galaxies: kinematics and dynamics,Galaxies: structure}, -month = {jan}, -number = {1}, -pages = {107--124}, -primaryClass = {astro-ph}, -title = {{Mass loss from dwarf spheroidal galaxies: The origins of shallow dark matter cores and exponential surface brightness profiles}}, -volume = {356}, -year = {2005} -} -@article{Inoue2012, -abstract = {We explore the weak lensing effect by line-of-sight haloes and subhaloes with a mass of M ≲ 10 7M ⊙ in Quasi-Stellar Object (QSO)-galaxy strong lens systems with quadruple images in a concordant $\Lambda$ cold dark matter universe. Using a polynomially fitted non-linear power spectrum P(k) obtained from N-body simulations that can resolve haloes with a mass of M ∼ 10 5M ⊙, or structures with a comoving wavenumber of k ∼ 3 × 10 2hMpc -1, we find that the ratio of magnification perturbation due to intervening haloes to that of a primary lens is typically ∼10 per cent and the predicted values agree well with the estimated values for six observed QSO-galaxy lens systems with quadruple images in the mid-infrared band without considering the effects of substructures inside a primary lens. We also find that the estimated amplitudes of convergence perturbation for the six lenses increase with the source redshift as predicted by theoretical models. Using an extrapolated matter power spectrum, we demonstrate that small haloes or subhaloes in the line of sight with a mass of M = 10 3-10 7M ⊙, or structures with a comoving wavenumber of k = 3 × 10 2-10 4hMpc -1, can significantly affect the magnification ratios of the lensed images. Flux-ratio anomalies in QSO-galaxy strong lens systems offer us a unique probe into the clustering property of minihaloes with a mass of M < 10 6M ⊙. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1207.2139v2}, -author = {Inoue, Kaiki Taro and Takahashi, Ryuichi}, -doi = {10.1111/j.1365-2966.2012.21915.x}, -eprint = {arXiv:1207.2139v2}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: formation}, -number = {4}, -pages = {2978--2993}, -title = {{Weak lensing by line-of-sight haloes as the origin of flux-ratio anomalies in quadruply lensed QSOs}}, -volume = {426}, -year = {2012} -} -@article{Costantin2017, -abstract = {The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. We intended to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the {\$}i{\$}-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new ({\$}B/A{\$}, {\$}C/A{\$}) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations {\$}25{\^{}}{\{}\backslashcirc{\}} {\textless} \backslashtheta {\textless} 65{\^{}}{\{}\backslashcirc{\}}{\$} we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66{\%}), with a smaller fraction of prolate spheroids (19{\%}) and triaxial ellipsoids (15{\%}). The majority of triaxial bulges are in barred galaxies (75{\%}). Moreover, we found that bulges with low S$\backslash$'ersic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, also bulges in late-type galaxies or in less massive galaxies have no preference in being oblate, prolate, or triaxial. On the contrary, bulges with high S$\backslash$'ersic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L and M{\'{e}}ndez-Abreu, J and Corsini, E M and Eliche-Moral, M C and Tapia, T and Morelli, L and Bont{\`{a}}, E Dalla and Pizzella, A}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -issn = {0004-6361}, -keywords = {bulges - galaxies,evolution - galaxies,formation - galaxies,fundamental parameters - galaxies,galaxies,photometry -}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -year = {2017} -} -@article{Fergus2014, -abstract = {High dynamic range imagers aim to block or eliminate light from a very bright primary star in order to make it possible to detect and measure far fainter companions; in real systems, a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronagraph. The model uses principal components analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles, but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of the order of a percent of the brightness of the speckles, or up to 10-7 times the brightness of the primary star. This outperforms existing methods by a factor of two to three and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Metcalf2018, -abstract = {Large-scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images, and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects, reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100 000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. Having multi-band, ground based data is found to be better for this purpose than single-band space based data with lower noise and higher resolution, suggesting that multi-colour data is crucial. Multi-band space based data will be superior to ground based data. The most difficult challenge for a lens finder is differentiating between rare, irregular and ring-like face-on galaxies and true gravitational lenses. The degree to which the efficiency and biases of lens finders can be quantified largely depends on the realism of the simulated data on which the finders are trained.}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R B and Meneghetti, M and Avestruz, C and Bellagamba, F and Bom, C R and Bertin, E and Cabanac, R and Courbin, F and Davies, A and Decenci{\`{e}}re, E and Flamary, R and Gavazzi, R and Geiger, M and Hartley, P and Huertas-Company, M and Jackson, N and Jacobs, C and Jullo, E and Kneib, J P and Koopmans, L V E and Lanusse, F and Li, C L and Ma, Q and Makler, M and Li, N and Lightman, M and Petrillo, C E and Serjeant, S and Sch{\"{a}}fer, C and Sonnenfeld, A and Tagore, A and Tortora, C and Tuccillo, D and Valent{\'{i}}n, M B and Velasco-Forero, S and {Verdoes Kleijn}, G A and Vernardos, G}, -doi = {10.1051/0004-6361/201832797}, -eprint = {1802.03609}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Gravitational lensing: strong - methods: data anal}, -title = {{The strong gravitational lens finding challenge}}, -url = {http://arxiv.org/abs/1802.03609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201832797}, -volume = {625}, -year = {2019} -} -@article{Shi2015, -abstract = {{\textcopyright}2015. The American Astronomical Society. All rights reserved.We study how halo intrinsic dynamical properties are linked to their formation processes for halos in two mass ranges, 1012-1012.5 h-1M⊙ and ≥1013 h-1M⊙, and how both are correlated with the large-scale tidal field within which the halos reside at present. We identify infall halos that are about to merge with their hosts. We find that the tangential infall velocity increases significantly with the strength of the tidal field, but no strong correlation is found for the radial component. These results can be used to explain the environmental dependence of internal velocity anisotropy and spin of halos. The position vectors and velocities of infall halos are aligned with the principal axes of the tidal field, and the alignment depends on the strength of the tidal field. Opposite accretion patterns are found in weak and strong tidal fields, showing that in a weak field the accretion flow is dominated by radial motion within the local structure, while a large tangential component is present in a strong field. These findings can be used to understand the strong alignments we find between the principal axes of the internal velocity ellipsoids of halos and the tidal field, and their dependence on the strength of the tidal field. We further find that only in weak tidal fields does the spin-tidal field alignment follow the prediction of the tidal torque theory. We discuss how our results may be used to understand the spins of disk galaxies and velocity structures of elliptical galaxies and their correlations with large-scale structure.}, -archivePrefix = {arXiv}, -arxivId = {1501.07764}, -author = {Shi, Jingjing and Wang, Huiyuan and Mo, H J}, -doi = {10.1088/0004-637X/807/1/37}, -eprint = {1501.07764}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: halos,large-scale structure of universe,methods: statistical}, -number = {1}, -title = {{Flow Patterns Around Dark Matter Halos: the Link Between Halo Dynamical Properties and Large-Scale Tidal Field}}, -volume = {807}, -year = {2015} -} -@article{Veale2016, -abstract = {We present spatially resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (ETGs; MK ≲ -25.7 mag, stellar mass M* ≳ 1011.8 M⊙) of the volumelimited (D < 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650-5850 {\AA} from the 246-fibre Mitchell integral-field spectrograph at McDonald Observatory, covering a 107 arcsec×107 arcsec field of view(often reaching 2 to 3 effective radii).We measure the 2D spatial distribution of each galaxy's angular momentum ($\lambda$ and fast or slow rotator status), velocity dispersion ($\sigma$), and higher order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ($\sim$80 per cent) of slow and non-rotators with $\lambda$ ≲ 0.2. When combined with the lower mass ETGs in the ATLAS3D survey, we find the fraction of slow rotators to increase dramatically with galaxy mass, reaching $\sim$50 per cent at MK $\sim$ -25.5 mag and $\sim$90 per cent at MK ≲ -26 mag. All of our fast rotators show a clear anticorrelation between h3 and V/$\sigma$, and the slope of the anticorrelation is steeper in more round galaxies. The radial profiles of s show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK ≲ -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat s profiles, whereas five of the seven 'isolated' galaxies are all fainter than MK = -25.8 mag and have falling $\sigma$. All of our galaxies have positive average h4; the most luminous galaxies have average h4 $\sim$ 0.05, while less luminous galaxies have a range of values between 0 and 0.05. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising s profiles. We discuss the implications for the relationship among dynamical mass, $\sigma$, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E. and McConnell, Nicholas J. and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P. and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Veale et al. - 2017 - The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Leauthaud2017, -abstract = {We present high signal-to-noise galaxy-galaxy lensing measurements of the BOSS CMASS sample using 250 square degrees of weak lensing data from CFHTLenS and CS82. We compare this signal with predictions from mock catalogs trained to match observables including the stellar mass function and the projected and two dimensional clustering of CMASS. We show that the clustering of CMASS, together with standard models of the galaxy-halo connection, robustly predicts a lensing signal that is 20-40{\%} larger than observed. Detailed tests show that our results are robust to a variety of systematic effects. Lowering the value of {\$}S{\_}{\{}\backslashrm 8{\}}=\backslashsigma{\_}{\{}\backslashrm 8{\}} \backslashsqrt{\{}\backslashOmega{\_}{\{}\backslashrm m{\}}/0.3{\}}{\$} compared to Planck2015 reconciles the lensing with clustering. However, given the scale of our measurement ({\$}r{\textless}10{\$} {\$}h{\^{}}{\{}-1{\}}{\$} Mpc), other effects may also be at play and need to be taken into consideration. We explore the impact of baryon physics, assembly bias, massive neutrinos, and modifications to general relativity on {\$}\backslashDelta\backslashSigma{\$} and show that several of these effects may be non-negligible given the precision of our measurement. Disentangling cosmological effects from the details of the galaxy-halo connection, the effects of baryons, and massive neutrinos, is the next challenge facing joint lensing and clustering analyses. This is especially true in the context of large galaxy samples from Baryon Acoustic Oscillation surveys with precise measurements but complex selection functions.}, -archivePrefix = {arXiv}, -arxivId = {1611.08606}, -author = {Leauthaud, Alexie and Saito, Shun and Hilbert, Stefan and Barreira, Alexandre and More, Surhud and White, Martin and Alam, Shadab and Behroozi, Peter and Bundy, Kevin and Coupon, Jean and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Mandelbaum, Rachel and Miller, Lance and Moraes, Bruno and Pereira, Maria E S and Rodr{\'{i}}guez-Torres, Sergio A and Schmidt, Fabian and Shan, Huan Yuan and Viel, Matteo and Villaescusa-Navarro, Francisco}, -doi = {10.1093/mnras/stx258}, -eprint = {1611.08606}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {3}, -pages = {3024--3047}, -title = {{Lensing is low: Cosmology, galaxy formation or new physics?}}, -volume = {467}, -year = {2017} -} -@article{pyswarms, -author = {Miranda, Lester James V}, -doi = {10.21105/joss.00433}, -journal = {Journal of Open Source Software}, -number = {21}, -title = {{{P}y{S}warms, a research-toolkit for {P}article {S}warm {O}ptimization in {P}ython}}, -url = {https://doi.org/10.21105/joss.00433}, -volume = {3}, -year = {2018} -} -@article{Mendez-Abreu2010, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Murray2013a, -abstract = {Pocket-pumping is an established technique for identifying the locations of charge trapping sites within the transport channels of CCDs. Various parameters of the pumping process can be manipulated to increase the efficiency, or allow characterisation of the trap sites effective during nominal operating modes. A CCD273 was irradiated in a triangular region by protons to a 10 MeV equivalent fluence of 1.2E9 p.cm-2, ensuring a suitably low trap density for the development of an automated trap recognition algorithm. X-rays of 5, 898 eV were incident on the CCD above the region irradiated with the triangle, such that events could be analysed having passed through an increasing length of irradiated silicon and hence number of trapping sites as a function of column number. Here we present the relationship between the number of traps identified by pocket pumping within the parallel transport channels of a CCD273 and the amount of signal that is deferred by the trapping process during readout. {\textcopyright}2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Hall, David and Holland, Andrew D}, -doi = {10.1117/12.2024826}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {ccd,cic,cte,eper,euclid vis,fpr,multi-level,pocket pumping,trap pumping,tri-level}, -number = {0}, -pages = {88600H}, -title = {{The relationship between pumped traps and signal loss in buried channel CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024826}, -volume = {8860}, -year = {2013} -} -@article{Hopkins2012, -abstract = {Feedback from massive stars is believed to play a critical role in driving galactic super-winds that enrich the IGM and shape the galaxy mass function and mass-metallicity relation. In previous papers, we introduced new numerical methods for implementing stellar feedback on sub-GMC through galactic scales in galaxy simulations. This includes radiation pressure (UV through IR), SNe (Type-I {\&} II), stellar winds ('fast' O-star through 'slow' AGB winds), and HII photoionization. Here, we show that these feedback mechanisms drive galactic winds with outflow rates as high as {\$\sim${}}10-20 times the galaxy SFR. The mass-loading efficiency (wind mass loss rate divided by SFR) scales inversely with circular velocity, consistent with momentum-conservation expectations. We study the contributions of each feedback mechanism to galactic winds in a range of galaxy models, from SMC-like dwarfs {\&} MW-analogues to z{\$\sim${}}2 clumpy disks. In massive, gas-rich systems (local starbursts and high-z galaxies), radiation pressure dominates the wind generation. For MW-like spirals and dwarf galaxies the gas densities are much lower, and shock-heated gas from SNe and stellar winds dominates production of large-scale outflows. In all models, however, winds have a multi-phase structure that depends on interactions between multiple feedback mechanisms operating on different spatial {\&} time scales: any single mechanism fails to reproduce the winds observed. We provide fitting functions for wind mass-loading and velocities as a function of galaxy properties, for use in cosmological simulations and semi-analytic models. These differ from typically-adopted formulae with explicit dependence on gas surface density that can be very important in both low-density dwarf galaxies and high-density gas-rich galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1110.4638}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2012.20593.x}, -eprint = {1110.4638}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Stars: formation}, -number = {4}, -pages = {3522--3537}, -title = {{Stellar feedback in galaxies and the origin of galaxy-scale winds}}, -volume = {421}, -year = {2012} -} -@article{Hopkins2011, -abstract = {We present analytic calculations of angular momentum transport and gas inflow in galaxies, from scales of {\$\sim${}}kpc to deep inside the potential of a central massive black hole (BH). We compare these analytic calculations to numerical simulations and use them to develop a sub-grid model of BH growth that can be incorporated into semi-analytic calculations or cosmological simulations. Motivated by both analytic calculations and simulations of gas inflow in galactic nuclei, we argue that the strongest torque on gas arises when non-axisymmetric perturbations to the stellar gravitational potential produce orbit crossings and shocks in the gas. This is true both at large radii {\$\sim${}}0.01-1kpc, where bar-like stellar modes dominate the non-axisymmetric potential, and at smaller radii ≲10pc, where a lopsided/eccentric stellar disc dominates. The traditional orbit-crossing criterion is not always adequate to predict the locations of, and inflow due to, shocks in gas+stellar discs with finite sound speeds. We derive a modified criterion that predicts the presence of shocks in stellar-dominated systems even absent formal orbit crossing. We then derive analytic expressions for the loss of angular momentum and the resulting gas inflow rates in the presence of such shocks. We test our analytic predictions using hydrodynamic simulations at a range of galactic scales, and show that they successfully predict the mass inflow rates and quasi-steady gas surface densities with a small scatter ≃0.3dex. We use our analytic results to construct a new estimate of the BH accretion rate given galaxy properties at larger radii, for use in galaxy and cosmological simulations and semi-analytic models. While highly simplified, this accretion rate predictor captures the key scalings in the numerical simulations. By contrast, alternate estimates such as the local viscous accretion rate or the spherical Bondi rate fail systematically to reproduce the simulations and have significantly larger scatter. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1007.2647}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1365-2966.2011.18542.x}, -eprint = {1007.2647}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Quasars: general}, -number = {2}, -pages = {1027--1050}, -title = {{An analytic model of angular momentum transport by gravitational torques: From galaxies to massive black holes}}, -volume = {415}, -year = {2011} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since z = 1.0. We find that lower mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher mass or lower redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single-aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys; we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xu et al. - 2017 - The inner structure of early-type galaxies in the Illustris simulation.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1824--1848}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {469}, -year = {2017} -} -@article{Holl2012, -abstract = {Gaia, the next astrometric mission of the European Space Agency, will use a camera composed of 106 CCDs to collect multiple observations for one billion stars. The astrometric core solution of Gaia will use the estimated location of the stellar images on the CCDs to derive the astrometric parameters (position, parallax and proper motion) of the stars. The Gaia CCDs will suffer from charge transfer inefficiency (CTI) mainly caused by radiation damage. CTI is expected to significantly degrade the quality of the collected images which ultimately affects the astrometric accuracy of Gaia. This paper is the second and last in a study aiming at characterizing and quantifying the impact of CCD radiation damage on Gaia astrometry. Here we focus on the effect of the image location errors induced by CTI on the astrometric solution. We apply the Gaia Astrometric Global Iterative Solution (AGIS) to simulated Gaia-like observations for 1 million stars including CTI-induced errors as described in the first paper. We show that a magnitude-dependent image location bias is propagated in the astrometric solution, biasing the estimation of the astrometric parameters as well as decreasing its precision. We demonstrate how the Gaia scanning law dictates this propagation and the ultimate sky distribution of the CTI-induced errors. The possibility of using the residuals of the astrometric solution to improve the calibration of the CTI effects is investigated. We also estimate the astrometric errors caused by (faint) disturbing stars preceding the stellar measurements on the CCDs. Finally, we show that, for single stars, the overall astrometric accuracy of Gaia can be preserved to within 10per cent of the CTI-free case for all magnitudes by appropriate modelling at the image location estimation level and using the solution residuals. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.1547}, -author = {Holl, B and Prod'homme, T and Lindegren, L and Brown, A G A}, -doi = {10.1111/j.1365-2966.2012.20429.x}, -eprint = {1110.1547}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: numerical,Space vehicles}, -number = {4}, -pages = {2786--2807}, -title = {{The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solution}}, -volume = {422}, -year = {2012} -} -@article{Baudis2017, -abstract = {The dark matter problem is almost a century old. Since the 1930s evidence has been growing that our cosmos is dominated by a new form of non-baryonic matter that holds galaxies and clusters together and influences cosmic structures up to the largest observed scales. At the microscopic level, we still do not know the composition of this dark, or invisible, matter, which does not interact directly with light. The simplest assumption is that it is made of new particles that interact with gravity and, at most, weakly with known elementary particles. I will discuss searches for such new particles, both space- and Earth-bound, including those experiments placed in deep underground laboratories. While a dark matter particle has not yet been identified, even after decades of concerted efforts, new technological developments and experiments have reached sensitivities where a discovery might be imminent, albeit certainly not guaranteed.}, -archivePrefix = {arXiv}, -arxivId = {hep-ph/0606014}, -author = {Baudis, Laura}, -doi = {10.1017/S1062798717000783}, -eprint = {0606014}, -issn = {14740575}, -journal = {European Review}, -pages = {1--12}, -primaryClass = {hep-ph}, -title = {{The Search for Dark Matter}}, -year = {2017} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -publisher = {MNRAS}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Chu2013, -abstract = {An arbitrary surface mass density of the gravitational lens can be decomposed into multipole components. We simulate the ray tracing for the multipolar mass distribution of the generalized Singular Isothermal Sphere model based on deflection angles, which are analytically calculated. The magnification patterns in the source plane are then derived from an inverse shooting technique. As has been found, the caustics of odd mode lenses are composed of two overlapping layers for some lens models. When a point source traverses this kind of overlapping caustics, the image numbers change by ±4, rather than ±2. There are two kinds of caustic images. One is the critical curve and the other is the transition locus. It is found that the image number of the fold is exactly the average value of image numbers on two sides of the fold, while the image number of the cusp is equal to the smaller one. We also focus on the magnification patterns of the quadrupole (m = 2) lenses under the perturbations of m = 3, 4, and 5 mode components and found that one, two, and three butterfly or swallowtail singularities can be produced, respectively. With the increasing intensity of the high-order perturbations, the singularities grow up to bring sixfold image regions. If these perturbations are large enough to let two or three of the butterflies or swallowtails make contact, then eightfold or tenfold image regions can be produced as well. The possible astronomical applications are discussed. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -author = {Chu, Z. and Lin, W. P. and Li, G. L. and Kang, X.}, -doi = {10.1088/0004-637X/765/2/134}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Chu2013Multipoles.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {gravitational lensing: strong,methods: analytical,methods: numerical}, -number = {2}, -title = {{Multipole gravitational lensing and high-order perturbations on the quadrupole lens}}, -volume = {765}, -year = {2013} -} -@article{Kuhn2021, -abstract = {We present a combined cosmic shear analysis of the modeling of line-of-sight distortions on strongly lensed extended arcs and galaxy shape measurements in the COSMOS field. We develop a framework to predict the covariance of strong lensing and galaxy shape measurements of cosmic shear on the basis of the small scale matter power-spectrum. The weak lensing measurement is performed using data from the COSMOS survey calibrated with a cloning scheme using the Ultra Fast Image Generator UFig [1]. The strong lensing analysis is performed by forward modeling the lensing arcs with a main lensing deflector and external shear components from the same Hubble Space Telescope imaging data set. With a sample of three strong lensing shear measurements we present a 2-sigma detection of the cross-correlation signal between the two complementary measurements of cosmic shear along the identical line of sight. With large samples of lenses available with the next generation ground and space based observatories, the covariance of the signal of the two probes with large samples of lenses allows for systematic checks, cross-calibration of either of the two measurement and the measurement of the small scale shear power-spectrum.}, -archivePrefix = {arXiv}, -arxivId = {2010.08680}, -author = {Kuhn, Felix Arjun and Birrer, Simon and Bruderer, Claudio and Amara, Adam and Refregier, Alexandre}, -doi = {10.1088/1475-7516/2021/04/010}, -eprint = {2010.08680}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Kuhn2020SLWLCOSMOSSHEAR.pdf:pdf}, -issn = {14757516}, -journal = {JCAP}, -keywords = {cosmic web,cosmological simulations,gravitational lensing}, -number = {4}, -title = {{Combining strong and weak lensing estimates in the Cosmos field}}, -volume = {2021}, -year = {2021} -} -@article{Carpenter2017, -abstract = {Stan is a probabilistic programming language for specifying statistical models. A Stan program imperatively defines a log probability function over parameters conditioned on specified data and constants. As of version 2.14.0, Stan provides full Bayesian inference for continuous-variable models through Markov chain Monte Carlo methods such as the No-U-Turn sampler, an adaptive form of Hamiltonian Monte Carlo sampling. Penalized maximum likelihood estimates are calculated using optimization methods such as the limited memory Broyden-Fletcher-Goldfarb-Shanno algorithm. Stan is also a platform for computing log densities and their gradients and Hessians, which can be used in alternative algorithms such as variational Bayes, expectation propagation, and marginal inference using approximate integration. To this end, Stan is set up so that the densities, gradients, and Hessians, along with intermediate quantities of the algorithm such as acceptance probabilities, are easily accessible. Stan can be called from the command line using the cmdstan package, through R using the rstan package, and through Python using the pystan package. All three interfaces support sampling and optimization-based inference with diagnostics and posterior analysis. rstan and pystan also provide access to log probabilities, gradients, Hessians, parameter transforms, and specialized plotting.}, -author = {Carpenter, Bob and Gelman, Andrew and Hoffman, Matthew D and Lee, Daniel and Goodrich, Ben and Betancourt, Michael and Brubaker, Marcus A and Guo, Jiqiang and Li, Peter and Riddell, Allen}, -doi = {10.18637/jss.v076.i01}, -issn = {15487660}, -journal = {Journal of Statistical Software}, -keywords = {Algorithmic differentiation,Bayesian inference,Probabilistic program,Stan}, -number = {1}, -title = {{Stan: A probabilistic programming language}}, -volume = {76}, -year = {2017} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by an internal driver and a positive feedback mechanism, which creates regular geometric and/or temporal patterns and decreases the entropy, in contrast to random processes. Here we investigate for the first time a comprehensive number of 16 self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous {\{}{\$}\backslash{\$}sl order out of chaos{\}}, during the evolution from an initially disordered system to an ordered stationary system, via quasi-periodic limit-cycle dynamics, harmonic mechanical resonances, or gyromagnetic resonances. The internal driver can be gravity, rotation, thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational instability, the Rayleigh-B{\$}\backslash{\$}'enard convection instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or loss-cone instability. Physical models of astrophysical self-organization processes involve hydrodynamic, MHD, and N-body formulations of Lotka-Volterra equation systems.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C M and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G and Scargle, Jeffrey D and Melatos, Andrew and Wagoner, Robert V and Trimble, Virginia and Green, William H}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Arquitectura2015, -abstract = {Predicting the binding mode of flexible polypeptides to proteins is an important task that falls outside the domain of applicability of most small molecule and protein−protein docking tools. Here, we test the small molecule flexible ligand docking program Glide on a set of 19 non-$\alpha$-helical peptides and systematically improve pose prediction accuracy by enhancing Glide sampling for flexible polypeptides. In addition, scoring of the poses was improved by post-processing with physics-based implicit solvent MM- GBSA calculations. Using the best RMSD among the top 10 scoring poses as a metric, the success rate (RMSD ≤ 2.0 {\AA} for the interface backbone atoms) increased from 21% with default Glide SP settings to 58% with the enhanced peptide sampling and scoring protocol in the case of redocking to the native protein structure. This approaches the accuracy of the recently developed Rosetta FlexPepDock method (63% success for these 19 peptides) while being over 100 times faster. Cross-docking was performed for a subset of cases where an unbound receptor structure was available, and in that case, 40% of peptides were docked successfully. We analyze the results and find that the optimized polypeptide protocol is most accurate for extended peptides of limited size and number of formal charges, defining a domain of applicability for this approach.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {Arquitectura, Energ{\'{i}}a Y and Introducci, Tulo I and 赫晓霞 and Iv, Tulo and Teatinas, L A S and Conclusiones, Tulo V I I and Contempor{\'{a}}neo, Perspectivas D E U S O and Evaluaci, Tulo V and Ai, Farshad and Jakubiec, John Alstan and Weeks, Digital Photography COMPLETE COURSE Learn Everithing You Need to Know in 20 and Mu, Ari and Inan, Tuǧba and {Sierra Garriga}, Carlos and Library, Pao Yue-kong and Hom, Hung and Kong, Hong and Castilla, Nuria and Uzaimi, Achmad and {Febriand Abdel}, Jack and Armaidah, Rita and Por, Paso and Para, Paso and Pol, Responsables and Julio, Ticos and La, Antecedentes and Herder, De and Olbina, Svetlana and {Valerio Ubierna}, Ignacio and Hafiz, Dalia O and Jones, James R and Gibbons, Ronald B and Schubert, Robert and Araji, Mohamad T and رسولی, چاپار and Sky, Date and Mbe, H P R and Mbe, Perez and Rmse, H P R and Rmse, Perez and Calculo, Pr{\'{a}}ctica and Phantom, D E L and Toma, Toma and Media, Toma and Bertolotti, Dimas and Karmarkar, Bharati and Mu, Ari and Jacobsson, Emma and Eriksson, Fredrik and Pereira, Alvaro Luis dos Santos and Amaral, G. and Bushee, J. and Cordani, U. G. and KAWASHITA, KOJI and Reynolds, J. H. and ALMEIDA, Fernando FL{\'{A}}VIO MARQUES De E and de Almeida, F. F.M. and Hasui, Y. and {de Brito Neves}, B. B. and Fuck, R. A. and Oldenzaal, Zorgcentrum and Guida, Aim{\'{e}}e and Tchalenko, J S and Peacock, David C.P. and Sanderson, David J. and Rotevatn, Atle and Nixon, C. W. and Rotevatn, Atle and Sanderson, David J. and Zuluaga, L. F. and Dimmen, V. and Rotevatn, Atle and Sanderson, David J. and 1 and Peacock, David C.P. and Nixon, C. W. and Rotevatn, Atle and Sanderson, David J. and Zuluaga, L. F. and Crider, Juliet G. and Tjia, H D and Kim, Young Seog and Peacock, David C.P. and Sanderson, David J. and Katz, Yoram and Weinberger, Ram and Aydin, Atilla and Peacock, David C.P. and Marrett, Randall and Peacock, David C.P. and Doblas, Miguel and Petit, J. P. and Hancock, P. L. and Barka, A. A. and Barron, K and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and Souza, Iata Anderson De E and Viana, Adilson and J{\'{u}}nior, Soares and {Jacques Angelier} and Angelier, Jacques and Mechler, P. and Burini, Arthur and Marginal, Brazilian and Clemente, Pilar and Beasley, Craig J and Dribus, John R and Mawson, By Nicola and Tubbs, Bonnie and Fugita, A. M. and Jos, Mareio and Magalh, Jullano and {ANP - Ag{\^{e}}ncia Nacional do Petr{\'{o}}leo} and Garcia, S{\'{a}}vio Francis de Melo and Filho, Andr{\'{e}} Danderfer Antonio Thomaz and Lamotte, Dominique Frizon De and Rudkiewicz, Jean Luc and Lima, Jo{\~{a}}o Victor and Mohriak, Webster Ueipass and Pereira, M{\'{a}}rcio J and Moreira, Jobel Louren{\c{c}}o Pinheiro and Valdetaro, Claudio and Gil, Jo{\^{a}}o Alexandre and Machado, Marco Ant{\^{o}}nio Pinheiro and Souza, Iata Anderson De E and Dirk, Hans and Castro, Joel Carneiro De and {De Geoci{\^{e}}ncias}, Instituto and {De P{\'{o}}s-Gradua{\c{c}}{\~{a}}o}, Programa and Geoci{\^{e}}ncias, Em and Balbinot, Mariana and {Da Bacia De Santos}, Cret{\'{a}}ceo-Terci{\'{a}}rio and Chang, Hung Kiang and Matos, Gabriel Correa De and Lima, Rodrigo Dias and Santos, Bacia De E and Haupert, Isabelle and Manatschal, Gianreto and Decarlis, Alessandro and Unternehr, Patrick and Macedo, Juliano Magalh{\~{a}}es and Corr{\^{e}}a, Fernando Santos and Alberto, Gustavo and Jorge, Correia and Corr{\^{e}}a, Rui and Bueno, Gilmar Vital and {A. C. Vidal, C. H. Kiang, F. S. Correa, F. L. Fernandes, J. C. de Castro, J. S. Tinen, L. Koike}, M. L. Assine and S. P. Rostirolla and Moreira, Jobel Louren{\c{c}}o Pinheiro and Esteves, Carlos Augusto and Rodrigues, Jos{\'{e}} Joaquim and de Vasconcelos, Claudemir Severiano and {De Mio}, Eduardo and Chang, Hung Kiang and Corr{\^{e}}a, Fernando Santos and Santos, Bacia De E and Barroso, Alberto Silva and Tarc{\'{i}}sio, Celso and Silva, De Souza Da and Carlos, Luiz Luis and Pires, Gomes L.C. and Damasceno, Luis Carlos and Filoco, Paulo Roberto and Assine, Mario Luis M{\'{a}}rio Luis and Corr{\^{e}}a, Fernando Santos and Chang, Hung Kiang and Santos, Bacia De E and Balbinot, Mariana and Santos, Bacia De E and Dolares, Maria and Carvalho, De and Pra{\c{c}}a, Uyara Mundlm and De, Jos{\^{e}} Jorge and Vincentelli, Maria Gabriela C and Barbosa, Mauro and Karam*, M{\'{a}}rcia Kuhn and Porto, Roberto and Saito, Makoto and Contreras, Jorham and Z{\"{u}}hlke, Rainer and Bowman, Scott and Bechst{\"{a}}dt, Thilo and Moreira, Jobel Louren{\c{c}}o Pinheiro and Carminatti, M{\'{a}}rio and Chang, Hung Kiang and Assine, Mario Luis M{\'{a}}rio Luis and Corr{\^{e}}a, Fernando Santos and Tinen, Julio Setsuo and Vidal, Alexandre Campane and Koike, Luzia and Garcia, S{\'{a}}vio Francis de Melo and Letouzey, Jean and Rudkiewicz, Jean Luc and {Danderfer Filho}, Andr{\'{e}} and {Frizon de Lamotte}, Dominique and {Hung Kiang Chang} and Kowsmann, Renato Oscar and Figueiredo, Antonio M.G. Manuel Ferreira and Bender, Andr{\'{e}}Adriano and Zal{\'{a}}n, Pedro Victor and Paulo, Universidade D E S {\~{A}} O A O and N, Publica{\c{c}}{\~{a}}o Especial and Ulbrich, HORSTPETER H. G. J. and Miranda, Carlos Eduardo and Aslanian, Daniel and Moulin, Maryline and Olivet, Jean Louis and Unternehr, Patrick and Matias, Luis and Bache, Fran{\c{c}}ois and Rabineau, Marina and Nouz{\'{e}}, Herv{\'{e}} and Klingelheofer, Frauke and Contrucci, Isabelle and Labails, Cinthia and Fluminense, Universidade Federal and Blaich, Olav A. and Faleide, Jan Inge and Tsikalas, Filippos and Gordon, A. C. and Mohriak, Webster Ueipass and Brune, Sascha and Williams, Simon E. and {Dietmar M{\"{u}}ller}, R. and Cobbold, Peter R. and Davy, P. and Gapais, D. and Rossello, E. A. and Sadybakasov, E. and Thomas, J. C. and {Tondji Biyo}, J. J. and de Urreiztieta, M. and Meisling, Kristian E. and Cobbold, Peter R. and Mount, Van S. and Suria, Chandra and Legg, Christopher and Gordon, Stuart and Crawford, Mike and He, Zhiyong and Elliot, Ed and Quo, Lih and Chiossi, Dario and Green, Paul F and Japsen, Peter and Bonow, Johan and Cogn{\'{e}}, Nathan and Gallagher, Kerry and Cobbold, Peter R. and Riccomini, CL{\'{A}}UDIO Claudio and Gautheron, Cecile and Strozyk, Frank and Back, Stefan and Kukla, Peter A. and Mohriak, Webster Ueipass and Bassetto, Marcelo and Vieira, Ines Santos and Stanton, Natasha and Schmitt, Renata da Silva and Galdeano, A. and Maia, M{\'{a}}rcia and Mane, M. A. and Dehler, Nolan Maia and Magnavita, Luciano Portugal and Gomes, Leonardo Correa Lucy and Rigoti, Caesar Augusto and de Oliveira, Jo{\~{a}}o Alberto Bach and Sant'Anna, Mar{\'{i}}lia Vidigal and da Costa, Felipe Garcia Domingues and Gallagher, Kerry and Hawkesworth, Chris J. and Mantovani, Marta S.M. M.S. and {Svartman Dias}, Anna Eliza and Hayman, Nicholas W. and Lavier, Luc L. and Direen, Nicholas G. and Stagg, Howard M.J. and Symonds, Philip A. and Norton, Ian O. and Evain, M and Afilhado, A and Rigoti, Caesar Augusto and Loureiro, A and Alves, D and Klingelhoefer, Frauke and Feld, A and Fuck, R. A. and Soares, J and Evain, M and Afilhado, A and Rigoti, Caesar Augusto and Loureiro, A and Alves, D and Brenner, Thomas and Ferrari, ANDR{\'{E}} LUIZ and Penha, H{\'{e}}lio and Silva, A and Alves, E C and Franke, Dieter and Gallagher, Kerry and Hawkesworth, Chris J. and Mantovani, Marta S.M. M.S. and Garcia, S{\'{a}}vio Francis de Melo and Letouzey, Jean and Rudkiewicz, Jean Luc and {Danderfer Filho}, Andr{\'{e}} and {Frizon de Lamotte}, Dominique and Gomes, Paulo Ot{\'{a}}vio and Kilsdonk, Bill and Grow, Tim and Minken, Jon and Barragan, Roberto and Heine, C. and Zoethout, J. and M{\"{u}}ller, R. Dietmar and Souza, Iata Anderson De E and Kellogg, J. N. and Mohriak, Webster Ueipass and Kvarven, Trond and Mjelde, Rolf and Hjelstuen, Berit Oline and Faleide, Jan Inge and Thybo, Hans and Flueh, Ernst R. and Murai, Yoshio and Lavier, Luc L. and Manatschal, Gianreto and Cobbold, Peter R. and Meisling, Kristian E. and Mount, Van S. and de Souza, Pricilla Cam{\~{o}}es Martins and Schmitt, Renata da Silva and Stanton, Natasha and Lima, Jo{\~{a}}o Victor and Mohriak, Webster Ueipass and Paula, Osni B. and Leroy, Sylvie and Rosendahl, B. R. and Nem{\v{c}}ok, Michal and Enciso, G. and Fainstein, Roberto and Moulin, Maryline and Aslanian, Daniel and Rabineau, Marina and Patriat, Martin and Matias, Luis and Olivet, Jean Louis and Contrucci, Isabelle and Matias, Luis and G{\'{e}}li, Louis and Klingelhoefer, Frauke and Nouz{\'{e}}, Herv{\'{e}} and R{\'{e}}hault, Jean Pierre and Unternehr, Patrick and Riccomini, CL{\'{A}}UDIO Claudio and Peloggia, A. U.G. and Saloni, J. C.L. and Kohnke, M. W. and Figueira, R. M. and Nem{\v{c}}ok, Michal and Henk, A. and Allen, R. and Sikora, P. J. and Stuart, C. J. and Rosendahl, B. R. and Welker, C. and Smith, S and Nem{\v{c}}ok, Michal and Sinha, Sudipta T. and Stuart, C. J. and Welker, C. and Choudhuri, M. and Sharma, S. P. and Misra, Achyuta Ayan and Sinha, N. and Venkatraman, S. and P{\'{e}}rez-Gussinye, Marta and Richetti, P. C. and Schmitt, Renata da Silva and Reeves, C. and Clerc, Camille and Ringenbach, Jean Claude and Jolivet, Laurent and Ballard, Jean Fran{\c{c}}ois and Savastano, V{\'{i}}tor Lamy Mesiano and Schmitt, Renata da Silva and de Ara{\'{u}}jo, M{\'{a}}rio Neto Cavalcanti and Inoc{\^{e}}ncio, Leonardo Campos and Scotchman, I. C. and Gilchrist, G. and Kusznir, N. J. and Roberts, A. M. and Fletcher, R. and Sibuet, Jean Claude and Tucholke, Brian E. and de Souza, Pricilla Cam{\~{o}}es Martins and Schmitt, Renata da Silva and Stanton, Natasha and Ponte-Neto, Cosme and Bijani, Rodrigo and Masini, Emmanuel and Fontes, S. and Flexor, J. M. and Ponte-Neto, Cosme and Bijani, Rodrigo and Ibanez, Delano M. and Pestilho, Andr{\'{e}} L.S. and Turra, Bruno B. and Destro, Nivaldo and Miranda, Fernando P. and Riccomini, CL{\'{A}}UDIO Claudio and Lammoglia, Talita and Dubois, Daniel S. and Schmidt, Jaques S. and Cogn{\'{e}}, Nathan and Cobbold, Peter R. and Riccomini, CL{\'{A}}UDIO Claudio and Gallagher, Kerry and Stica, Juliano M and Zal{\'{a}}n, Pedro Victor and Ferrari, ANDR{\'{E}} LUIZ and Sant'Anna, L. G. and Riccomini, CL{\'{A}}UDIO Claudio and Rodrigues-Francisco, B. H. and Sial, Alcides Nobrega and Carvalho, M. D. and Moura, C. A.V. and Gomes, Paulo Ot{\'{a}}vio and Kilsdonk, Bill and Minken, Jon and Grow, Tim and Barragan, Roberto and Parry, Jonathan and Martins, Wisley and {Engelmann de Oliveira}, Christie Helouise and Jelinek, Andr{\'{e}}a Ritter and Chemale, Farid and Cupertino, Jos{\'{e}} Ant{\^{o}}nio and {THOMAZ FILHO}, Antonio ANT{\^{O}}NIO and MIZUSAKI, Ana Maria Pimentel and MILANI, EDISON JOSE and Cesero, PEDRO DE and Ussami, Naomi and Chaves, Carlos Alberto Moreno and Marques, Leila Soares and Ernesto, Marcia and Heidbach, O. and Rajabi, M. and Reiter, K. and Ziegler, M. and Cordani, Renato and Shukowsky, Wladimir and Agarwal, V K and Huang, C H and Physics, Engineering and Clemson, J. and Cartwright, J. and Booth, J. and Daly, M. C. and Chorowicz, J. and Fairhead, J. D. and I, John a Dunbar and Sawyer, Dale S and Gibson, G. M. and Totterdell, J. M. and White, L. T. and Mitchell, C. H. and Stacey, A. R. and Morse, M. P. and Whitaker, A. and Modisi, M. P. and Atekwana, E. A. and Kampunzu, A. B. and Ngwisanyi, T. H. and Moulin, Maryline and Aslanian, Daniel and Scheck, Magdalena and Bayer, Ulf and Otto, Volker and Lamarche, Juliette and Banka, Dirk and Pharaoh, T. Tim and van Wijk, J. W. and Ashby, D and {MACHADO J{\'{U}}NIOR}, DELZIO DE LIMA and Srivastava, Rajesh K. and ALMEIDA, Fernando FL{\'{A}}VIO MARQUES De E and Carneiro, CELSO DAL R{\'{E}} and Bellieni, Giuliano and Com{\'{i}}n, P and Marques, Leila Soares and Melfi, A. J. and Piccirillo, Enzo M. and Nardy, Antonio Jos{\'{e}} Ranalli and Rosemberg, A and McNulty, Judiann and Clark, David A. and Coelho, Raphael Martins and Chaves, Alexandre de Oliveira and Buckingham, David and Sefton-Green, Julian and {Vianna Coutinho}, Jos{\'{e}} Moacyr and Almeida, Julio C.H. J{\'{u}}lio Julio and Dios, Fatima and Mohriak, Webster Ueipass and Valeriano, Claudio de Morisson CL{\'{A}}UDIO DE MORISSON Claudio De Morisson and Heilbron, MONICA and Eirado, Luiz Guilherme and Tomazzoli, Edison Ramos and Wl, G and Cordani, U. G. and Kawaseita$\sim$, K and Reynolds$\sim$, J H and Brazil, S&o Paulo and Bennio, L. and Brotzu, P. and D'Antonio, M. and Feraud, G. and Gomes, Celso B. de Barros and Marzoli, Andrea and Melluso, Leone and Morbidelli, L. and Morra, Vincenzo and Rapaille, Cedric and Ruberti, Excelso and de SOUZA, B. T. and Carvas, Karine Zuccolan and Chaves, Alexandre de Oliveira and {de Oliveira Chaves}, Alexandre and Neves, Jos{\'{e}} Luiz Peixoto Marques Correia and Em, Mestrado and P{\'{u}}blica, Sa{\'{u}}de and Paper, Conference and Tupinamb, Miguel and Nordeste, Setores Centro-norte E and Enxame, D O and Da, D E Diques and Corval, Artur and Valente, S.C. S{\'{e}}rgio de Castro Sergio de Castro and Duarte, Beatriz Paschoal B.P. and Famelli, N. and Zanon, M. and Deckart, Katja and F{\'{e}}raud, Gilbert and Marques, Leila Soares and Bertrand, Herv{\'{e}} and P{\'{o}}s-gradua{\c{c}}{\~{a}}o, Programa D E and Sciences, Atmospheric and State, North Carolina and Park, Menlo and Garda, Gianna Maria and Schorscher, Johann Hans Daniel and Do, Universidade and Do, Estado and Janeiro, Rio I O De E and Geologia, Faculdade D E and Guedes, Eliane and Heilbron, MONICA and Vasconcelos, Paulo M. and {de Morisson Valeriano}, Cl{\'{a}}udio Claudio and {Horta de Almeida}, J{\'{u}}lio C{\'{e}}sar and Teixeira, Wilson and Filho, Andr{\'{e}} Danderfer Antonio Thomaz and 关华 and Guedes, Eliane and Heilbron, MONICA and {de Morisson Valeriano}, Cl{\'{a}}udio Claudio and de Almeida, Julio Cesar Horta C{\'{e}}sar Horta Cesar Horta and Szatmari, Peter and Magalh{\~{a}}es, Joana and Matos, Lara and metode penelitian {Nursalam, 2016} and Bhiwapurkar, Nitin and Rathi, Manoj and Mohan, Ned and NGONGE, EMMANUEL DONALD and Pires, Paulo Roberto and Geologia, Disserta{\c{c}}{\~{a}}o De Mestrado and Tomba, C.L.B. and Trotta, Mario Cesar and Turner, Simon P. and Regelous, Marcel and Kelley, Simon and Hawkesworth, Chris J. and Mantovani, Marta S.M. M.S. and Lobo, Jana{\'{i}}na Teixeira and Duarte, Beatriz Paschoal B.P. and Szatmari, Peter and Valente, S.C. S{\'{e}}rgio de Castro Sergio de Castro and Corval, Artur and Duarte, Beatriz Paschoal B.P. and Ellam, Robert M. and Fallick, Anthony E. and Meighan, Ian Gordon and Dutra, Thiago and Ernesto, Marcia and Raposo, Maria I.B. Irene Bartolomeu and Marques, Leila Soares and Renne, Paul Randall and Diogo, L. A. and {De Min}, Angelo and Florisbal, Luana Moreira and Heaman, Larry M. and {de Assis Janasi}, Valdecir and {de Fatima Bitencourt}, Maria and Hergt, J. M. and Peate, David W. and Hawkesworth, Chris J. and Hou, Guiting and Jourdan, Fred and F{\'{e}}raud, Gilbert and Bertrand, Herv{\'{e}} and Watkeys, M. K. and Kampunzu, A. B. and {Le Gall}, B. and Kouamo, No{\"{e}}l Aim{\'{e}}e Keutchafo and Tchaptchet, Depesquidoux Tchato and Ngueguim, Anne Laure Tezanou and Wambo, Nicole Armelle Simeni and Tchouankoue, Jean Pierre and Cucciniello, Ciro and Lare, C O C and Reland, I and Mcnamara, Maria E and Machado, F{\'{a}}bio Braz and Rocha-J{\'{u}}nior, Eduardo Reis Viana R.V. and Marques, Leila Soares and Nardy, Antonio Jos{\'{e}} Ranalli and Zezzo, Larissa Vieira and Marteleto, Natasha Sarde and Ernesto, Marcia and Marteleto, Natasha Sarde and Mcmaster, Michael and Almeida, Julio C.H. J{\'{u}}lio Julio and Heilbron, MONICA and Guedes, Eliane and Mane, M. A. and Linus, J. H. and Motoki, Akihisa and Sichel, Susanna Eleonora and Petrakis, Giannis Hans and Renne, Paul Randall and Glen, Jonathon M Jonathan M. and Milner, Simon C. and Duncan, Andrew R. and Hall, Walton and Keynes, Milton and Peate, David W. and Urubici, Y and Gramado, Y and Raposo, Maria I.B. Irene Bartolomeu and Ernesto, Marcia and Renne, Paul Randall and Santiago, Ra{\'{i}}ssa and Caxito, Fabr{\'{i}}cio de Andrade and Neves, Mirna Aparecida and Dantas, Elton Luiz and de {Medeiros J{\'{u}}nior}, Edgar Batista and Queiroga, Gl{\'{a}}ucia Nascimento and Renne, Paul Randall and Ernesto, Marcia and Pacca, G and Coe, Robert S and Glen, Jonathon M Jonathan M. and Prevot, Michel and Perrin, Mireille and Deckart, Katja and Ernesto, Marcia and F{\'{e}}raud, Gilbert and Piccirillo, Enzo M. and Santos, Adjacente C. {\`{A}} Bacia D E and Brasil, S- S E D O and Agashev, A M and Takazawa, Eiichi and Albar{\'{e}}de, F and Modeling, Geochemical and York, New and Chester, Port and Pyle, David and Kumar, Santosh and Stewart, Kathy and Turner, Simon P. and Kelley, Simon and Hawkesworth, Chris J. and Kirstein, Linda A. and Mantovani, Marta S.M. M.S. and Thiede, David S. and Vasconcelos, Paulo M. and Vasconcelos, David L. and Bezerra, Francisco H.R. and Clausen, Ole R. and Medeiros, Walter E. and de Castro, David L. and Vital, Helenice and Barbosa, Jos{\'{e}} A. Roberto and White, R. and McKenzie, D. and Will, Thomas M. and Frimmel, Hartwig E. and Alves, Costa F. and Ferrari, ANDR{\'{E}} LUIZ and J{\'{u}}nior, Cleber Peralta Gomes and Fossen, Haakon and Jackson, Chris and Rotevatn, Atle and Preto, Federal De Ouro and Zerfass, Henrique and {Chemale Junior}, Farid and {Paulo Ot{\'{a}}vio Gomes}, Bill Kilsdonk Jon Minken Tim Grow and Roberto Barragan and Granot, Roi and Dyment, J{\'{e}}r{\^{O}}me and Hartwig, Marcos Eduardo and Heilbron, MONICA and Machado, NUNO and Valeriano, Claudio de Morisson CL{\'{A}}UDIO DE MORISSON Claudio De Morisson and Valladares, CL{\'{A}}UDIA SAY{\~{A}}O Claudia and Machado, NUNO and Pedrosa-soares, Ant{\^{o}}nio Carlos and Carlos, Luiz Luis and Allard, Rudolph and Trouw, Johannes and Mohriak, Webster Ueipass and Valerianol, M and Milani, J and Almeida, Julio C.H. J{\'{u}}lio Julio and Tupinambfil, M and Petreo, P and Tupinamb{\'{a}}, Miguel and Valeriano, Claudio de Morisson CL{\'{A}}UDIO DE MORISSON Claudio De Morisson and Armstrong, Richard and {Do Eirado Siva}, Luiz Guilherme and Melo, Renata Seibel and Simonetti, Antonio and {Pedrosa Soares}, Antonio Carlos and Machado, NUNO and Heine, C. and Zoethout, J. and M{\"{u}}ller, R. Dietmar and Caldeira, Jefter and Kirstein, Linda A. and Kelley, Simon and Hawkesworth, Chris J. and Turner, Simon P. and Mantovani, Marta S.M. M.S. and Wijbrans, Jan and Kumar, Naresh and Danforth, A. Al and Nuttall, P. and Helwig, J. and Bird, D. E. and Venkatraman, S. and Acharya, Tapas and Nag, Sisir Kanti and Basumallik, Sukumar and Almeida, Julio C.H. J{\'{u}}lio Julio and Heilbron, MONICA and Valeriano, Claudio de Morisson CL{\'{A}}UDIO DE MORISSON Claudio De Morisson and Acharya, Tapas and Mallik, Sukumar Basu and Ectono, E Volu{\c{c}}{\~{a}}o T and Do, Strutural and Ar{\'{e}}u, C Ampo D E X and Boyer, Robert E and Mcqueen, Jereld E and Morelli, M. and Piana, F. and Coward, M. P. and Daly, M. C. and da Concei{\c{c}}{\~{a}}o, Rommulo Vieira Raimundo Almir Costa and Ferreira, Joaquim M. and Bezerra, Francisco H.R. and Sousa, Maria O.L. and do Nascimento, Aderson F. and S{\'{a}}, Jaziel M. and Fran{\c{c}}a, George S. and {شجاعی، رؤیا} and Gontijo-Pascutti, Ambrosina Helena Ferreira and Cesar, Julio and Almeida, Horta De and Bezerra, Francisco H.R. and Terra, Emanuele La and Almeida, Julio C.H. J{\'{u}}lio Julio and Hobbs, W. H. and Hodgson, Robert A and Jacques, Patricia Duringer and Machado, R{\^{o}}mulo and Nummer, Alexis Rosa and {De Oliveira}, Roberto Gusm{\~{a}}o and Ferreira, Francisco Jos{\'{e}} Fonseca and {De Castro}, Lu{\'{i}}s Gustavo and Nummer, Alexis Rosa and Justo, A N A Paula and Wild, J and Tir{\'{e}}n, Sven and Anisimova, O. V. and Koronovsky, N. V. and Chiang, Liu Chan and Liu, Chan Chiang and Franco-Magalh{\~{a}}es, Ana Olivia Barufi and Hackspacher, Peter Christian and Saad, Antonio Roberto and Estado, Capes-universidade D O and Rio, D O and Vol, Nature and Zealand, New and Island, North and Islands, Kurile and {De Lima}, Jose Valdeni and Nag, Sisir Kanti and Chakraborty, Surajit and Leary, D W O and Friedman, J D and Pohn, H A and Solomon, Semere and Ghebreab, Woldai and Gabrielsen, Roy H. and Braathen, Alvar and Dehis, John and Roberts, David and Hickman, M. H. and Nur, Amos and Cort{\'{e}}s, A. L. and Soriano, M. A. and Maestro, A. and Casas, A. M. and Good, Nadine and {De Wit}, Maarten J. and Sarti, Therence Paoliello and Fisiograficos, Aspectos and Anteriores, Trabalhos and Geol, Contexto and Brasiliano, Evento and Ribeira, Faixa and Litoestratigr, Unidade and Estruturais, Aspectos and Geol, Contexto and Tect, Regimes and Continentais, Rifts and Meso-cenoz, Tecnonismo and Bibliogr, Pesquisa and Fundamentais, D E Conceitos and Estrutural, D E Geologia and Wheeler, Russell L. and Pinto, Victor Hugo and Wilson, J. T. and Misra, Achyuta Ayan and Mukherjee, Soumyajit and Edition, Second and Geraldes, Mauro Cesar C{\'{e}}sar and Weizsacker, Von and Weizsacker, Von and {شجاعی، رؤیا} and Terrestre, Crosta and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and Sr, Rb- and Pb, Pb and Pb, Pb and Th, Th and Unidos, Estados and Drilling, Scientific Ocean and Trouw, Rudolph A J and Mandl, Georg and metode penelitian {Nursalam, 2016} and Machado, NUNO and Valladares, CL{\'{A}}UDIA SAY{\~{A}}O Claudia and Heilbron, MONICA and Valeriano, Claudio de Morisson CL{\'{A}}UDIO DE MORISSON Claudio De Morisson and {MACHADO J{\'{U}}NIOR}, DELZIO DE LIMA and Grande, Barra and Almeida, Julio C.H. J{\'{u}}lio Julio and Peternel, Rodrigo and Ramos, Renato R Cabral and Guimar{\~{a}}es, Paulo V and Rodrigues, Sergio W De O and Rezende, Estev{\~{a}}o M C De and P{\'{e}}rico, Rafael and Costa, Vitor and Np, Em and Effektivwert, Echter and Marc{\'{e}}n, M. and Casas-Sainz, A. M. and Rom{\'{a}}n-Berdiel, T. and Griera, A. and Santanach, P. and Pocov{\'{i}}, A. and Gil-Imaz, A. and Aldega, L. and Izquierdo-Llavall, E. and Marques, Leila Soares and {De Min}, Angelo and Rocha-J{\'{u}}nior, Eduardo Reis Viana R.V. and Babinski, M. and Bellieni, Giuliano and Figueiredo, Antonio M.G. Manuel Ferreira and Merdith, Andrew S. and Williams, Simon E. and Brune, Sascha and Collins, Alan S. and M{\"{u}}ller, R. Dietmar and Mohriak, Webster Ueipass and Danforth, A. Al and Post, Paul J. and Brown, David E. and Tari, Gabor C. and Nem{\v{c}}ok, Michal and Sinha, Sudipta T. and Moulin, Maryline and Aslanian, Daniel and Unternehr, Patrick and Cai, Chen and Wiens, Douglas A. and Shen, Weisen and Eimer, Melody and {Andr{\'{e}} Pires Negr{\~{a}}o} and N{\"{u}}rnberg, Dirk and M{\"{u}}ller, R. Dietmar and Gravim, Dados and Setentrional, Nordeste and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and Elisa, Dr{\textordfeminine} and Rocha, Soares and Ufg, Barbosa and Augusto, Pedro Prof and Silva, De Souza Da and Pequeno, M{\^{o}}nica Alves and metode penelitian {Nursalam, 2016} and Mukasa, Samuel B. and Flower, Martin F.J. and Miklius, Asta and Marques, Leila Soares and Ulbrich, Mabel N.C. C. and Ruberti, Excelso and Tassinari, Colombo G. C.G. Celso Gaeta C.G. and Fodor, R. V. and Hanan, B. B. and Motoki, Akihisa and Vargas, Thais Tha{\'{i}}s and Iwanuch, Woldemar and {Da Silva}, Samuel and Balmant, Alex and Gon{\c{c}}alves, Juliana and Sichel, Susanna Eleonora and Mello, Sidney Luiz Matos and Motoki, Kenji Freire and Aires, Jos{\'{e}} Ribeiro and Siebel, W. and Becchio, R. and Volker, F. and Hansen, M. A.F. and Viramonte, J. and TRUMBULL, R. B. and Haase, G. and Zimmer, M. and Weaver, Barry L. and Saka, Hiroyasu and Weaver, Barry L. and Kar, Aditya and Davidson, Jon and Colucci, Mike and Cordani, U. G. and Teixeira, Wilson and D'Agrella-Filho, M. S. and Trindade, R. I. and Filho, Andr{\'{e}} Danderfer Antonio Thomaz and de Cesero, Pedro and MIZUSAKI, Ana Maria Pimentel and Le{\~{a}}o, Joana Gisbert and Santos, Rodrigo Bijani Rosana N. and Marques, Leila Soares and Sturm, R. and Grange, M. and Scharer, U. and Merle, R. and Girardeau, J. and Cornen, G. and Comin-Chiaramonti, PIERO and Junqueira-Brod, TEREZA CRISTINA and ROIG, HENRIQUE LLACER and Gaspar, JOS{\'{E}} CARLOS and Brod, JOS{\'{E}} AFFONSO and MENESES, PAULO ROBERTO and Aguirre, Luis and Controles, E and Dos, G{\^{e}}nese and F{\'{o}}sforo, Dep{\'{o}}sitos D E and Doutorado, Tese D E and Prof, Orientador and Carlos, Jos{\'{e}} and Ig, Gaspar and Claudinei, Prof and Oliveira, Gouveia De and Unb, I G and Augusto, Pedro Prof and Bittencourt, Cesar and Ig, Pires and Maria, Profa and Motta, Cristina and Usp, De Toledo and Df, Bras{\'{i}}lia and Lopes, Jos{\'{e}} Carrilho and Niu, Yaoling and Wilson, Marjorie and Humphreys, Emma R. and O'Hara, Michael J. and Hirano, Naoto and Machida, Shiki and Abe, Natsue and Morishita, Tomoaki and Tamura, Akihiro and Arai, Shoji and USDA and Let{\'{i}}cia, Mara and Da, Torres and Aitchison, Jean and Huddlestone, Rodney and Pullum, Geoffrey K. and Estadual, Universidade and Microscopy, Carl Zeiss and Mata, Jo{\~{a}}o and Alves, Costa F. and Martins, L{\'{i}}nia and Miranda, Rui and Madeira, Jos{\'{e}} and Pimentel, N. and Martins, S. and Azevedo, Maria Ros{\'{a}}rio and Youbi, Nasrrddine and {De Min}, Angelo and Almeida, I. M. and Bensalah, Mohamed Khalil and Terrinha, Pedro and Motoki, Akihisa and {Chaves Novais}, Luiz Carlos and Motoki, Kenji Freire and Oliveira, Leonardo Costa De and {De Fasolo}, Ricardo Souza and Lima, Adrienne Brito and Putirka, Keith Daniel and Perfit, Michael and Ryerson, F. J. and Jackson, Matthew G. and The, Eochemistry O F Efinitions and The, Volution O F and Kawabata, Hiroshi and Hanyu, Takeshi and Chang, Qing and Kimura, Jun Ichi and Nichols, Alexander R.L. and Tatsumi, Yoshiyuki and Motoki, Akihisa and Novais, Lu{\'{i}}s Carlos Chaves and Sichel, Susanna Eleonora and Neves, Jos{\'{e}} Luiz Peixoto Marques Correia and Aires, Jos{\'{e}} Ribeiro and Jalowitzki, Tiago Luis Reis and Katz, Richard F. and Spiegelman, Marc and Langmuir, Charles H. and Jacobsen, S. B. and Wasserburg, G. J. and Le{\~{a}}o, Zelinda M and Ahmadzadeh, Gholamreza and Zamani, Reza and Albarede, Francis and Aldanmaz, Ercan and K{\"{o}}pr{\"{u}}başi, N. and G{\"{u}}rer, {\"{O}} F. and Kaymak{\c{c}}i, N. and Gourgaud, A. and Allsgre, Claude J and Schiano, Pierre and Lewin, Eric and LARSEN, L. M. and Kogarko, L. N. and Onicas, O E S Tect and Eleonora, Susanna and Maria, Cristina and Campos, Pinheiro De and Alves, Costa F. and {CARMICHAEL ISE} and {NICHOLLS J} and {SMITH AL} and Cawthorn, R G and Collerson, K. D. and MORIMOTO, N and Nacional, Museo and Ciencias, De and Putirka, Keith Daniel and Perfit, Michael and Ryerson, F. J. and Jackson, Matthew G. and Haschke, M. and Siebel, W. and G{\"{u}}nther, A. and Scheuber, E. and Exemplos, X and Anderson, Don L. and Armienti, Pietro and Gasperini, Daniela and Motoki, Akihisa and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and Spinelli, Fernando Pelegrini and {De Barros Gomes}, Celso and metode penelitian {Nursalam, 2016} and Douglass, Jill and Schilling, Jean-Guy and Fontignie, Denis and Xu, Yigang and Huang, Xiaolong and Menzies, Martin A. and Wang, Rucheng and Ersoy, Yal{\c{c}}in and Helvaci, Cahit and Geldmacher, J{\"{o}}rg and {Van Den Bogaard}, Paul and Hoernle, Kaj and Schmincke, Hans Ulrich and Hastie, Alan R. and Mitchell, Simon F. and Kerr, Andrew C. and Minifie, Matthew J. and Millar, Ian L. and Delimit{\'{a}}-lo, Almeidianas A O and Geraldes, Mauro Cesar C{\'{e}}sar and Tassinari, Colombo G. C.G. Celso Gaeta C.G. and Babinski, M. and Martinelli, C. D. and Iyer, S. S. and Barboza, E. S. and Pinho, F. E.C. and Onoe, A. T. and Borisov, A. A. and Shapkin, A. I. and Hofmann, Albrecht W. and Jochum, K. P. and Seufert, M. and White, William M. and De, S{\'{e}}ries and THOMPSON, ROBERT N. and Gibson, SALLY A. and Mitghell, J. G. and Dickin, A. P. and Leonardos, O. H. and Brod, JOS{\'{E}} AFFONSO and Greenwood, J. G. and Dada, O. A and Ashano, E. C and Karsli, Orhan and Aydin, Faruk and Sadiklar, M. Burhan and Rudnick, Roberta L and Gao, Shan and Matteini, Massimo and Dantas, Elton Luiz and Pimentel, Marcio M. and B{\"{u}}hn, Bernhard and Samoilov, Valery S. and Vapnik, Yevgeny and Phemister, James and Pilet, S{\'{e}}bastien and Sharp, Warren D. and Renne, Paul Randall and Shcherbakov, Vasily D. and Plechov, Pavel Yu and Izbekov, Pavel E. and Shipman, Jill S. and Smith, Douglas David C. and Atlantic, South East and {Holanda dos Santos}, Werlem and Bergamaschi, S{\'{e}}rgio and Rodrigues, Ren{\'{e}} and {Bezerra da Costa}, Diego Felipe and Chaves, Hernani Aquini Fernandes and THOMPSON, ROBERT N. and Ottley, C. J. and Smith, P. M. and Pearson, D. G. and Dickin, A. P. and Morrison, M. A. and Leat, Philip T. and Gibson, SALLY A. and Clemente, Eliane de Paula Eliene de Paula and Schaefer, Carlos Ernesto G.R. and Oliveira, F{\'{a}}bio Soares and {Albuquerque Filho}, Manoel Ricardo and Alves, Ruy V{\'{a}}lka and S{\'{a}}, Mariana M{\'{e}}dice Firme and Melo, Vander de Freitas and Corr{\^{e}}a, Guilherme Resende and Chakhmouradian, Anton R. and Reguir, Ekaterina P. and Kamenetsky, Vadim S. and Sharygin, Victor V. and Golovin, Alexander V. and Assump{\c{c}}ao, Marcelo and Schimmel, Martin and Escalante, Christian and Barbosa, Jos{\'{e}} A. Roberto and Rocha, Marcelo Peres and Barros, Lucas V. and Cisalhamento, Zonas De and Azzone, Rog{\'{e}}rio Guitarrari and Ruberti, Excelso and {Da Silva}, J{\'{u}}lio C{\'{e}}sar Lopes and {De Barros Gomes}, Celso and Rojas, Gaston Eduardo Enrich and {De Hollanda}, Maria Helena Bezerra Maia and Tassinari, Colombo G. C.G. Celso Gaeta C.G. and MacIntyre, Jane E. and MacIntyre, Jane E. and Bongiolo, Everton M. and Pires, Gomes L.C. and Geraldes, Mauro Cesar C{\'{e}}sar and Santos, Adjacente C. {\`{A}} Bacia D E and Neumann, R. and Green, Nathan L and Usdansky, Steven I and Acevedo, Rogelio D. and Quartino, Bernab{\'{e}} J. and Ersoy, Emrah Yal{\c{c}}in and Beccaluva, Luigi and Bianchini, Gianluca and Natali, Claudio and Siena, Franca and Boomeri, M and Callegaro, Sara and Rapaille, Cedric and Marzoli, Andrea and Bertrand, Herv{\'{e}} and Chiaradia, Massimo and Reisberg, Laurie and Bellieni, Giuliano and Martins, L{\'{i}}nia and Madeira, Jos{\'{e}} and Mata, Jo{\~{a}}o and Youbi, Nasrrddine and {De Min}, Angelo and Azevedo, Maria Ros{\'{a}}rio and Bensalah, Mohamed Khalil and Comin-Chiaramonti, PIERO and {De Min}, Angelo and Girardi, Vicente A.V. and Gomes, Celso B. de Barros and Friedman, Irving and O'Neil, James R JR and Hwang, Jeong and Zheng, Xiangshen and Ripley, Edward M. and Lee, Jong Ik and Shin, Dongbok and Mitchell, Roger H. and Mysen, Bjorn and Turi, B. and Boettcher, AL and O'Neil, James R JR and Brod, JOS{\'{E}} AFFONSO and Gibson, SALLY A. and THOMPSON, ROBERT N. and Junqueira-Brod, TEREZA CRISTINA and SEER, HILDOR JOS{\'{E}} and MORAES, L{\'{U}}CIA CASTANHEIRA DE and BOAVENTURA, GERALDO RESENDE and Burg, Jean Pierre and Bussweiler, Yannick and Foley, Stephen F. and Prelevi{\'{c}}, Dejan and Jacob, Dorrit E. and Analysis, Diopside and Ferrari, ANDR{\'{E}} LUIZ and Riccomini, CL{\'{A}}UDIO Claudio and Campos, Lucia and Lavrado, Helena and Gamboa, L. and Souza, Kaiser De and Geotect{\^{o}}nico, I Contexto and Forma{\c{c}}{\~{a}}o, De and Sudeste, Margem and Troalen, Fr{\'{e}}d{\'{e}}ric and Sedimentares, Bacias and Brasileira, Margem Continental and Sial, Alcides Nobrega and MCreath, Ian and GUSM{\~{A}}O, LUIZ GUILHERME S{\'{A}} and Motoki, Akihisa and Motoki, Kenji Freire and de Melo, Dean Preira and Coltorti, M. and Bonadiman, Costanza and Hinton, R. W. and Siena, Franca and Upton, B. G.J. and Wagner, Jo{\~{a}}o and Castro, Alencar and Chang, Zhaoshan and Vervoort, Jeffery D. and McClelland, William C. and Knaack, Charles and Saunders, A. D. and Langmuir, Charles H. and B{\'{e}}zos, A. and Escrig, S. and Parman, S. W. and Sun, Shen Su and McDonough, William F. and Bryson, John M. and Zindler, A. and Hart, Stanley R. and MARTINSSON, ANDERS and BASSETT, MICHAEL G. and Chakhmouradian, Anton R. and B{\"{o}}hm, C O and Kressall, R D and Lenton, P G and metode penelitian {Nursalam, 2016} and MARTINS-NETO, MARCELO A. and Frisch, Thomas and Colli, Lorenzo and Fichtner, Andreas and Bunge, Hans Peter and Mantle, G. W. and Collins, W. J. and Kushiro, Ikuo and Renda, Imposto D E and Fonte, N A and Verzegnassi, Emerson and Bizzi, L A and Schobbenhaus, C and Stocco, Luana Birchler and Conrad, Clinton P. and Lithgow-Bertelloni, Carolina and das Rochas, Geoquimica and Cient{\'{i}}fica, S{\'{e}}rie and 鷹巣豊治 and Crosby, A. G. and McKenzie, D. and Sclater, John G. and Rahman, S and MacKenzie, W S and Wijbrans, C. H. and Klemme, S. and Berndt, Jasper and Vollmer, C. and Dalton, Colleen A. and Langmuir, Charles H. and Gale, Allison and Dasgupta, Rajdeep and Hirschmann, Marc M. and Smith, Neil D. and Stalker, Kathryn and Davis, F. A. and Hirschmann, Marc M. and Humayun, M. and Bas, Le and Zhang, Li and Meng, Yue and Yang, Wenge and Wang, Lin and Mao, Wendy L. and Zeng, Qiao Shi and Jeong, Jong Seok and Wagner, Andrew J. and Mkhoyan, K. Andre and Liu, Wenjun and Xu, Ruqing and Mao, Ho Kwang and Pesquisa, Pr{\'{o}}-reitoria D E and de Almeida, Vidy{\~{a}} Vieira and Geologia, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o E M and Ara{\c{c}}ua{\'{i}}, Or{\'{o}}geno and Salinas, A Oeste D E and Horizonte, Belo and Weigert, Stefan Cruz and Antoniassi, J. L and Gon{\c{c}}alves, Rhaine Matos and Webster, James D. and Botcharnikov, Roman E. and Dobosi, G. and Fodor, R. V. and Fonseca, Ariadne Do Carmo and Skolotnev, S. G. and Peyve, A. A. and Turko, N. N. and Keskin, Mehmet and Dombroski, Brian A. and Fodor, R. V. and Droop, G. T. R. and Ellam, Robert M. and Ellrs, Devro and WYLLIE, PETER and Ernst, Richard E. and Buchan, Kenneth L. and Davies, D. R. and Rawlinson, N. and Iaffaldano, G. and Campbell, I. H. and EWART, A. and Jalowitzki, Tiago Luis Reis and da Concei{\c{c}}{\~{a}}o, Rommulo Vieira Raimundo Almir Costa and Orihashi, Yuji and Bertotto, Gustavo Walter and Nakai, Shun'ichi and Schilling, Manuel Enrique and SOMMER, CARLOS AUGUSTO and Lima, EVANDRO FERNANDES DE and NARDI, LAURO VALENTIM STOLL and Sack, Richard O. and Walker, David and Carmichael, Ian S.E. and Reath, Kevin A. and Ramsey, Michael S. and Carlson, Richard W and Frost, D. J. and Langenhorst, F. and {Van Aken}, P. A. and Nekvasil, H. and I, Disciplina G E Mineralogia and Sari, Shinta Permata and Gao, Jian Feng and Zhou, Mei Fu and Robinson, Paul T. and Wang, Changming Christina Yan and Zhao, Jun Hong and Malpas, John and ALMEIDA, Fernando FL{\'{A}}VIO MARQUES De E and F{\'{a}}varo, D{\'{e}}borah In{\^{e}}s Teixeira and {De Oliveira}, Sonia Maria Barros and Damatto, Sandra Regina and Menor, Eldemar and Moraes, Alex Souza and Mazzilli, Barbara Paci and Ferrara, G. and Preite-Martinez, M. and Taylor, H. P. and Tonarini, S. and Turi, B. and {THOMAZ FILHO}, Antonio ANT{\^{O}}NIO and Cesero, PEDRO DE and MIZUSAKI, Ana Maria Pimentel and Le{\~{a}}o, Joana Gisbert and {Da Costa Alves}, Eliane and Maia, M{\'{a}}rcia and Sichel, Susanna Eleonora and {De Campos}, Cristina Maria Pinheiro and Fodor, R. V. and Galar, P. and Island, Kahoolawe and Fodor, R. V. and Dobosi, G. and Sial, Alcides Nobrega and McKee, E. H. and Asmus, H. E. and Foley, Stephen F. and Prelevic, Dejan and Rehfeldt, Tatjana and Jacob, Dorrit E. and Crystallization, Fractional and Melting, Fractional and Guti{\'{e}}rrez-Alonso, Gabriel and Collins, Alan S. and Fern{\'{a}}ndez-Su{\'{a}}rez, Javier and Pastor-Gal{\'{a}}n, Daniel and Gonz{\'{a}}lez-Clavijo, Emilio and Jourdan, Fred and Weil, Arlo B. and Johnston, Stephen T. and Verati, Chrystele and F{\'{e}}raud, Gilbert and Fitton, J. Godfrey and Upton, B. G.J. and Frost, B. Ronald and Frost, Carol D. and Janou{\v{s}}ek, Vojt{\v{e}}ch and Farrow, C. M. and Erban, Vojt{\v{e}}ch and Fran{\c{c}}a, Z. and Ulbrich, HORSTPETER H. G. J. and Demaiffe, D. and VLACH, Silvio R.F. F. and Ulbrich, Mabel N.C. C. and Kay, R W and Seifert, Karl and Brunotte, Dale and RIZZOTTO, GILMAR JOS{\'{E}} and Lima, EVANDRO FERNANDES DE and {CHEMALE JR}, FARID and Bonito, Rio and Geraldes, Mauro Cesar C{\'{e}}sar and Motoki, Akihisa and Costa, Anderson and Mota, Carlos Eduardo Miranda and Mohriak, Webster Ueipass and {شجاعی، رؤیا} and Weaver, Barry L. and Wood, D. A. and Tarney, J. and Joron, J. L. and Leal, Angela Beatriz de Menezes and Paul, Debajyoti and da Silveira, Walter Peixoto and Leal, Luiz Rog{\'{e}}rio Bastos and Cruz, Simone Cerqueira Pereira and Santos, Joilma Prazeres and Lusa, Marcelo and Lusa, Marcelo and Philipp, Ruy Paulo and Valentim, Lauro and Nardi, Stoll and Skolotnev, S. G. and Peive, A. A. and Cushman, Buffy and Sinton, John M. and Ito, Garrett and Dixon, Jacqueline Eaby and Gibson, SALLY A. and THOMPSON, ROBERT N. and Day, J. A. and Humphris, Susan E. and Dickin, A. P. and Leonardos, O. H. and Dickin, A. P. and Mitchell, John G. and {Gibson S.A., Thompson R.N., Weska R.K., Dickin A.P.}, Leonardos O.H. and Gibson, SALLY A. and THOMPSON, ROBERT N. and Weska, R. K. and Dickin, A. P. and Leonardos, O. H. and Drescher, Hermann and Gnev, N H and Green, D. H. and Ringwood, A. E. and Green, Trevor H. and Green, D. H. and Ringwood, A. E. and Grove, Timothy L. and Till, Christy B. and Krawczynski, Michael J. and Haase, Karsten M. and Beier, Christoph and Kemner, Fabian and Davies, Gareth R and Halliday, Alex N and Lee, Der-chuen and Tommasini, Simone and Paslick, Cassi R and Fitton, J. Godfrey and James, Dodie E and Hartmann, Gerald and Wedepohl, K. Hans and Wentworth, Chester K. and Macdonald, Gordon A. and M{\"{a}}kip{\"{a}}{\"{a}}, H. and Heinonen, Jussi S. and Jennings, Eleanor S. and Riley, Teal R. and Herz, Norman and Hirano, Naoto and Kawamura, K. and Hattori, M. and Saito, K. and Ogawa, Y. and Machida, Shiki and Abe, Natsue and Morishita, Tomoaki and Tamura, Akihiro and Arai, Shoji and {De Hoog}, Jan C.M. and Gall, Louise and Cornell, David H. and Humphris, Susan E. and Thompson, Geoffrey and Mota, Carlos Eduardo Miranda and Souza, F A L De and Vargas, Thais Tha{\'{i}}s and Geraldes, Mauro Cesar C{\'{e}}sar and metode penelitian {Nursalam, 2016} and Resende, Fl{\'{a}}vio and {THOMAZ FILHO}, Antonio ANT{\^{O}}NIO and MIZUSAKI, Ana Maria Pimentel and Antonioli, Luzia and Carbonin, C. and {Dal Negro}, A. and Ganeo, S. and Piccirillo, Enzo M. and Kronberg, Bengt and Holmberg, Krister and Lindman, Bj{\"{o}}rn and Ishimaru, Satoko and Arai, Shoji and White, William M. and {Anelise Losangela Bertotti} and Regional, Geologia and Vergara, Mercedes Diaz and Torquato, Joaquim Raul and Widom, Elisabeth and Bindeman, Ilya and Keken, Van and Ablay, G. J. and Carroll, M. R. and Palmer, M. R. and Mart{\'{i}}, J. and Sparks, R. S.J. and Kar, Aditya and Weaver, Barry L. and Davidson, Jon and Colucci, Mike and {Le Roex}, Anton P. and Lanyon, Ruth and Weis, D. and Frey, F. A. and Giret, A. and Cantagrel, J. M. and THOMPSON, ROBERT N. and Ottley, C. J. and Smith, P. M. and Pearson, D. G. and Dickin, A. P. and Morrison, M. A. and Leat, Philip T. and Gibson, SALLY A. and Weis, D. and Frey, F. A. and Giret, A. and Cantagrel, J. M. and Harris, Chris and Marsh, Julian S. and Milner, Simon C. and Peate, David W. and Hawkesworth, Chris J. and Mantovani, Marta S.M. M.S. and Rogers, Nick W. and Turner, Simon P. and Kamber, B. S. and Collerson, K. D. and Nekvasil, H. and Simon, A. and Lindsley, Donald H. and SPATH, A. and HELLEBRAND, Eric and Regelous, Marcel and TRUMBULL, R. B. and Jung, Caroline and Jung, Stefan and Hoffer, Edgar and Berndt, Jasper and Schuth, Stephan and M{\"{u}}nker, Carsten and K{\"{o}}nig, Stephan and Qopoto, Cromwell and Basi, Stanley and Garbe-Sch{\"{o}}nberg, Dieter and Ballhaus, Chris and {Le Roex}, Anton P. and Class, Cornelia and O'Connor, John M. and Jokat, Wilfried and Kawabata, Hiroshi and Hanyu, Takeshi and Chang, Qing and Kimura, Jun Ichi and Nichols, Alexander R.L. and Tatsumi, Yoshiyuki and Jackson, Matthew G. and Jellinek, A. Mark and Hart, Stanley R. and Konter, Jasper G. and Koppers, Anthony A.P. and Staudigel, Hubert and Kurz, Mark D. and Blusztajn, Jerzy S. and Sinton, John M. and Saal, Alberto E. and Shimizu, Nobumichi and Kurz, Mark D. and Blusztajn, Jerzy S. and Skovgaard, Anna C. and Ramo, Geologia and Coimbra, Universidade De and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and Junqueira-Brod, TEREZA CRISTINA and Gaspar, JOS{\'{E}} CARLOS and Brod, JOS{\'{E}} AFFONSO and Jost, Hardy and {Rocha Barbosa}, Elisa Soares and Kafino, Camilla Vasconcelos and Oriental, Oriental E Paraguai and Kaur, Parampreet and Zeh, Armin and Chaudhri, Naveen and Eliyas, Nusrat and Kawabata, Hiroshi and Hanyu, Takeshi and Chang, Qing and Kimura, Jun Ichi and Nichols, Alexander R.L. and Tatsumi, Yoshiyuki and Kelley, Katherine A. and Plank, Terry and Grove, Timothy L. and Stolper, Edward M. and Newman, Sally and Hauri, Erik and Kempton, P.D. and Casey, J.F. and ichiro Aoki, Ken and Kushiro, Ikuo and Kent, Adam J.R. and Norman, Marc D. and Hutcheon, Ian D. and Stolper, Edward M. and Alibert, C and Ketchum, Kirsty Y. and Heaman, Larry M. and Bennett, Gerry and Hughes, David J. and Ganne, Jerome and Feng, Xiaojun and Stanley, J. R. and Flowers, R. M. and Klein, V. C. and Vieira, A. C. and Kostopoulos, Dimitris K. and James, Simon D. and Fowler, Reading and McKibbin, Seann J. and O'Neill, Hugh St C. and Mallmann, Guilherme and Halfpenny, Angela and Langmuir, Charles H. and Hanson, G. N. and Leake, Bernard E. and Woolley, Alan R. and Arps, Charles E.S. and Birch, William D. and Gilbert, M. Charles and Grice, Joel D. and Hawthorne, Frank C. and Kato, Akira and Kisch, Hanan J. and Krivovichev, Vladimir G. and Linthout, Kees and Laird, Jo and Mandarino, Joseph A. and Maresch, Walter V. and Nickel, Ernest H. and Rock, Nicholas M.S. and Schumacher, John C. and Smith, Douglas David C. and Stephenson, Nick C.N. and Ungaretti, Luciano and Whittaker, Eric J.W. and Youzhi, Guo and Bas, M. J.Le and Maitre, R. W.Le and Streckeisen, A. L. and Zanettin, B. and Fractionation, Crystal and Island, Ocean and Thursday, Basalts and Leeman, W P and ALMEIDA, Fernando FL{\'{A}}VIO MARQUES De E and Carneiro, CELSO DAL R{\'{E}} and MIZUSAKI, Ana Maria Pimentel and Liou, Juhn G. and Tsujimori, Tatsuki and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and Brasiliensis, Geochimica and {Prazeres Filho}, Helcio Jose and Harara, Ossama Mohamed and {Stipp Basei}, Miguel Angelo and Passarelli, Claudia Regina and {Siga Jr.}, Oswaldo and Parsons, Marianne and MacQueen, Jeffrey and {Sverre Berstad} and Horstad, Idar and Nacional, Parque and Abrolhos, Marinho De and Marine, Abrolhos and B{\'{a}}rbara, Santa and These, Guarita and Paulo, S{\~{a}}o and Spinelli, Fernando Pelegrini and {De Barros Gomes}, Celso and ALMEIDA, Fernando FL{\'{A}}VIO MARQUES De E and Carneiro, CELSO DAL R{\'{E}} and MIZUSAKI, Ana Maria Pimentel and Azzone, Rog{\'{e}}rio Guitarrari and Ruberti, Excelso and Rojas, Gaston Eduardo Enrich and {De Barros Gomes}, Celso and Mohriak, Webster Ueipass and Janeiro, Rio I O De E and Montes-Lauar, C. R. and Pacca, I. G. and Melfi, A. J. and KAWASHITA, KOJI and Agostinho, Santo and Ya, Vicente and Carmelita, Convento and Castelo, Forte and O'Connor, John M. and Duncan, R. A. and Tomazzoli, Edison Ramos and Pellerin, J{\"{o}}el Robert George Marcel and Ulbrich, HORSTPETER H. G. J. and VLACH, Silvio R.F. F. and Ulbrich, Mabel N.C. C. and KAWASHITA, KOJI and White, William M. and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and {شجاعی، رؤیا} and Merli, Marcello and Bonadiman, Costanza and Diella, Valeria and Pavese, Alessandro and Yuen, David A and Ulbrich, Mabel N.C. C. and Machida, Shiki and Kogiso, Tetsu and Hirano, Naoto and Vel{\'{a}}zquez, Victor Fernandez and Riccomini, CL{\'{A}}UDIO Claudio and Gomes, Celso B. de Barros and de Figueredo, Lucia and Figueredo, Carlos and Workman, Rhea K. and Hart, Stanley R. and Martins, S. and Mendes, Marcos P. H and Mata, Jo{\~{a}}o and Munh{\'{a}}, J and Caldeira, R and Madureira, Pedro and Mata, Jo{\~{a}}o and Mattielli, Nadine and Queiroz, Gabriela and Silva, Pedro and Reich, C. J. and Ferrelli, Federico and Scientific, National and Scientific, National and Piccolo, Maria Cintia and Mota, Carlos Eduardo Miranda and Geraldes, Mauro Cesar C{\'{e}}sar and de Almeida, Julio Cesar Horta C{\'{e}}sar Horta Cesar Horta and Vargas, Thais Tha{\'{i}}s and {De Souza}, D{\'{e}}bora Marinho and {De Oliveira Loureiro}, Renata and {Da Silva}, Aline Pimentel and do NASCIMENTO, Marcos Antonio Leite and Vi, Cap{\'{i}}tulo and do NASCIMENTO, Marcos Antonio Leite and Pl, Tridimensional D O and Japi, T O N D E and M., Babinski and McCarter, Renee' L. and Fodor, R. V. and Trusdell, Frank and Melluso, Leone and Guarino, Vincenza and Lustrino, Michele and Morra, Vincenzo and de' Gennaro, Roberto and Linnen, Robert L. and Keppler, Hans and Kinzler, Rosamond J. and Ghiorso, Mark S and Gualda, Guilherme A R and Regelous, Marcel and Niu, Yaoling and Abouchami, Wafa and Castillo, Pat R. and H{\'{e}}mond, Christophe and Hofmann, Albrecht W. and Vlast{\'{e}}lic, Ivan and Nauret, Fran{\c{c}}ois and Motoki, Akihisa and Paul, Debajyoti and White, William M. and Turcotte, Donald L. and Motoki, Akihisa and Ara{\'{u}}jo, Ana L{\'{u}}cia and Sichel, Susanna Eleonora and Geraldes, Mauro Cesar C{\'{e}}sar and Jourdan, Fred and Motoki, Kenji Freire and Silva, Samuel and Campos, Thomas Ferreira da Costa and Srivastava, Narendra Kumar and Soares, Rodrigo and Stasiuk, M. V. and Barclay, J. and Carroll, M. R. and Jaupart, C. and Ratt{\'{e}}, J. C. and Sparks, R. S.J. and Tait, S. R. and M{\"{u}}ller, R. Dietmar and Roest, Walter R. and Royer, Jean-Yves Y. and Gahagan, Lisa M. and Sclater, John G. and Sdrolias, Maria and Gaina, Carmen and Roest, Walter R. and Leat, Philip T. and Day, Simon J. and Tate, Alex J. and Martin, Tara J. and Owen, Matthew J. and Tappin, David R. and M{\"{u}}ller, R. Dietmar and Sdrolias, Maria and Gaina, Carmen and Roest, Walter R. and Muller, R. D. and Royer, Jean-Yves Y. and Lawver, L. A. and Hofmann, Albrecht W. and WASYLENKI, L. E. and Neumann, E R and Nielsen, Roger L. and Nishimura, Koshi and Niu, Yaoling and O'Hara, Michael J. and {Yaoling Niu} and Batiza, R. and Nude, Prosper M. and Shervais, John W. and Attoh, Kodjopa and Vetter, Scott K. and Barton, Corey and O'Connor, John M. and Jokat, Wilfried and Wijbrans, Jan and Colli, Lorenzo and Sclater, John G. and White, William M. and Rural, Universidade Federal and Enxame, Pesquisas and Rural, Universidade Federal and Valente, Castro and Markl, Gregor and Marks, Michael A.W. and {Ronald Frost}, B. and Gasperini, Daniela and Hern{\'{a}}ndez, Agust{\'{i}}n and Cruz, D E L A and Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias and Variations, Obliquity and Kadik, A. A. and Campos, ROBERTO SACKS DE and Pandey, Ashutosh and {Chalapathi Rao}, N. V. and Pandit, Dinesh and Pankaj, Praveer and Pandey, Rohit and Sahoo, Samarendra and Kumar, Alok and Pang, Kwan Nang and Chung, Sun Lin and Zarrinkoub, Mohammad Hossein and Khatib, Mohammad Mahdi and Mohammadi, Seyyed Saeid and Chiu, Han Yi and Chu, Chiu Hong and Lee, Hao Yang and Lo, Ching Hua and Anderson, Don L. and Sammis, Charles and Pearce, Julian A. and Harris, Nigel B.W. and Tindle, Andrew G. and Pesaran, M. Hashem and Putirka, Keith Daniel and Durand-Charre, Madeleine and Putirka, Keith Daniel and Johnson, Marie C and Kinzler, Rosamond J. and Walker, David and Andersen, David J. and Lindsley, Donald H. and Davidson, Paula M. and Magnani, Marco and Fujii, Toshitsugu and Orihashi, Yuji and Yasuda, Atsushi and Hirata, Takafumi and Santo, Alba P. and Vaggelli, Gloria and Yang, Zong Feng and Zhou, Jun Hong and Galton, Francis and Figure, From and Ray, Jytisankar and Sen, Gautam and Kunzmann, Thomas and THOMPSON, ROBERT N. and Ottley, C. J. and Smith, P. M. and Pearson, D. G. and Dickin, A. P. and Morrison, M. A. and Leat, Philip T. and Gibson, SALLY A. and Pires, Gomes L.C. and Bongiolo, Everton M. and Geraldes, Mauro Cesar C{\'{e}}sar and Renac, C. and Santos, Adjacente C. {\`{A}} Bacia D E and Jourdan, Fred and Neumann, R. and {Lustrino, M; Dallai, L; Giordano, R; Gomes}, C.B.; and Poli, Stefano and Schmidt, Max W. and Pf{\"{a}}nder, J A and M{\"{u}}nker, Carsten and Jung, Stefan and Mezger, K and Gibson, SALLY A. and THOMPSON, ROBERT N. and Weska, R. K. and Dickin, A. P. and Leonardos, O. H. and Lehky, Sidney R. and Tanaka, Keiji and Atentamente, Leia and Instru{\c{c}}{\~{o}}es, A S and Tese, Souza Bologna and Padilha, Antonio Lopes and Putirka, Keith Daniel and Quirk, David G. and Hertle, Michael and Jeppesen, Jon W. and Raven, Madeleine and Mohriak, Webster Ueipass and Kann, Dorthe J. and N{\o}rgaard, Mette and Howe, Matthew J. and Hsu, Dan and Coffey, Brian and Mendes, Marcos P. H and Rampone, Elisabetta and Borghini, Giulio and Godard, Marguerite and Ildefonse, Benoit and Crispini, Laura and Fumagalli, Patrizia and Rasskazov, Sergei and Chuvashova, Irina and Turner, Simon P. and Caulfield, John and Turner, Michael and {Van Keken}, Peter and Maury, Ren{\'{e}} and Sandiford, Mike and Prouteau, Gaelle and Alves, Leandro Soares Gouveia Martins; Ruy Jos{\'{e}} Valka and White, William M. and Cheatham, M. M. and Duncan, R. A. and {شجاعی، رؤیا} and Ocean, South Atlantic and Ericsson, K. Anders and Rivalenti, Giorgio and Mazzucchelli, Maurizio and Girardi, Vicente A.V. and Vannucci, Riccardo and Barbieri, M. Adelaide and Zanetti, Alberto and Goldstein, Steve L. and Miranda, Rui and Terrinha, Pedro and Mata, Jo{\~{a}}o and Azevedo, Ros{\'{a}}rio and Chadwick, Jane and Louren{\c{c}}o, Nuno and Moreira, M{\'{a}}rio and Rocha, Marcelo Peres and Schimmel, Martin and Assump{\c{c}}{\~{a}}o, Marcelo and Liz, Joaquim Daniel De and Lima, EVANDRO FERNANDES DE and Valentim, Lauro and Nardi, Stoll and {Le Bas}, M. J. and Streckeisen, A. L. and Harangi, Szabolcs and Downes, Hilary and Thirlwall, Matthew and Gm{\'{e}}ling, Katalin and Rov, P L and Rojas, Gaston Eduardo Enrich and Ruberti, Excelso and Azzone, Rog{\'{e}}rio Guitarrari and {De Barros Gomes}, Celso and Rona, Peter a and Richardson, Evan S and Sanfilippo, Alessio and Tribuzio, Riccardo and Tiepolo, Massimo and Sato, Hiroaki and Saunders, A. D. and Norry, M. J. and Tarney, J. and Siebel, W. and Becchio, R. and Volker, F. and Hansen, M. A.F. and Viramonte, J. and TRUMBULL, R. B. and Haase, G. and Zimmer, M. and Rodgers, Mel and Roman, Diana C. and Geirsson, Halldor and LaFemina, Peter and Mu{\~{n}}oz, Angelica and Guzman, Carlos and Tenorio, Virginia and Regelous, Marcel and Niu, Yaoling and Abouchami, Wafa and Castillo, Pat R. and Shorttle, Oliver and Moussallam, Yves and Hartley, Margaret E. and Maclennan, John and Edmonds, Marie and Murton, Bramley J. and ALMEIDA, Fernando FL{\'{A}}VIO MARQUES De E and Siivola, J and Schmid, R and Dasgupta, Rajdeep and Hirschmann, Marc M. and Stalker, Kathryn and Paulo, Universidade D E S {\~{A}} O A O and Entologia, Sedim and Jos{\'{e}}, Augusto and Pedreira, De C L and C, Augusto Jos{\'{e}} De and Pedreira, L and Oor-rnc, Nrcrror- W A and Bonifacio, Juliana Fernandes and Skolotnev, S. G. and Peyve, A. A. and Turko, N. N. and Bylinskaya, M. E. and Golovina, L. A. and Ipat'eva, I. S. and Lindzus, Dipl Jennifer and Osnabr{\"{u}}ck, Universit{\"{a}}t and Tatistik, {\"{U}} Bung S and Datenanalyse, U N D and Sleep, Norman H and Sobolev, N. V. and Logvinova, A. M. and Zedgenizov, D. A. and Pokhilenko, N. P. and Malygina, E. V. and Kuzmin, D. V. and Sobolev, A. V. and Solomatov, V and Sonoki, I. K and Garda, Gianna Maria and and Meckling, Jensen and Anderson, Don L. and Jung, Stefan and Stracke, Andreas and Hofmann, Albrecht W. and Hart, Stanley R. and Wolff, John A and Tackley, Paul J. and Dias, Armando and J{\'{u}}nior, Tavares and Geraldes, Mauro Cesar C{\'{e}}sar and Costa, Anderson and Holanda, Werlem and Herzberg, C. and Asimow, P. D. and Arndt, N. and Niu, Yaoling and Lesher, C. M. and Fitton, J. Godfrey and Cheadle, M. J. and Saunders, A. D. and Fuhrman, Miriam L. and Lindsley, Donald H. and Hunt, Heather K and Silveira, F V and Almeida, Ricardo Nascimento and Geologia, Curso D E and Gale, Allison and Langmuir, Charles H. and Dalton, Colleen A. and M{\"{o}}ller, H and {THOMAZ FILHO}, Antonio ANT{\^{O}}NIO and RODRIGUES, Aliotti ANA L{\'{U}}CIA and Clemente, Eliane de Paula Eliene de Paula and Schaefer, Carlos Ernesto G.R. and Oliveira, F{\'{a}}bio Soares and {Albuquerque Filho}, Manoel Ricardo and Alves, Ruy V{\'{a}}lka and S{\'{a}}, Mariana M{\'{e}}dice Firme and Melo, Vander de Freitas and Corr{\^{e}}a, Guilherme Resende and Adam, John and Green, Trevor H. and Marks, Michael A.W. and Halama, Ralf and Wenzel, Thomas and Markl, Gregor and {شجاعی، رؤیا} and Mattos, Wanessa Melchert and Rollinson, Hugh R. and Laurent, Antonin and Janou{\v{s}}ek, Vojt{\v{e}}ch and Magna, Tom{\'{a}}{\v{s}} and Schulmann, Karel and M{\'{i}}kov{\'{a}}, Jitka and Cagnoli, B. and Romano, G. P. and Haase, Karsten M. and Devey, Colin W. and Vilalva, Frederico Castro Jobim and VLACH, Silvio R.F. F. and Vogel, Thomas A. and Hidalgo, Paulo J. and Patino, Lina and Tefend, Karen S. and Ehrlich, Robert and Skolotnev, S. G. and Peyve, A. A. and Turko, N. N. and MEIRELLES, MARCELO R. and DARDENNE, MARCEL A. and Walters, A. L. and Phillips, J. C. and Brown, R. J. and Field, M. and Gernon, T. and Stripp, G. and Sparks, R. S.J. and Humphris, Susan E. and Thompson, Geoffrey and Wang, Changming Christina Yan and Chen, Liang and Bagas, Leon and Lu, Yongjun and He, Xinyu and Lai, Xiangru and Wass, Suzanne Y. and HEKINIAN, ROGER and Weaver, Barry L. and Kar, Aditya and Davidsont, J O N and Colucci, Mike and Welsch, Benoit and Hammer, Julia and Baronnet, Alain and Jacob, Samantha and HELLEBRAND, Eric and Sinton, John M. and White, William M. and Whitney, Donna L. and Evans, Bernard W. and Woolley, Alan R. and {Garth Platt}, R. and Wang, Zhi Hui and Ge, Wen Chun and Yang, Hao and Bi, Jun Hui and Ji, Zheng and Dong, Yu and Xu, Wen Liang and Publications, Peter J Wyllie and Yang, Gaoxue and Li, Yongjun and Safonova, Inna and Yi, Shanxin and Tong, Lili and Seltmann, Reimar and Zhang, Chuan Lin and Zou, Hai Bo and Wang, Hong Yan and Li, Huai Kun and Ye, Hai Min and Zhu, Yongfeng and Ogasawara, Yoshihide and Dmitry, Zozulya and Nelson, E B Y and David, K. and Schiano, Pierre and All{\`{e}}gre, C. J. and Laurentino, Lauro De Sena and Quirk, David G. and Hertle, Michael and Jeppesen, Jon W. and Raven, Madeleine and Mohriak, Webster Ueipass and Kann, Dorthe J. and N{\o}rgaard, Mette and Howe, Matthew J. and Hsu, Dan and Coffey, Brian and Mendes, Marcos P. H and de Melo, Aline Cristina and Santos, Rodrigo Bijani Rosana N. and Carlos, Dion{\'{i}}sio Uendro and Neto, Cosme F. Ponte and Barbosa, Val{\'{e}}ria C. F. and Lins, Carlos Alberto C and Jacques, Ana Paula R and Riccomini, CL{\'{A}}UDIO Claudio and Gomes, Leonardo Correa Lucy and Anna, Sant and Rigoti, Caesar Augusto and {Bento dos Santos}, Telmo M. and Tassinari, Colombo G. C.G. Celso Gaeta C.G. and Fonseca, Paulo E. and Siedner, Gerard and Mitchell, John G. and Salomon, Eric and Passchier, Cees and Koehn, Daniel and Tupinamb{\'{a}}, Miguel and Heilbron, MONICA and Duarte, Beatriz Paschoal B.P. and Nogueira, Jos{\'{e}} Renato and Valladares, CL{\'{A}}UDIA SAY{\~{A}}O Claudia and Almeida, Julio C.H. J{\'{u}}lio Julio and Silva, Luiz Guilherme do Eirado and de Medeiros, Silvia Regina and de Almeida, Clayton Guia and Miranda, Alan and Ragatky, C{\'{e}}lia Diana and Mendes, Julio Cezar J{\'{u}}lio and Ludka, Isabel and Teixeira, Wilson and Heilbron, MONICA and Valeriano, Claudio de Morisson CL{\'{A}}UDIO DE MORISSON Claudio De Morisson and Tupinamb{\'{a}}, Miguel and Simonetti, Antonio and Heilbron, MONICA and de Almeida, Julio Cesar Horta C{\'{e}}sar Horta Cesar Horta and do Eirado, Luiz Guilherme and Zal{\'{a}}n, Pedro Victor and de Oliveira, Jo{\~{a}}o Alberto Bach and Valeriano, Claudio de Morisson CL{\'{A}}UDIO DE MORISSON Claudio De Morisson and Mendes, Julio Cezar J{\'{u}}lio and Tupinamb{\'{a}}, Miguel and Bongiolo, Everton M. and Heilbron, MONICA and Junho, Maria do Carmo Bustamante and Meek, Christopher and Hfiana, Sara Ali and {Mu{\~{n}}oz Nu{\~{n}}ez}, Daniel Gerardo and Ji, Guanzhou and Mohler, Rick and Omar, Osama Mohamed El-said and Wael, Arch and Adel, Mohamed and Civil, Faculdade D E Engenharia and Urbanismo, Arquitetura E and Das, Avalia{\c{c}}{\~{a}}o and Em, Janelas and Escolares, Edif{\'{i}}cios and Elaine, Fl{\'{a}}via and RODRIGUES, Aliotti ANA L{\'{U}}CIA and Das, Avalia{\c{c}}{\~{a}}o and Em, Janelas and Escolares, Edif{\'{i}}cios and Rahimzadeh, Shahab Din and Peterson, Nicole L and White, Jonathan Robert and {Tapia Zeas}, Cristian Eduardo and {Ministerio de Electricidad y Energ{\'{i}}a Renovable} and Meneses, Edgar and {Rojas Cortorreal}, Gilkauris Mar{\'{i}}a and Karpicka, Edyta and Brembilla, Eleonora and {Aguilar S{\'{a}}nchez}, Alexis and Confort, L U Z Y and {Anand Athalye}, Rahul and Boyce, Peter and Hunter, Claudia and Howlett, Owen and Eriksson, Sara and Waldenstr{\"{o}}m, Lovisa}, -eprint = {arXiv:1011.1669v3}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9788578110796}, -issn = {1098-6596}, -journal = {Acta Universitatis Agriculturae et Silviculturae Mendelianae Brunensis}, -keywords = {(),(UMI)AAI10293775,- basalt,-picrite,0514:School administration,0729:Architecture,1,10,10.1002/2014JB011561 and Santos Basin,1007,12691,132ma,1999,2,2 apresentam raz{\~{o}}es la,2004 para prospec-,2006,2013,238U and 232Th series,238U-230Th-226Ra systematics,3-18,3He/4He,4044 derring hall,40Ar/39Ar,40Ar/39Ar age dating,40Ar/39Ar ages,40Ar/39Ar dating,40Ar/39Ar geochronology,41-46,70 km,87Sr/86Sr isotopes,9998:No ProQuest subject assigned,A-type granites,AAPG Bulletin,ABSTRACT,AFC,AFC processes,AIFC,ANALYTICAL TECHNIQUES,Abrolhos continental shelf,Absolute age,Accommodation zone,Accretionary wedge,Activity Based Costing,Adakite,Adjoint method,Aegirine,Aeromagnetic data,Aeromagnetics,Aeromagnetism,Africa,African plate motion,Agitation gradient,Agpaitic rocks,Alcalina,Alkali basalt,Alkali basalts,Alkali-basalt,Alkalic,Alkaline and tholeiitic magmatism,Alkaline core,Alkaline intrusions,Alkaline magmatism,Alkaline rocks,Alkaline volcanic,Alkaline-carbonatite complex,Aluminous A-type granite,Amambay regions,Amazonian Craton,Ambient mantle temperatures,America,American Society for Photogrammetry,Amphibole,Amphibolite partial melting,Amp{\`{e}}re Seamount,Analyse chimique,Andesite,Anisotropy of magnetic susceptibility,Ankaramite,Annual Daylight Metrics,Anorogenic granite,Antarctica,An{\'{a}}lise estrutural. Deforma{\c{c}}{\~{a}}o r{\'{u}}ptil. Lineamentos,An{\'{a}}lisis qu{\'{i}}mico,Apatite fission track,Approaching,Ar-40/Ar-39,Ar-Ar dating,Ar-Ar geochronology,Ar/Ar,Arc magmatism,Arc-type volcanic rocks,Architecture,Argentina,Arizona rhyolite compositions,Arraial do Cabo peninsula,Ascencion fracture zone,Ascension Island,Asia,Assimilation,Asthenosphere,Asthenosphere flow,Atlantic,Atlantic continental margin,Atlantic margin,Atlantic ocean opening,Augite,Azores,Bacia de (SP),Bacia de Campos,Bacia do Parna{\'{i}}ba,Baddeleyite U-Pb dating,Balanced restoration,Basalt,Basaltic dikes,Basalts,Basanite,Base erosion,Basement,Basement control,Basement inheritance,Basin analysis,Basin development,Bezymianny Volcano,Bibliographies,Binary mixing,Biology,Body waves,Bohemian Massif,Borborea province,Botswana,Boudinage,Brasiliano orogeny,Brasiliano-Panafrican,Brazil,Brazil magmatism,Brazilian margin,Brazilian rifted margin,Breakup unconformity,Brittle structures,Building Performance Simulation,C,CENTROS INFANTILES,CESifo Working Paper no. 7303,Calc-alkaline magmatism,Calcite,Caldera,Cambrian,Campos Basin,Campos and Santos basins,Campos basin,Canan{\'{e}}ia,Carbonate-rich rocks,Carbonated eclogite,Carbonated peridotite,Carbonatite,Carbonatites,Carpathian-Pannonian region,Cataclasis,Cenozoic,Cenozoic rifts,Cenozoic tectonics,Central Atlantic magmatic province,Chain silicates,Chemical composition,Chemical ratios,Chemistry,Chemostratigraphy,Chile trench,Chondrites,Chronology,Classification,Classrooms,Climate-Based Daylight Modelling,Clinopyroxene,Colorado Plateau,Columbia,Columbia seamount,Communication and the arts,Compatibility,Complex,Composition diagrams,Conjugate Atlantic margin,Conjugate margins,Continental Geology,Continental breakup,Continental collision,Continental crust,Continental flood basalt,Continental flood basalts,Continental volcanism,Core-mantle boundary,Corporate income tax,Corvo,Cost management,Cpx,Craton,Cretaceous Serra do Mar,Cretaceous hingeline,Crust,Crustal anatexis,Crustal architecture,Crustal assimilation,Crustal boundary,Crustal composition,Crustal contamination,Crustal modeling,Crustal recycling,Crustal stretching,Crustal structure,Crustal thickness,Crustal thinning,Crystal fractionation,Crystal isotope stratigraphy,Crystallization,Cumulate,Cumulate texture,Cunhaporanga Batholith,DES,DISE{\~{N}}O DE ILUMINACION,DIVA,DMM,Dacite,Damage zone,Damage zones,Data analysis,Daylight,Daylight factor,Daylighting,Debris flows,Deep seismic,Deep seismic data,Deep seismic reflection and refraction,Deep water,Deformation bands,Degree of melting,Dendrite,Density,Depleted upper mantle,Depositionol element,Desertas Islands,Dharwar,Diagrama equilibrio,Diagramme {\'{e}}quilibre,Diamond,Didactic,Different target prices,Digital isochrons,Dike Swarm,Dike swarm,Dike swarms,Dilatational fractures,Diorite,Dual model,Dupal Anomaly,Dupal mantle anomaly,Dyke swarm,Dyke swarms,Dykes,Dynamics of lithosphere and mantle,D″,EM-1,Early Jurassic,Earth history,Eastern Pontides,Eclogite,Ecotipos,Education,Educational institutions,Efeito Banco,Eifel,Elbe Fault System,Element partitioning,Endemic soils,Enriched mantle source,Enrichment,Enxame de Diques de Florian{\'{o}}polis,Eocene,Eocene-Oligocene,Eopaleozoic,Equatorial Atlantic,Equilibrium,Eritrea,Eruption transitions,Eruptions,Esp{\'{i}}rito Santo basin,Etendeka,Experimental petrology,Experimental phase equilibria,FOZO,Factor analysis,Faroes,Fault growth,Fault interaction,Fault reactivation,Fault stepovers,Fault surfaces,Fault tip,Faults,Faults and fractures,Fe-Ti oxides,Feldspars,Felsic magmatism,Fernando Poo fracture zone,Fernando de Noronha,Financial performance,Flood basalt,Flood basalts,Florian{\'{o}}polis Dyke Swarm,Fluid flow,Fluid inclusion,Foliation,Foreign direct investment,Forma{\c{c}}{\~{a}}o Serra Geral,Fractional crystallization,Fractionation,Fractionation crystallization,Fracture,Fracture networks,Fracture zone,Fracture-frequency,Fractures,Free-air gravity,Full waveform inversion,Gabbro,Gabbroic xenoliths,Gabbronorite,Galapagos plume,Garnet peridotite,Geobarometry,Geochemical modeling,Geochemical modelling,Geochemistry,Geochemistry of boreholes,Geochronology,Geodynamic,Geodynamics,Geofisica,Geologia estrutural,Geology,Geometry,Geophysical,Geophysical anomaly,Geophysics,Geoprocessing,Geoqu{\'{i}}mica,Geotectonics,Geothermal,Geothermal gradient,Geothermobarometry,Geothermometry,Germany,Glass inclusions,Gondwana,Gondwana amalgamation,Gondwana breakup,Graciosa Province,Granite,Granitoid-related mineralisation,Granitoids,Graphs,Grasshopper,Gravitational collapse of orogenic crust,Gravity inversion.,Gravity settling,Green-core clinopyroxene,Groupe pyrox{\`{e}}ne,Grupo piroxeno,HIMU,HIMU OIB,Hafnium,Hawaii,Hawaii petrology,Hb3gr hornblende,Heterogeneity,Hidroac{\'{u}}stica,High field strength elements,High pressure,High resolution aerotnagnetnometry,Hole model,HoneyBee,Hot spot,Hot spots,Hotspot track,Hotspots,Hydraulically significant fracture,Hydrology,Hydrothermal alteration,Hydrothermalism,Hydrous,Hyper-extension,Hyperspectral,ILUMINACION NATURAL,INTRODUCTION,IRAN,IRON SKARN DEPOSIT,Iberia,Igneous intrusions,Igneous rocks,Ilha de Santa Catrina,Illumination,Ilmenite,Imperfect fractional crystallization,In situ crystallization,In-situ sr isotopes,Inclusion,India,Industry,Inequality,Interaction,Interaction between Rodinian plume and plate subdu,Intercalibration,Interpretation of magnetic surveys,Intersection,Intra-plate,Intra-plate basalts,Intracontinental deformation,Intraplate deformation,Intraplate seismicity,Inverse theory,Investment,Iran,Irtysh-Zaisan and Junggar-Balkhash Oceans,Isostatic compensation,Isotope,Isotope geochemistry,Isotopic chemistry,Israel,Itabora{\'{i}} basin,Jacupiranga - Brazil,Jacu{\'{i}}pe Basin,Japi Surface,Joints,Juan Fernandez hotspot,July 1964,Jurassic-Cretaceous transition,Karoo,Katungite,Kilauea Iki,Kimberlite,Kinematic analysis,Kinematic indicators,Kinematic reconstruction and constraints,Kinematics,Kink band,Kokchetav,LA-ICP-MS,LA-MC-ICP-MS,LLSVP,LadyBug,Lages Dome,Lagoa da Vira{\c{c}}āo,Lamprophyre,Landsat TM,Laptev Sea,Large igneous province,Large igneous provinces,Laser ablation,Late Aptian-Early Albian transtension,Late Cretaceous highlands,Late Palaeoproterozoic,Late-Variscan fault,Laterite,Lava lake,Lava stratigraphy,Left-lateral shear zone,Light,Light distribution,Lighting systems,Lineament,Lineamentos,Linear concentration relationship,Linkage,Liquid immiscibility,Lithosphere,Lithosphere plate,Lithosphere thinning,Lithospheric extension,Lithospheric mantle,Lithospheric strength,Lithospheric subcontinental mantle,Lithospheric subcontinental mantle en,Loihi seamount,Low-frequency seismicity,Lower continental crust,Lower crust,Lu-Hf,Lut,Luz natural,MORB,MS Windows,Madeira,Mafic dyke swarms,Mafic-felsic magma interaction,Mafic-ultramafic cumulates,Mafurite,Magma chamber,Magma evolution,Magma genesis,Magma mixing,Magma types,Magma-poor margin,Magmas,Magmatic Arc,Magmatic petrology,Magnesian olivine,Magnesiow{\"{u}}stite,Magnetic anomalies,Magnetic petrology,Magnetic petrophysics,Magnetic sector ICP-MS,Major element,Major elements,Makran,Manjo,Mantle,Mantle convection,Mantle fO2,Mantle geochemistry,Mantle heterogeneity,Mantle isochron,Mantle melting,Mantle metasomatism,Mantle metasomatism en,Mantle plume,Mantle plumes,Mantle processes,Mantle sources,Marquesas,Martin Vaz island,Mauna Kea,Mauna Kea volcano,Mauna Loa,Mechanics,Melt,Melt inclusions,Melt metasomatism,Melt/ solid reaction,Melt/rock reaction,Melting,Melting model,Mesozoic,Messum complex,Metasomatised lithosphere,Metasomatism,Metasomatized mantle source,Microanalysis,Mid ocean ridge basalt,Mid-Atlantic Ridge,Mid-Polish Basin,Mid-atlantic ridge,Mid-ocean ridge,Mid-ocean ridge basalts,Mid-ocean ridges,Mineral abbreviations,Mineral chemistry,Mineral compositions,Mineral-melt trace element partitioning,Mineralization,Mineralogy,Miocene volcanism,Misra2015,Mixing,Mode of emplacement,Model,Modelo Tese UERJ,Morphostructural,Morro Redondo Complex,Morro Vermelho Formation age,Morro de s{\~{a}}o jo{\~{a}}o,Muddy system,Multiplets,Mylonite,M{\o}re Margin,NE Paraguay,NW Iran,Namibia,Nazca Plate,Nb/Ta decoupling,Nb/Ta decoupling en,Nd and Pb isotopes,Nd-144/Nd-143,Neoproterozoic,Neoproterozoic bimodal intrusive complex,Neotectonics,Nepheline syenite,Nephelinite,Nephelinite suite,Nephelinite–phonolite magmatism,Networks,New Zealand,Ni enrichment,Niobium ore deposits,No ProQuest subject assigned,Nomenclatura,Nomenclature,Non-volcanic passive continental margin,Norms,North China Craton,North German Basin,Northeastern China,Northern Aravalli orogen,OIB,OIB genesis,Ocean Drilling,Ocean Island Basalts,Ocean crust,Ocean drilling,Ocean floor,Ocean island basalt,Ocean island basalts,Ocean island magmatism,Ocean islands,Ocean-continent transition,Ocean-island basalts,Oceanic basalts,Oceanic fracture zone,Oceanic islands volcanism,Oceanic lithosphere,Offshore Santos Basin,Okavango,Olivine,Olivine trace element chemistry,Onshore-offshore correlation,Ophiolites,Ore-forming fluids,Orocline,Orogenic collapse,Orthopyroxene,Oscillatory zoning,Oxybarometry,Oxygen,Oxygen fugacity,PHEM,Palaeogeomorphology,Paleo-Pacific Ocean,Paleobreccias,Paleocene,Paleocontinent rifting and breakup,Paleozoic,Pan-African Dahomeyide orogen,Parallel dyke swarm,Parameterization,Parana,Parana Basin,Parana Brazil,Parana flood basalts,Parana-Etendeka volcanism,Paran{\'{a}} Basin,Paran{\'{a}} Continental Flood Basalts,Paran{\'{a}} Magmatic Province,Paran{\'{a}}-Etendeka,Paran{\'{a}}-Etendeka Large Igneous Province,Paran{\'{a}}-Etendeka magmatic province,Parental magma,Partial Melting,Partial mantle melting,Partial melting,Partition coefficients,Passive continental margin,Passive margin,Passive margins,Patagonia,Patagonia en,Patag{\^{o}}nia (Argentina e Chile),Pb isotope,Pb isotopes,Pb paradox,Pb-207/Pb-204,Pb-208/Pb-204,Pb-Sr-Hf isotopes,Peralkaline melts,Peridotite,Permeable,Perovskite,Petit-spot,Petrogenesis,Petrogenetic modelling,Petrography,Petrologic modeling,Petrology,Phase equilibria,Phonolite,Photogrammetric Engineering,Phreatic eruption,Picrite,Picrites,Pigeonite,Piroxeno,Plagioclase,Plagioclase phenocrysts,Plagioclase zoning patterns,Plate kinematic,Plate motions,Plate tectonics,Plate-wide stress,Platinum group elements,Plug model,Plume-ridge interaction,Plumes,Portugal,Post-collisional,Post-collisional extension,Post-orogenic magmatism,Post-perovskite,Potassic and sodic series,Precambrian,Pressure,Pressure-driven asthenospheric flow,Profit shifting,Programa REVIZEE,Proterozoic,Proterozoic granite,Prov{\'{i}}ncia magm{\'{a}}tica Paran{\'{a}},Pr{\'{e}}-sal,Pseudo color,Psychology--Abstracting,Pyrochlore,Pyroclastic flows,Pyroxene,Pyroxenite,Pyrox{\`{e}}ne,QUIIF,Quartz,Quaternary,Quaternary dating,Quiet zone,R language,REE ratios,Radiance,Radiating dyke swarm,Radiogenic isotopes,Raohe accretionary complex,Rare earth element modeling,Reactivation,Reactivation of structures,Real-estate,Recycled oceanic crust,Recycling,Relay ramps,Relay structures,Remote sensing,Representaci{\'{o}}n arquitect{\'{o}}nica,Rhinoceros,Rhyolite,Rhyolite mineral compositions,Ribeira Belt,Ribeira belt,Riedel structures,Rift,Rift stage,Rifting,Rifting deformation,Rifting evolution,Ringwoodite,Rio Apa,Rio Doce formation,Rio bonito,Rock avalanches,Rock magnetism,Rodinia,Russia,SANGAN,SANTOS Basin,SCHEM,SE Brazil,SEBASS,STABLE ISOTOPES,Saint Peter Saint Paul Islets,Salite,Salt basin,Salt tectonics,Salton Sea,Samoa,Sandy system,Santa Catarina Shield,Santas Basin,Santos,Santos Basin,Sao Paulo Plateau,Satellite-derived gravimetry,School administration,Seafloor spreading,Seamount,Seawater,Section restoration,Sector zoning,Sedimentary basin,Segmentation,Segregation veins,Seismic,Seismic stratigraphy,Seismic tomography,Sensoriamento remoto,Sergipe-Aalagoas Basin,Serra Geral,Serra do Mar Province,Serra do Mar alkaline province,Shear,Shear fractures,Shear zone,Shear zones,Shear-zone,Shona,Shona plume,Silica activity,Simulaci{\'{o}}n virtual.,Sistan,Slab,Slab break up,Slab window,Slickensides,Small-scale mantle heterogeneity,Social sciences,Society,Sodic and potassic,Software,Solomon Islands,Solution model,South,South Africa,South America,South American continent,South Atlantic,South Atlantic Ocean,South Atlantic opening,South China Sea,South Gondwana breakup,South and Equatorial Atlantic Oceans,Southeast Brazil,Southeast atlantic ocean,Southeastern Brazil,Southeastern Brazilian margin,Southeastern Ghana,Southern Brazilian occurrences,Southern Brazilian rifted margin,Southwestern Angola,Spinel,Spreading ridge,Spreadsheet program,Sr,Sr isotopes,Sr-87/Sr-86,Sr-Nd isotopes,Sr-Nd-Os isotopes,Sr-Nd-Pb isotopes,Sr-Nd-Pb-Os isotopes,Sr–Nd–Hf isotopes,St. Helena,Standards,Statistic,Strain,Strain localization,Stress,Stress variability,Strike-slip faults,Strike-slip reactivation,Strontium,Structural analysis,Structural geology,Structural inheritance,Structural lineaments,Sub-continental lithospheric mantle,Sub-continental mantle,Subaqueous eruption,Subcontinental lithospheric mantle (SCLM),Subduction,Subduction zone,Submarine volcanism,Subsalt imaging,Subsidence,Subsidence modeling,Sudetic Granite Belt,Suites,Sulfide melt,Summit level map,Supercontinent breakup,Supercontinent cycle,Supercontinents,Supergene ores,Superimposed slickenlines,Supplementary tables,S{\~{a}}o Paulo Plateau,Taishanmiao,Tangu{\'{a}},Target costing,Tarim in NW China,Taubat{\'{e}} Basin,Tax avoidance,Tax havens,Tectonic breccias,Tectonic evolution northeastern Brazil,Tectonic reactivations,Tectonic setting,Tectonic uplift,Tectonics,Tectono-stratigraphic evolution,Tect{\^{o}}nica,Telica,Temperature,Tengchong,Tephrite,Terceira Island,Tese de doutorado,The Czech Republic,Thermal boundary layer,Thermal infrared,Thermal subsidence,Thermometry,Thessalon volcanic rocks,Thinning processes,Tholeiites,Tholeiitic dyke swarm,Tholeiitic magmatism,Tholeitiic,Ti-magnetite,Tibetan plateau,Tonalite,Tonga Trench,Topography,Topology,Trace element enrichment,Trace element mapping,Trace element modeling,Trace element variation,Trace elements,Trace-element partitioning,Trachybasalt,Transfer zone,Transform margin,Transition metals,Transition zone,Transitional domain,Transport model,Travertine,Tres Corregos,Trindade Island,Trindade hotspot,Trindade island,Trindade plume,Triple junction,Tristan,Tristan plume,Troctolites,Tuffisite,Turkey,U'Pb ages,U-Pb,U-Pb dating,U-Pb geochronology,U-value,U/Pb,UAV geological mapping,Ugandite,Ultra-low velocity zone,Ultramafic mantle xenoliths,Ultramafic mantle xenoliths en,Ultramafic xenoliths,Ultrapotassic lavas,Upper mantle convective planform,Upper plate magma-poor rifted margins,Upper-mantle tomography,Uruguay,Value engineering,Vent,Vertical segregation,Vesicularity,Viscosity,Vit{\'{o}}ria-trindade chain,Vol 30,Volatiles,Volcanic arc,Volcanic rifted margin,Volcanic rocks,Volcanic successions,Volcanism,Volcanology,Wave-cut bench,West Bengal,West Gondwana,West Iberian Margin magmatism,Western Cameroon,Western Gondwana,Western USA,Wide-angle seismic,Window size,Windows,XANES,Xenoliths,Xinjiang Autonomous Region,Yunnan,Zigana Granitoid,Zircon,Zircon U-Pb-Hf isotopes,Zircon U–Pb dating,Zircon ages,Zircon dating,Zirconium,Zona Econ{\^{o}}mica Exclusiva das regi{\~{o}}es Central e Nor,a,a an{\'{a}}lise do padr{\~{a}}o,a atividade vulc{\^{a}}nica nesta,a avalia{\c{c}}{\~{a}}o de dados,a dada,a evolu{\c{c}}{\~{a}}o de tais,a paleoproterozoic unit constituted,a potential petrogenetic and,a preserva{\c{c}}{\~{a}}o parcial,a prov{\'{i}}ncia cont{\'{e}}m algumas,a-si,absolute age,abstract geochemistry and petrology,abstract investigation of the,abyssal peridotites,acampamento velho,acumula{\c{c}}{\~{a}}o de hidrocarbonetos,adem{\'{a}}s se realiza una,adquiridos e processados em,agent-based modelling,aires,al,alcalinas situada no sudeste,alcalino da por{\c{c}}{\~{a}}o sul,alcalinos na por{\c{c}}{\~{a}}o norte,algumas evid{\^{e}}ncias geol{\'{o}}gicas,aliados a dados geol{\'{o}}gicos,alkaline,alkaline basalts,alkaline complexes,alkaline earth metals,alkaline rock,alkaline rocks,alkaline syenite,alkaline-carbonatite complexes,almacenamiento,amphibole,amphibole composition,amphibole nomenclature,amphibolite,amphibolites,an evolution of active,analisar,and dykes,and e,and pb isotope signatures,and percentage of,angola-etendeka province,an{\'{a}}lise multi - escala,ao litoral do,ao longo do plano,aos metapsamitos,apip,application in structural analysis,apresenta resultados de an{\'{a}}lises,apresentando n{\'{i}}veis intrusivos,ar,ar geochronology,ar-ar age,ara{\'{u}}jo,arc basin,arizona rhyolite compositions,arm's length principle,arraial do cabo,article,as bacias sedimentares,as intrus{\~{o}}es e extrus{\~{o}}es,as principais,asset management,associadas,associa{\c{c}}{\~{a}}o vulcanossedimentar arqueana do,atl{\^{a}}ntica do continente tem,attitude sensors {\^{a}}ngulos de,bachelorThesis,bacias da margem continental,bacias sedimentares,back&hyphen,baixo-tio 2 e alto-tio,balizada pela idade das,basaltic dikes,basaltic vulcanism,basalto,basaltos e andesitos bas{\'{a}}lticos,basalts,basanite,basin analysis,basin development,batholiths,bloco em fase explorat{\'{o}}-,borda sudeste da bacia,boundary layer instabilities,brasil,brasileira,brazil,brazilian alkaline complexes,brazilian sedimentary basins,bulk silicate Earth,by tonalitic,c ashano,ca,cabo,cabo frio,cabo frio island,cambrian,carbonatite,catapleiite,central and southern brazil,ceo inferior,cerca de 250 x,cerca de 5000 m,cf,chegado ao limite leste,chemical stratigraphy - magma,chilwa,chondrite,cite this article,classification,classroom spaces,coastal basins,coastal region,com,com contribui{\c{c}}{\~{o}}es locais de,com rochas b{\'{a}}sicas-ultrab{\'{a}}sicas vulcanocl{\'{a}}sticas,comin-chiaramonti et,como,como geossinclinal e tect{\^{o}}nica,comparando-o com o das,comparison of energy consumption,complex,composition of amphiboles from,composi{\c{c}}{\~{a}}o qu{\'{i}}mica e evolu{\c{c}}{\~{a}}o,comp{\~{o}}em as serras do,conhe-,contains supplementary,continental crust,continental extension,continental flood basalts -,continental margin,continental margin in the,continental rifting,convection,copyright 2005 by svetlana,corpo intrusivo da ilha,corporate tax,correlations,corresponding author,cosmogenic nuclides,cretaceous,cretaceous flood tholeiites,cretaceous until eocene times,cristalinos mais ricos em,crossite,crust,crustal anatexis,crustal assimilation,crustal contamination,crustal recycling,crustal structure,cuja resolu{\c{c}}{\~{a}}o {\'{e}} sobretudo,cummingtonite,d,da crosta para o,da ilha de cabo,da passagem da placa,da textura e mineralogia,dados s{\'{i}}smicos tridimensionais de,dados th-u-pb total por,dannemorite,das mais extensas exposi{\c{c}}{\~{o}}es,data science,dates,daylight,daylight factor,daylight level,daylighting,daylighting architecture,daylighting calculation,daylighting design,daylighting tools,de,de afinidade tholeiitica com,de campo e considera{\c{c}}{\~{a}}o,de caraj{\'{a}}s,de contato dos diques,de diques plio-pleistoc{\^{e}}nicos da,de falhas naturais,de goi{\'{a}}s,de idade cret{\'{a}}ceo superior,de iguape,de janeiro,de lineamentos na,de natureza vulc{\^{a}}nica alcalina,de orienta{\c{c}}{\~{a}}o do enxame,de placas,de profundidade,de rochas alcalinas,de rochas magm{\'{a}}ticas predo,de um grande edif{\'{i}}cio,decay seri,decay series,delamina{\c{c}}{\~{a}}o t{\'{e}}rmica ou fraturamento,department of geological,depleted,depth-dependent thermal expansivity,desarrollo de nuevos productos,despertado quest{\~{o}}es controvertidas,detachment,diab{\'{a}}sio,diferencia{\c{c}}{\~{a}}o do magma de,dike swarm,diques,diques da serra do,dire{\c{c}}{\~{a}}o de sh max,dire{\c{c}}{\~{a}}o wnw-ese,do continente,do estado de s{\~{a}}o,do parna{\'{i}}ba,do plano de contato,do plat{\^{o}} do taquarembo,doi,doi:10.,doi:10.1029/2000GL012426,doi:10.1029/2004GL022192,doi:10.1029/2005JB003732,doi:10.1029/9,doi:10.1029/91JB01933,doi:10.1029/94JB00661,doi:10.1029/98JB02642,doi:10.1029/JB073i002p00619,dom pedrito,domenico m,doronzo,dos diques m{\'{a}}ficos da,dos metagabros {\'{e}} o,dr,duas su{\'{i}}tes,durante a,durante o {\'{e}}oceno,dyke swarm,e,e ambientes associados,e arraial do cabo,e condicionamento tect{\^{o}}nico da,e la,e n8,e paleomagn{\'{e}}ticos,e vulc{\^{a}}nicas na por{\c{c}}{\~{a}}o,early stages of design,early-,editorial handling,electronic supplementary material the,elementos de simetria,em adotar crit{\'{e}}rios e,em condi{\c{c}}{\~{o}}es de baixa,em fun{\c{c}}{\~{a}}o da necessidade,em parte,emi-himu signature,encantadas complex,energy,energy loads,entre otros,esse hot spot teria,esta unidade neoproteroz{\'{o}}ica {\'{e}},este artigo apresenta a,este artigo apresenta descri{\c{c}}{\~{o}}es,estes basaltos,estes dados sugerem,euler,euler angles,evaluaci{\'{o}}n de las,evento metam{\'{o}}rf{\"{i}}co-deformacional progressivo e,everton marques bongiolo,evolu{\c{c}}{\~{a}}o dos conhecimentos sobre,exhumation,exibem caracter{\'{i}}sticas estruturais e,experimental petrology,explosive eruption,extended kalman filter,extrusive,f,fault-plane markings,fei{\c{c}}{\~{o}}es {\'{i}}mpares da borda,filtro de,first author,flood basalts,fluid,fluidisation,fonolitos,foreign direct investment,fozo,fractionation,fractionation crystallization,fracture zone,fracture zones,frequentemente negligenciada,frio,from early,g,gabbro xe-,gap,garnet,genesis,gen{\'{e}}ticas para os xen{\'{o}}litos,geobarometry,geochemical modeling,geochemistry,geochronology,geocronol{\'{o}}gicos k,geodynamics,geological structures,geomatics 1,geomorfol{\'{o}}gicas e geocronol{\'{o}}gicas,geoprocessing,geoqu{\'{i}}mica,geotectonics,geothermobarometric indicator,geothermobarometry,geothermometry,glass - vesicles,glazing,glazing to wall area,glazing type,grandense,granites,grupo gr{\~{a}}o-par{\'{a}},gwar,h,hawaiian tholeiite composition -,hc.mk,heat flow,heterog{\'{e}}neo,hidr{\'{a}}ulico de cizalhamento,high temperature alteration,hot spot,hot spots,hotspot,hotspots,hotspots and melting anomalies,http://dx.doi.org/10.1029/2000GL012426,http://dx.doi.org/10.1029/2004GL022192,http://dx.doi.org/10.1029/2005JB003732,http://dx.doi.org/10.1029/91JB01933,http://dx.doi.org/10.1029/94JB00240,http://dx.doi.org/10.1029/94JB00661,http://dx.doi.org/10.1029/98JB02642,http://dx.doi.org/10.1029/JB073i002p00619,http://dx.doi.org/10.1029/JB082i005p00803,http://dx.doi.org/10.1029/JB089iB07p05835,http://dx.doi.org/10.1029/JB094iB06p07278,https,https://dspace.lboro.ac.uk/2134/20417,hydraulic shear fracturing,hydrothermal alteration,icle,igneous,igneous rocks,illuminance,impact structures,incluem-se numa s{\'{e}}rie transicional,incluindo desde complexos m{\'{a}}fico-ultram{\'{a}}ficos,indicators,influenciados por teorias geotect{\^{o}}nicas,infrastructure,inicialmente,initial kinematic reconstruction,integram o enxame de,integrated,internet of things,interpretation,intraplate deformation,intraplate volcanism,introduction and geological setting,introduction the paran{\'{a}} basin,introdu{\c{c}}{\~{a}}o este trabalho sintetiza,introdu{\c{c}}{\~{a}}o estudos realizados na,intrusions,intrusiva de pariq{\"{u}}era a{\c{c}}u,intrusive,intr{\'{i}}nseca de se ordenar,inverse-forward modelling,in{\'{u}}meras,is characterized by early,isochron,isotope,isotope and trace element,isotope fractionation,isotope geochemistry,isotope ratios,isotopes,isot{\'{o}}picas rb-sr de interesse,ito and van keken,iv simp{\'{o}}sio de vulcanismo,iwanuch,j,japi,jgg-1-1-7,jourdan,journal of geosciences and,k,k-ar dispon{\'{i}}veis na literatura,kalman estendido,kamafugite,kimberlite pipe,l,l stratigraphic chart,large igneous province,large igneous provinces,lava flow,lead,lineages,linear volcanic rises,lip,lithochemistry,lithogeochemistry,lithosphere,litogeoqu{\'{i}}mica,litosf{\'{e}}rica sul-americana por sobre,lo,location and orientation in,los campos de la,lower paleozoic,luminance,l{\'{i}}quidos,m,mafic dyke,mafic dyke swarms,mafic dyke swarms of,magma,magma chamber,magmatic lineaments,magmatic sources,magmatic sources of post-collisional,magmatic volatiles,magmatism,magm{\'{a}}tica das rochas alcalinas,magnetic anomalies,maior parte dos casos,manjo,mantle,mantle evolution,mantle geochemistry,mantle lithosphere,mantle melting,mantle plumes,mantle source,mantle sources,mantle temperatures,mantle wedge,manufacturing and processing,mar e da mantiqueira,mar no sudeste do,margem con-,marginal basins,mello,melt,melt petrogenesis,melting anomaly,mesozoic,mesozoic-cenozoic magmatism,metagabbros,metagabros da sequ{\^{e}}ncia metavulcanossedimentar,metagranites of encantadas,metals,metapelitos,methodology,metrics,mica,microcrystalline silicon,microqu{\'{i}}micos,microssonda,mid-atlantic ridge,minas gerais,mineral chemistry,mineral composition,mineral compositions - rhyolitic,mineral redox buffer,minous magmatism occurred in,miocene volcanism,missing Ar,mobile belt,morb,motoki,multinational enterprise,mush,mylonites,m{\'{a}}ficos da {\'{a}}rea de,n,na,na regi{\~{a}}o do baixo,nb,nd,nd model ages,near-solidus,nefelina sienito com assimila{\c{c}}{\~{a}}o,neodymium,neoproterozoic,nepheline syenite,nephelinite,no,no caso correspondente a,no eocret{\'{a}}ceo pr{\'{e}}-aptiano,no estado do rio,noliths - magma convection,nonchondritic Earth,normal-reverse magnetizations,normalization,northcentral nigeria,nova brasil{\^{a}}ndia,numerical basin modeling,numerical modeling,nw,o,o artigo,o conhecimento,o de anomalias magn,o magmatismo cret{\'{a}}ceo-terci{\'{a}}rio nas,o pacote vulc{\^{a}}nico,o remanescente na interpretac,o vulcanismo bas{\'{a}}ltico {\'{e}},o-c-sr-nd isotopes,ocean island basalts,ocorre ao longo de,of porphyritic and equigranular,of post-collisional alkaline,oib,olbina,olivine,online version of this,orbitais e a{\'{e}}reos aplicados,org,oria-trindade chain,os valores de idades,ou seja,p e alta t,p-morb,pa-,paep,pago,paleogene,paleomagnetic virtual poles,paleomagnetism,paleoprotero-,paleoproterozoic,panafrican,para desarrollar aplicaciones en,para os,parana,parentais da su{\'{i}}te de,part of the paran{\'{a}}-,partial melting,partially layered convection,particle size distribution,passive margin,pattern,pau-,pequena exposi{\c{c}}{\~{a}}o de rochas,peridotite,permite limitar mais adequada-,permitiu a determina{\c{c}}{\~{a}}o da,pertencentes ao distrito ferrifero,pesquisas que t{\^{e}}m sido,petrakis - xen{\'{o}}litos tabulares,petrography,petroleum exploration,petrology,petrology.exp,petrol{\'{i}}feros da,petrol{\'{i}}feros e modelos de,ph,phlogopite,phonolite,phonolites and nepheline syenites,pico viejo,pirocl{\'{a}}sticas e vulcanocl{\'{a}}sticas denominada,placa litosf{\'{e}}rica,plate divergence,pleistocene,pliocene,plugs fonol{\'{i}}ticos,plume,plumes,plutonic rocks,ponta grossa arch,por uma,por{\c{c}}{\~{a}}o nordeste da ilha,por{\c{c}}{\~{a}}o oeste do escudo,post-collisional magmatism,post-perovskite phase transition,po{\c{c}}os de caldas,po{\c{c}}os de caldas-cabo frio,pp 630-635,predicted bathymetry,predictive maintenance,predominantes na por{\c{c}}{\~{a}}o central,present address,pressure,primitive mantle,principalmente em func,procesamiento de alimentos,producci{\'{o}}n primaria,prof,propor esquemas para classificar,prop{\~{o}}e-se que o alinhamento,proterozoic granite,pv module,pyroxene,pyroxene group,que se estende na,r,radiative heat transfer in,radioactive disequilibrium,radioactive isotopes,radiogenic isotopes,ran,rare earth element modeling,rare earths,ratio,rb,reactivation,realizadas no sentido de,redox reactions,redox zonations,referida geralmente como forma{\c{c}}{\~{a}}o,reflex{\~{a}}o,regi{\~{a}}o,remanent magnetization,remonta provavelmente ao paleoceno,resultado da maior compet{\^{e}}ncia,resumo,resumo - motoki,resumo a ilha da,resumo a origem dos,resumo a prov{\'{i}}ncia alcalina,resumo ao longo da,resumo com base em,resumo o maci{\c{c}}o alcalino,resumo o presente artigo,resumo o vulcanismo {\'{a}}cido,resumo os anf{\'{i}}bolitos e,resumo os corpos n4,resumo sintetizam-se informa{\c{c}}{\~{o}}es sobre,rheology,rhyolite mineral compositions,rhyolites,rhyolites -,ribeira belt,rift,rifting,rj,rochas alcalinas sub-vulc{\^{a}}nicas,rochas f{\'{e}}lsicas,rochas pirocl{\'{a}}sticas,ron fodor,rosenbuschite,rs,rs est{\'{a}} localizado na,s,s institution,s12517-019-4424-y,santa catarina state,santana da boa vista,santos basin,santos basin l stratigraphy,sciences,sedimentary basins,sedimentation,segundo n60w,seguridad alimentaria,seismic interpretation,seismic stratigraphy,sendo representada nesta regi{\~{a}}o,sensores de atitude,sequence,sequ{\^{e}}ncia vulc{\^{a}}nica {\'{a}}cida,serra do mar dyke,serra dos caraj{\'{a}}s,shear heating,shoshonitic association as the,shoshonitic association is related,shoshonitic associations,shoshonitic series based upon,sichel,sidelighting,silva,simulation,sistemas montanhosos subparalelos que,sliding normalization,sliding normalization technique using,south atlantic,south-american plate,southeast Brazil,southeast atlantic ocean,southern brazil,southern brazilian rifted margin,sp-mg,sr,sr and k,sr-nd-pb isotopes,stability,stable,stable isotopes,stereographic projection,stress-field,strontium,structural geology,structure,subcontinental lithospheric mantle,subduction,subduction zone,submarine,submersa a,subvulc{\^{a}}nicos e nefelina sienitos,sucess{\~{a}}o de rochas efusivas,sudeste do brasil,suites,sul,sul-rio-,sul-rio-grandense shield,sunlight,superf{\'{i}}cies de eros{\~{a}}o do,sustainability,sva,sw amazonian craton,swarm,syenite,s{\~{a}}o analisados e comparados,s{\~{a}}o constitu{\'{i}}dos por uma,t,t - continental break-up,tabular xenolith,tabulares observados ao longo,tamb{\'{e}}m do alongamento de,teaching-learning,tectonic evolution,tectonic reactivation,tectonics,tectonism,tectono-magmatic activation,tectono-metamorphic evolution,teide,temperature- and pressure-dependent viscosity,tenerife,tenha se implantado quando,terr{\ae} didatica 2,texturais que refletem um,the,the encantadas complex is,the lavras do sul,thermal delamination,thermal transmittance,thermochronology,thermometry,this includes the extensive,tholeiites,tholeiitic basalts,tholeiitic series,tijucas terrane,tims,tinental brasileira e nas,tinguaitos,tirodite,to the early stages,toro diorite,toro dioritic complex,transfer pricing,transparent blinds,trazabilidad,treatise on geophysics,trindade,trindade island,tristan da cunha plume,trondhjemitic,types - boreholes -,ultrapotassic,um hot spot,uma faixa de dire{\c{c}}{\~{a}}o,universidade federal do rio,upper Precambrian,upwelling rates,vale do rio ribeira,vargas,venite,vertical foreclosure,virginia polytechnic institute and,vit,vit{\'{o}}ria-trindade chain,vogelsberg,volcanic rock,volcanism,volcano,volu-,volume,vulc{\^{a}}nico cuja base encontra-se,v{\'{a}}rios autores se preocuparam,w,water,western cameroon,wide-angle seismic,with regard to type,xenoliths,yb,zircon,{\`{a}},{\`{a}} compreens{\~{a}}o da origem,{\`{a}} deforma{\c{c}}{\~{a}}o em rela{\c{c}}{\~{a}}o,{\'{a}}rea de cabo frio,{\'{a}}reas emersas adjacentes,{\'{a}}reas oce{\^{a}}nicas adjacentes per-,{\c{c}}{\~{a}}o petrol{\'{i}}fera de um,{\'{e}} a por{\c{c}}{\~{a}}o emersa,{\'{e}} composto essencialmente por,{\'{e}} formado principalmente por,{\'{e}}poca de forma{\c{c}}{\~{a}}o,$\sigma$ 1,Киари}, -number = {9}, -pages = {1689--1699}, -pmid = {25246403}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}}, -url = {http://publications.lib.chalmers.se/records/fulltext/245180/245180.pdf%0Ahttps://hdl.handle.net/20.500.12380/245180%0Ahttp://dx.doi.org/10.1016/j.jsames.2011.03.003%0Ahttps://doi.org/10.1016/j.gr.2017.08.001%0Ahttp://dx.doi.org/10.1016/j.precamres.2014.12}, -volume = {53}, -year = {2015} -} -@article{Wood2014, -abstract = {The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D and Hall, D J and Murray, N J and Gow, J P D and Holland, A and Turner, P and Burt, D}, -doi = {10.1088/1748-0221/9/12/C12028}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv,visible and ir photons (s}, -number = {12}, -pages = {C12028----C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyse sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in 255 deg2 of the Kilo Degree Survey (KiDS), one of the currentgeneration optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii ≳1.4 arcsec, about twice the r-band seeing in KiDS. In a sample of 21 789 colour-magnitude selected luminous red galaxies (LRGs), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find {\$\sim${}}100 massive LRGgalaxy lenses at z ≲ 0.4 in KiDS when completed. In the most optimistic scenario, this number can grow considerably (to maximally {\$\sim${}}2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C E and Tortora, C and Chatterjee, S and Vernardos, G and Koopmans, L V E and Kleijn, G Verdoes and Napolitano, N R and Covone, G and Schneider, P and Grado, A and McFarland, J}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys,cD}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and $\backslash$nspectroscopic ESA cornerstone mission, currently scheduled for launch in$\backslash$nlate 2011. Its primary science drivers are the composition, formation$\backslash$nand evolution of the Galaxy. Gaia will not achieve its scientific$\backslash$nrequirements without detailed calibration and correction for radiation$\backslash$ndamage. Microscopic models of Gaia's CCDs are being developed to$\backslash$nsimulate the effect of radiation damage, charge trapping, which causes$\backslash$ncharge transfer inefficiency. The key to calculating the probability of$\backslash$na photoelectron being captured by a trap is the 3D electron density$\backslash$nwithin each CCD pixel. However, this has not been physically modelled$\backslash$nfor Gaia CCD pixels. In this paper, the first of a series, we motivate$\backslash$nthe need for such specialised 3D device modelling and outline how its$\backslash$nfuture results will fit into Gaia's overall radiation calibration$\backslash$nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -isbn = {9780819472311}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy III}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Cox2006, -abstract = {We use numerical simulations to study the kinematic structure of remnants formed from mergers of equal-mass disk galaxies. In particular, we show that remnants of dissipational mergers, which include the radiative cooling of gas, star formation, feedback from supernovae, and the growth of supermassive black holes, are smaller, rounder, have, on average, a larger central velocity dispersion, and show significant rotation compared to remnants of dissipationless mergers. The increased rotation speed of dissipational remnants owes its origin to star formation that occurs in the central regions during the galaxy merger. We have further quantified the anisotropy, three-dimensional shape, minor-axis rotation, and isophotal shape of each merger remnant, finding that dissipational remnants are more isotropic, closer to oblate, have the majority of their rotation along their major axis, and are more disky than dissipationless remnants. Individual remnants display a wide variety of kinematic properties. A large fraction of the dissipational remnants are oblate isotropic rotators. Many dissipational remnants, and all of the dissipationless ones, are slowly rotating and anisotropic. The remnants of gas-rich major mergers can well reproduce the observed distribution of projected ellipticities, rotation parameter (V/$\sigma$)*, kinematic misalignments, $\psi$, and isophotal shapes. The dissipationless remnants are a poor match to this data. We also investigate the properties of merger remnants as a function of initial disk gas fraction, orbital angular momentum, and the mass of the progenitor galaxies. Our results support the merger hypothesis for the origin of low-luminosity elliptical galaxies provided that the progenitor disks are sufficiently gas-rich, however our remnants are a poor match to the bright ellipticals that are slowly rotating and uniformly boxy. {\textcopyright} 2006. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0607446}, -author = {Cox, T. J. and Dutta, Suvendra N. and {Di Matteo}, Tiziana and Hernquist, Lars and Hopkins, Philip F. and Robertson, Brant and Springel, Volker}, -doi = {10.1086/507474}, -eprint = {0607446}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Elliptical and Lenticular,Galaxies: Evolution,Galaxies: Formation,Galaxies: Interactions,Methods: n-Body Simulations,cD}, -month = {oct}, -number = {2}, -pages = {791--811}, -primaryClass = {astro-ph}, -title = {{The Kinematic Structure of Merger Remnants}}, -url = {http://stacks.iop.org/0004-637X/650/i=2/a=791}, -volume = {650}, -year = {2006} -} -@article{LeFloch2005, -abstract = {We analyze a sample of {\$\sim${}}2600 MIPS/Spitzer 24mic sources brighter than {\$\sim${}}80muJy and located in the Chandra Deep Field South to characterize the evolution of the comoving infrared (IR) energy density of the Universe up to z{\$\sim${}}1. Using published ancillary optical data we first obtain a nearly complete redshift determination for the 24mic objects associated with R{\textless}24 counterparts at z{\textless}1. We find that the 24mic population at 0.5{\textless}z{\textless}1 is dominated by ``Luminous Infrared Galaxies'' (i.e., 10{\^{}}11 L{\_}sol {\textless} L{\_}IR {\textless} 10{\^{}}12 L{\_}sol), the counterparts of which appear to be also luminous at optical wavelengths and tend to be more massive than the majority of optically-selected galaxies. We finally derive 15mic and total IR luminosity functions (LFs) up to z{\$\sim${}}1. In agreement with the previous results from ISO and SCUBA and as expected from the MIPS source number counts, we find very strong evolution of the contribution of the IR-selected population with lookback time. Pure evolution in density is firmly excluded by the data, but we find considerable degeneracy between strict evolution in luminosity and a combination of increases in both density and luminosity (L*{\_}IR prop. to (1+z){\^{}}{\{}3.2{\_}{\{}-0.2{\}}{\^{}}{\{}+0.7{\}}{\}}, Phi*{\_}IR prop. to (1+z){\^{}}{\{}0.7{\_}{\{}-0.6{\}}{\^{}}{\{}+0.2{\}}{\}}). Our results imply that the comoving IR energy density of the Universe evolves as (1+z){\^{}}(3.9+/-0.4) up to z{\$\sim${}}1 and that galaxies luminous in the infrared (i.e., L{\_}IR {\textgreater} 10{\^{}}11 L{\_}IR) are responsible for 70+/-15{\%} of this energy density at z{\$\sim${}}1. Taking into account the contribution of the UV luminosity evolving as (1+z){\^{}}{\$\sim${}}2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z{\$\sim${}}0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24mic fluxes into luminosities.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506462}, -author = {{Le Floc'h}, Emeric and Papovich, Casey and Dole, Herve and Bell, Eric F and Lagache, Guilaine and Rieke, George H and Egami, Eiichi and Perez‐Gonzalez, Pablo G and Alonso‐Herrero, Almudena and Rieke, Marcia J and Blaylock, Myra and Engelbracht, Charles W and Gordon, Karl D and Hines, Dean C and Misselt, Karl A and Morrison, Jane E and Mould, Jeremy}, -doi = {10.1086/432789}, -eprint = {0506462}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Observations,Galaxies: Evolution,Galaxies: High-Redshift,Infrared: Galaxies}, -month = {oct}, -number = {1}, -pages = {169--190}, -primaryClass = {astro-ph}, -title = {{ Infrared Luminosity Functions from the Chandra Deep Field–South: The Spitzer View on the History of Dusty Star Formation at 0 ≲ z ≲ 1 }}, -url = {http://arxiv.org/abs/astro-ph/0506462%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/432789}, -volume = {632}, -year = {2005} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR $\eta$(z) using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of 102 SGL with the measurement of corresponding velocity dispersion $\sigma$0 and Einstein radius $\theta$E. In addition, we also use a dataset of 12 two image lensing systems containing the measure of time delay $\Delta$ t between source images. Jointly these two datasets give us the angular diameter distance DAol of the lens. Further, for luminosity distance, we use the 740 observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ($\eta$=1) within 2$\sigma$ confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R. F.L.}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rana et al. - 2017 - Probing the cosmic distance duality relation using time delay lenses(2).pdf:pdf}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Woo2014, -abstract = {We investigate the roles of two classes of quenching mechanisms for central and satellite galaxies in the Sloan Digital Sky Survey (z < 0.075): those involving the halo and those involving the formation of a compact centre. For central galaxies with inner compactness $\Sigma$1 kpc $\sim$ 109-9.4M⊙ kpc-2, the quenched fraction fq is strongly correlated with $\Sigma$1 kpc with only weak halo mass Mh dependence. However, at higher and lower $\Sigma$1 kpc, specific star formation rate (sSFR) is a strong function of Mh and mostly independent of $\Sigma$1 kpc. In other words, $\Sigma$1 kpc $\sim$ 109-9.4M⊙ kpc-2 divides galaxies into those with high sSFR below and low sSFR above this range. In both the upper and lower regimes, increasing Mh shifts the entire sSFR distribution to lower sSFR without a qualitative change in shape. This is true even at fixed M*, but varying M* at fixed Mh adds no quenching information. Most of the quenched centrals with Mh > 1011.8M⊙ are dense ($\Sigma$1 kpc > 109M⊙ kpc-2), suggesting compaction-related quenching maintained by halo-related quenching. However, 21 per cent are diffuse, indicating only halo quenching. For satellite galaxies in the outskirts of haloes, quenching is a strong function of compactness and a weak function of host Mh. In the inner halo, Mh dominates quenching, with $\sim$90 per cent of the satellites being quenched once Mh > 1013M⊙. This regional effect is greatest for the least massive satellites. As demonstrated via semi-analytic modelling with simple prescriptions for quenching, the observed correlations can be explained if quenching due to central compactness is rapid while quenching due to halo mass is slow.}, -archivePrefix = {arXiv}, -arxivId = {1406.5372}, -author = {Woo, Joanna and Dekel, Avishai and Faber, S. M. and Koo, David C.}, -doi = {10.1093/mnras/stu2755}, -eprint = {1406.5372}, -isbn = {0792388801}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: general,Galaxies: groups: general,Galaxies: haloes,Galaxies: star formation,Galaxies: structure}, -number = {1}, -pages = {237--251}, -title = {{Two conditions for galaxy quenching: Compact centres and massive haloes}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.448..237W}, -volume = {448}, -year = {2015} -} -@article{Bristow2002, -author = {Bristow, P and Alexov, A and Kerber, F and Rosa, M}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bristow et al. - 2002 - Modelling Charge Transfer on the STIS CCD(2).pdf:pdf}, -journal = {in Proc. 2002 HST Calibration Workshop: Hubble after the Installation of the ACS and the NICMOS Cooling System, ed.}, -pages = {176--179}, -title = {{Modelling Charge Transfer on the STIS CCD}}, -year = {2002} -} -@article{Vegetti2012, -abstract = {The mass function of dwarf satellite galaxies that are observed around Local Group galaxies differs substantially from simulations based on cold dark matter: the simulations predict many more dwarf galaxies than are seen. The Local Group, however, may be anomalous in this regard. A massive dark satellite in an early-type lens galaxy at a redshift of 0.222 was recently found using a method based on gravitational lensing, suggesting that the mass fraction contained in substructure could be higher than is predicted from simulations. The lack of very low-mass detections, however, prohibited any constraint on their mass function. Here we report the presence of a (1.9 ± 0.1) × 10 8M ⊙ dark satellite galaxy in the Einstein ring system JVAS B1938+666 (ref. 11) at a redshift of 0.881, where M ⊙ denotes the solar mass. This satellite galaxy has a mass similar to that of the Sagittarius galaxy, which is a satellite of the Milky Way. We determine the logarithmic slope of the mass function for substructure beyond the local Universe to be 1.1 +0.6-0.4, with an average mass fraction of 3.3 +3.6-1.8 per cent, by combining data on both of these recently discovered galaxies. Our results are consistent with the predictions from cold dark matter simulations at the 95 per cent confidence level, and therefore agree with the view that galaxies formed hierarchically in a Universe composed of cold dark matter. {\textcopyright} 2012 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1201.3643}, -author = {Vegetti, S. and Lagattuta, D. J. and McKean, J. P. and Auger, M. W. and Fassnacht, C. D. and Koopmans, L. V.E.}, -doi = {10.1038/nature10669}, -eprint = {1201.3643}, -isbn = {1476-4687 (Electronic)\n0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7381}, -pages = {341--343}, -pmid = {22258612}, -title = {{Gravitational detection of a low-mass dark satellite galaxy at cosmological distance}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012Natur.481..341V&link_type=ABSTRACT%5Cnpapers://dcc533b5-8613-47b7-b88c-2b0c0d39c33f/Paper/p4937}, -volume = {481}, -year = {2012} -} -@article{Talbot2018, -abstract = {We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for 8 of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with 2 background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched {\$\sim${}} 1.5 million spectra, of which 3065 contained multiple high signal-to-noise background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius {\textgreater}1.7", which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely.}, -archivePrefix = {arXiv}, -arxivId = {1803.03604}, -author = {Talbot, Michael S and Brownstein, Joel R and Bolton, Adam S and Bundy, Kevin and Andrews, Brett H and Cherinka, Brian and Collett, Thomas E and More, Anupreeta and More, Surhud and Sonnenfeld, Alessandro and Vegetti, Simona and Wake, David A and Weijmans, Anne Marie and Westfall, Kyle B}, -doi = {10.1093/mnras/sty653}, -eprint = {1803.03604}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: General,Gravitational lensing: Strong}, -number = {1}, -pages = {195--209}, -title = {{SDSS-IV MaNGA: The spectroscopic discovery of strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1803.03604%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty653}, -volume = {477}, -year = {2018} -} -@article{Iwanus2017, -abstract = {We describe and test a novel Dark Matter Annihilation Feedback (DMAF) scheme that has been implemented into the well known cosmological simulation code $\backslash$textsf{\{}GADGET-2{\}}. In the models considered here, dark matter can undergo self-annihilation/decay into radiation and baryons. These products deposit energy into the surrounding gas particles and then the dark matter/baryon fluid is self-consistently evolved under gravity and hydrodynamics. We present tests of this new feedback implementation in the case of idealised dark matter halos with gas components for a range of halo masses, concentrations and annihilation rates. For some dark matter models, DMAF's ability to evacuate gas is enhanced in lower mass, concentrated halos where the injected energy is comparable to its gravitational binding energy. Therefore, we expect the strongest signs of dark matter annihilation to imprint themselves onto the baryonic structure of concentrated dwarf galaxies through their baryonic fraction and star formation history. Finally we present preliminary results of the first self-consistent DMAF cosmological box simulations showing that the small scale substructure is washed out for large annihilation rates.}, -archivePrefix = {arXiv}, -arxivId = {1707.06770}, -author = {Iwanus, N and Elahi, P J and Lewis, G F}, -doi = {10.1093/MNRAS/STX1974}, -eprint = {1707.06770}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Large-scale structure of Universe}, -number = {1}, -pages = {1214--1225}, -title = {{Dark matter annihilation feedback in cosmological simulations - I: Code convergence and idealized haloes}}, -url = {http://arxiv.org/abs/1707.06770%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1974}, -volume = {472}, -year = {2017} -} -@article{LaBarbera2012, -abstract = {Radial trends of stellar populations in galaxies provide a valuable tool to understand the mechanisms of galaxy growth. In this paper, we present the first comprehensive analysis of optical-optical and optical-NIR colours, as a function of galaxy mass, out to the halo region (8Re) of early-type galaxies (ETGs). We select a sample of 674 massive ETGs (M*≳ 3 × 1010MȮ) from the Sloan Digital Sky Survey (SDSS)-based SPIDER survey. By comparing with a large range of population synthesis models, we derive robust constraints on the radial trends in age and metallicity. Metallicity is unambiguously found to decrease outwards, with a measurable steepening of the slope in the outer regions (Re > R > 8Re). The gradients in stellar age are found to be more sensitive to the models used, but in general, the outer regions of ETGs feature older populations compared to the cores. This trend is strongest for the most massive galaxies in our sample (M*≳ 1011Ṁ). Furthermore, when segregating with respect to large-scale environment, the age gradient is more significant in ETGs residing in higher density regions. These results shed light on the processes leading from the formation of the central core to the growth of the stellar envelope of massive galaxies. The fact that the populations in the outer regions are older and more metal-poor than in the core suggests a process whereby the envelope of massive galaxies is made up of accreted small satellites (i.e. minor mergers) whose stars were born during the first stages of galaxy formation. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1208.0587}, -author = {{La Barbera}, F. and Ferreras, I. and de Carvalho, R. R. and Bruzual, G. and Charlot, S. and Pasquali, A. and Merlin, E.}, -doi = {10.1111/j.1365-2966.2012.21848.x}, -eprint = {1208.0587}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Stellar content,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {3}, -pages = {2300--2317}, -title = {{SPIDER-VII. Revealing the stellar population content of massive early-type galaxies out to 8Re}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2012.21848.x}, -volume = {426}, -year = {2012} -} -@article{Zavala2012, -abstract = {We use the combined data sets of the Millennium I and II cosmological simulations to revisit the impact of mergers in the growth of bulges in central galaxies in the $\Lambda$ cold dark matter ($\Lambda$CDM) scenario. We seed galaxies within the growing CDM haloes using semi-empirical relations to assign stellar and gaseous masses, and an analytic treatment to estimate the transfer of stellar mass to the bulge of the remnant after a galaxy merger. We find that this model roughly reproduces the observed correlation between the bulge-to-total mass (B/T) ratio and stellar mass (M *) in present-day central galaxies as well as their observed demographics, although low-mass B/T < 0.1 (bulgeless) galaxies might be scarce relative to the observed abundance. In our merger-driven scenario, bulges have a composite stellar population made of (i) stars acquired from infalling satellites, (ii) stars transferred from the primary disc due to merger-induced perturbations and (iii) newly formed stars in starbursts triggered by mergers. We find that the first two are the main channels of mass assembly, with the first one being dominant for massive galaxies, creating large bulges with different stellar populations than those of the inner discs, while the second is dominant for intermediate/low-mass galaxies and creates small bulges with similar stellar populations to the inner discs. We associate the dominion of the first (second) channel to classical (pseudo) bulges, and compare the predicted fractions to observations. We emphasize that our treatment does not include other mechanisms of bulge growth such as intrinsic secular processes in the disc or misaligned gas accretion. Interestingly, we find that the evolution of the stellar and gaseous contents of the satellite as it spirals towards the central galaxy is a key ingredient in setting the morphology of the remnant galaxy, and that a good match to the observed bulge demographics occurs when this evolution proceeds closely to that of the central galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1204.0516}, -author = {Zavala, Jesus and Avila-Reese, Vladimir and Firmani, Claudio and Boylan-Kolchin, Michael}, -doi = {10.1111/j.1365-2966.2012.22100.x}, -eprint = {1204.0516}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: interactions,Galaxies: structure}, -number = {2}, -pages = {1503--1516}, -title = {{The growth of galactic bulges through mergers in $\Lambda$ CDM haloes revisited - I. Present-day properties}}, -volume = {427}, -year = {2012} -} -@article{Pulsoni2017, -abstract = {Wolbachia is an intracellular endosymbiont that induces a variety of reproductive alterations in diverse arthropods. The almond moth, Cadra cautella, is double infected with two Wolbachia variants, wCauA and wCauB, and expresses complete cytoplasmic incompatibility (CI). The individual contribution of wCauA and wCauB to the expression of CI are unclear, however, because the two variants have not been separated in this host. The effect of wCauA is of particular interest because it induces male killing when transferred into the Mediterranean flour moth, Ephestia kuehniella. In the present study, we generated C. cautella infected with only wCauA by treating double-infected insects with tetracycline. Single-infected C. cautella exhibited strong CI, demonstrating that wCauA induces two distinct reproductive phenotypes in different hosts: CI in C. cautella and male killing in E. kuehniella. CI was also observed in the cross of double-infected males and single-infected females. Comparison of the single- and double-infected insects by real-time quantitative polymerase chain reaction suggested that the wCauA density is not affected much by the presence or absence of wCauB. {\textcopyright}2005 Nature Publishing Group All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {http://www.R-project.org}, -author = {Sasaki, T and Massaki, N and Kubo, T}, -doi = {10.1038/sj.hdy.6800737}, -eprint = {/www.R-project.org}, -isbn = {0018-067X}, -issn = {0018067X}, -journal = {Heredity}, -keywords = {Cadra cautella,Cytoplasmic incompatibility,Double infection,Male killing,Real-time quantitative PCR,Wolbachia}, -number = {5}, -pages = {389--393}, -pmid = {16106260}, -primaryClass = {http:}, -title = {{Wolbachia variant that induces two distinct reproductive phenotypes in different hosts}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/16106260}, -volume = {95}, -year = {2005} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high-resolution N-body simulations of galactic dark matter haloes to test if this remarkable property can be understood within the context of the cold dark matter (CDM) cosmology. We construct halo merger trees from the simulations and use a semi-analytic model to follow the formation of satellite galaxies. We find that in all six of our simulations, the 11 brightest satellites are indeed distributed along thin, disc-like structures analogous to that traced by the satellites of the Milky Way. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhaloes within it, which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhaloes but is similar to that of the subset of subhaloes that had the most massive progenitors at earlier times. The elongated disc-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I and Frenk, Carlos S and Cole, Shaun and Helly, John C and Jenkins, Adrian and Navarro, Julio F and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Greene2015, -abstract = {We examine stellar population gradients in {\$\sim${}}100 massive early type galaxies spanning 180 {\textless} sigma* {\textless} 370 km/s and M{\_}K of -22.5 to -26.5 mag, observed as part of the MASSIVE survey (Ma et al. 2014). Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius ({\$\sim${}}2.5 R{\_}e). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift) stellar age and [alpha/Fe] increase with increasing sigma* and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 R{\_}e, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\backslash$sigmastar, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung-Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -eprint = {1504.02483}, -title = {{The MASSIVE Survey II: Stellar Population Trends Out to Large Radius in Massive Early Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -year = {2015} -} -@article{Myers2003, -abstract = {The Cosmic Lens All-Sky Survey (CLASS) is an international collaborative programme which has obtained high-resolution radio images of over 10 000 flat-spectrum radio sources in order to create the largest and best-studied statistical sample of radio-loud gravitationally lensed systems. With this survey, combined with detailed studies of the lenses found therein, constraints can be placed on the expansion rate, matter density and dark energy (e.g. cosmological constant, quintessence) content of the Universe that are complementary to and independent of those obtained through other methods. CLASS is aimed at identifying lenses where multiple images are formed from compact flat-spectrum radio sources, which should be easily identifiable in the radio maps. Because CLASS is radio-based, dust obscuration in lensing galaxies is not a factor, and the relative insensitivity of the instrument to environmental conditions (e.g. weather, 'seeing') leads to nearly uniform sensitivity and resolution over the entire survey. In four observing 'seasons' from 1994 to 1999, CLASS has observed 13 783 radio sources with the Very Large Array (VLA) at 8.4 GHz in its largest 'A'-configuration (0.2-arcsec resolution). When combined with the Jodrell Bank VLA Astrometric Survey (JVAS), the CLASS sample contains over 16 000 images. A complete sample of 11685 sources was observed, selected to have a flux density of at least 30 mJy in the Green Bank Survey (GB6) catalogue at 4.85 GHz (spanning the declination range 0° ≤ $\delta$ ≤ 75° and |b| ≥ 10°, excluding the Galactic plane) and a spectral index $\alpha$ ≥ -0.5 between the NRAO-VLA Sky Survey (NVSS) at 1.4 GHz and the GB6. A typical 30-s CLASS snapshot reached an rms noise level of 0.4 mjy. So far, CLASS has found 16 new gravitational lens systems, and the JVAS/CLASS survey contains a total of 22 lenses. The follow-up of a small number of candidates using the VLA, MERLIN, the Very Long Baseline Array (VLBA) and optical telescopes is still underway. In this paper, we present a summary of the CLASS observations, the JVAS/CLASS sample, and statistics on sub-samples of the survey. An accompanying paper presents the lens candidate selection, and in a third paper the implications for cosmology are discussed.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0211073}, -author = {Myers, S. T. and Jackson, N. J. and Browne, I. W.A. and {De Bruyn}, A. G. and Pearson, T. J. and Readhead, A. C.S. and Wilkinson, P. N. and Biggs, A. D. and Blandford, R. D. and Fassnacht, C. D. and Koopmans, L. V.E. and Marlow, D. R. and McKean, J. P. and Norbury, M. A. and Phillips, P. M. and Rusin, D. and Shepherd, M. C. and Sykes, C. M.}, -doi = {10.1046/j.1365-8711.2003.06256.x}, -eprint = {0211073}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing}, -month = {may}, -number = {1}, -pages = {1--12}, -primaryClass = {astro-ph}, -title = {{The Cosmic Lens All-Sky Survey -I. Source selection and observations}}, -volume = {341}, -year = {2003} -} -@article{Tinker2016, -abstract = {We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen etal (2012) clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of Mgal for galaxies with logMgal{\textgreater}=11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma{\_}logM. Using this approach, we find sigma{\_}logM=0.18{\^{}}{\{}+0.01{\}}{\_}{\{}-0.02{\}}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L and Brownstein, Joel R and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {121}, -title = {{The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -volume = {839}, -year = {2017} -} -@article{Veale2017a, -abstract = {We analyse the environmental properties of 370 local early-type galaxies (ETGs) in theMASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute K-band magnitude -21.5 ≳ MK ≳ -26.6, or stellar mass 8 × 109 ≲ M* ≲ 2 × 1012M⊙. We find these galaxies to reside in a diverse range of environments measured by four methods: group membership (whether a galaxy is a brightest group/cluster galaxy, satellite or isolated), halo mass, large-scale mass density (measured over a fewMpc) and local mass density (measured within the Nth neighbour). The spatially resolved IFS stellar kinematics provide robust measurements of the spin parameter $\lambda$e and enable us to examine the relationship among $\lambda$e, M* and galaxy environment. We find a strong correlation between $\lambda$e and M*, where the average $\lambda$e decreases from {\$\sim${}}0.4 to below 0.1 with increasing mass, and the fraction of slow rotators fslow increase from {\$\sim${}}10 to 90 per cent. We show for the first time that at fixed M*, there are almost no trends between galaxy spin and environment; the apparent kinematic morphology-density relation for ETGs is therefore primarily driven by M* and is accounted for by the joint correlations between M* and spin, and between M* and environment. A possible exception is that the increased fslow at high local density is slightly more than expected based only on these joint correlations. Our results suggest that the physical processes responsible for building up the present-day stellar masses of massive galaxies are also very efficient at reducing their spin, in any environment.}, -archivePrefix = {arXiv}, -arxivId = {1703.08573}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and McConnell, Nicholas and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/mnras/stx1639}, -eprint = {1703.08573}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {1428--1445}, -title = {{The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxies}}, -url = {http://arxiv.org/abs/1703.08573%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1639}, -volume = {471}, -year = {2017} -} -@article{McCarthy2010, -abstract = {The relatively recent insight that energy input from supermassive black holes (BHs) can have a substantial effect on the star formation rates (SFRs) of galaxies motivates us to examine the effects of BH feedback on the scale of galaxy groups. At present, groups contain most of the galaxies and a significant fraction of the overall baryon content of the Universe and, along with massive clusters, they represent the only systems for which it is possible to measure both the stellar and gaseous baryonic components directly. To explore the effects of BH feedback on groups, we analyse two high-resolution cosmological hydrodynamic simulations from the OverWhelmingly Large Simulations (OWLS) project. While both include galactic winds driven by supernovae, only one of the models includes feedback from accreting BHs. We compare the properties of the simulated galaxy groups to a wide range of observational data, including the entropy and temperature profiles of the intragroup medium, hot gas mass fractions, the luminosity-temperature and mass-temperature scaling relations, the K-band luminosity of the group and its central brightest galaxy (CBG), SFRs and ages of the CBG, and gas- and stellar-phase metallicities. Both runs yield entropy distributions similar to the data, while the run without active galactic nucleus (AGN) feedback yields highly peaked temperature profiles, in discord with the observations. Energy input from supermassive BHs significantly reduces the gas mass fractions of galaxy groups with masses less than a few × 1014 M⊙, yielding a gas mass fraction and X-ray luminosity scaling with system temperature that is in excellent agreement with the data, although the detailed scatter in the L-. T relation is not quite correct. The run without AGN feedback suffers from the well-known overcooling problem - the resulting stellar mass fractions are several times larger than observed and present-day cooling flows operate uninhibitedly. By contrast, the run that includes BH feedback yields stellar mass fractions, SFRs and stellar age distributions in excellent agreement with current estimates, thus resolving the long-standing 'cooling crisis' of simulations on the scale of groups. Both runs yield very similar gas-phase metal abundance profiles that match X-ray measurements, but they predict very different stellar metallicities. Based on the above, galaxy groups provide a compelling case that feedback from supermassive BHs is a crucial ingredient in the formation of massive galaxies. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0911.2641}, -author = {McCarthy, I. G. and Schaye, J. and Ponman, T. J. and Bower, R. G. and Booth, C. M. and Vecchia, C. Dalla and Crain, R. A. and Springel, V. and Theuns, T. and Wiersma, R. P.C.}, -doi = {10.1111/j.1365-2966.2010.16750.x}, -eprint = {0911.2641}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/McCarthy2010XraysGroups.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: clusters: general,Galaxies: formation,Galaxies: groups: general,Intergalactic medium,X-rays: galaxies: clusters}, -number = {2}, -pages = {822--839}, -title = {{The case for AGN feedback in galaxy groups}}, -volume = {406}, -year = {2010} -} -@article{Papadopoulos2011, -abstract = {We examine in detail the recent proposal that extreme cosmic ray dominated regions (CRDRs) characterize the interstellar medium of galaxies during events of high-density star formation, fundamentally altering its initial conditions (Papadopoulos 2010). Solving the coupled chemical and thermal state equations for dense UV-shielded gas reveals that the large CR energy densities in such systems [UCR∼ few × (103-104)UCR, Gal] will indeed raise the minimum temperature of this phase (where the initial conditions of star formation are set) from ∼10K (as in the Milky Way) to ∼50-100K. Moreover in such extreme CRDRs the gas temperature remains fully decoupled from that of the dust, with Tkin≫Tdust, even at high densities [n(H2) ∼ 105-106cm-3], quite unlike CRDRs in the Milky Way where Tk∼Tdust when n(H2) ≳ 105cm-3. These dramatically different star formation initial conditions will (i) boost the Jeans mass of UV-shielded gas regions by factors of ∼10-100 with respect to those in quiescent or less extreme star-forming systems and (ii) 'erase' the so-called inflection point of the effective equation of state of molecular gas. Both these effects occur across the entire density range of typical molecular clouds, and may represent a new paradigm for all high-density star formation in the Universe, with CRs as the key driving mechanism, operating efficiently even in the high dust extinction environments of compact extreme starbursts. The characteristic mass of young stars will be boosted as a result, naturally yielding a top-heavy stellar initial mass function (IMF) and a bimodal star formation mode (with the occurrence of extreme CRDRs setting the branching point). Such CRDRs will be present in Ultra-Luminous Infrared Galaxies (ULIRGs) and merger-driven gas-rich starbursts across the Universe where large amounts of molecular gas rapidly dissipate towards compact disc configurations where they fuel intense starbursts. In hierarchical galaxy formation models, CR-controlled star formation initial conditions lend a physical basis for the currently postulated bimodal IMF in merger/starburst versus quiescent/disc star-forming environments, while naturally making the integrated galactic IMFs a function of the star formation history of galaxies. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1009.2496}, -author = {Papadopoulos, Padeli P. and Thi, Wing Fai and Miniati, Francesco and Viti, Serena}, -doi = {10.1111/j.1365-2966.2011.18504.x}, -eprint = {1009.2496}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmic rays,Galaxies: interactions,Galaxies: star formation,Galaxies: starburst,ISM: molecules,ISM: supernova remnants}, -number = {2}, -pages = {1705--1714}, -primaryClass = {astro-ph.CO}, -title = {{Extreme cosmic ray dominated regions: A new paradigm for high star formation density events in the Universe}}, -volume = {414}, -year = {2011} -} -@article{Fergus2014, -abstract = {High dynamic range imagers aim to block or eliminate light from a very bright primary star in order to make it possible to detect and measure far fainter companions; in real systems, a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronagraph. The model uses principal components analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles, but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of the order of a percent of the brightness of the speckles, or up to 10-7 times the brightness of the primary star. This outperforms existing methods by a factor of two to three and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Lanusse2017a, -abstract = {Galaxy-scale strong gravitational lensing is not only a valuable probe of the dark matter distribution of massive galaxies, but can also provide valuable cosmological constraints, either by studying the population of strong lenses or by measuring time delays in lensed quasars. Due to the rarity of galaxy-scale strongly lensed systems, fast and reliable automated lens finding methods will be essential in the era of large surveys such as LSST, Euclid, and WFIRST. To tackle this challenge, we introduce CMU DeepLens, a new fully automated galaxy-galaxy lens finding method based on Deep Learning. This supervised machine learning approach does not require any tuning after the training step which only requires realistic image simulations of strongly lensed systems. We train and validate our model on a set of 20,000 LSST-like mock observations including a range of lensed systems of various sizes and signal-to-noise ratios (S/N). We find on our simulated data set that for a rejection rate of non-lenses of 99{\%}, a completeness of 90{\%} can be achieved for lenses with Einstein radii larger than 1.4" and S/N larger than 20 on individual {\$}g{\$}-band LSST exposures. Finally, we emphasize the importance of realistically complex simulations for training such machine learning methods by demonstrating that the performance of models of significantly different complexities cannot be distinguished on simpler simulations. We make our code publicly available at https://github.com/McWilliamsCenter/CMUDeepLens .}, -archivePrefix = {arXiv}, -arxivId = {1703.02642}, -author = {Lanusse, Fran{\c{c}}ois and Ma, Quanbin and Li, Nan and Collett, Thomas E and Li, Chun Liang and Ravanbakhsh, Siamak and Mandelbaum, Rachel and P{\'{o}}czos, Barnab{\'{a}}s}, -doi = {10.1093/mnras/stx1665}, -eprint = {1703.02642}, -isbn = {0021-9258 (Print)$\backslash$r0021-9258 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: statistical,gravitational lensing: strong}, -number = {3}, -pages = {3895--3906}, -pmid = {10913147}, -title = {{CMU DeepLens: Deep learning for automatic image-based galaxy-galaxy strong lens finding}}, -url = {http://arxiv.org/abs/1703.02642}, -volume = {473}, -year = {2018} -} -@article{Kitching2008, -abstract = {In this paper, we extend the Bayesian model fitting shape measurement method presented in Miller et al., and use the method to estimate the shear from the Shear TEsting Programme simulations (STEP). The method uses a fast model fitting algorithm that uses realistic galaxy profiles and analytically marginalizes over the position and amplitude of the model by doing the model fitting in Fourier space. This is used to find the full posterior probability in ellipticity. The shear is then estimated in a Bayesian way from this posterior probability surface. The Bayesian estimation allows measurement bias arising from the presence of random noise to be removed. In this paper, we introduce an iterative algorithm that can be used to estimate the intrinsic ellipticity prior and show that this is accurate and stable. We present results using the STEP parametrization that relates the input shear $\gamma$T to the estimated shear $\gamma$M by introducing a bias m and an offset c: $\gamma$M - $\gamma$T = m$\gamma$T + c. The average number density of galaxies used in the STEP1 analysis was 9 per square arcminute, for STEP2 the number density was 30 per square arcminute. By using the method to estimate the shear from the STEP1 simulations we find the method to have a shear bias of m = 0.006 ± 0.005 and a variation in shear offset with point spread function type of $\sigma$c = 0.0002. Using the method to estimate the shear from the STEP2 simulations we find that the shear bias and offset are m = 0.002 ± 0.016 and c = -0.0007 ± 0.0006, respectively. In addition, we find that the bias and offset are stable to changes in the magnitude and size of the galaxies. Such biases should yield any cosmological constraints from future weak lensing surveys robust to systematic effects in shape measurement. Finally, we present an alternative to the STEP parametrization by using a quality factor that relates the intrinsic shear variance in a simulation to the variance in shear that is measured and show that the method presented has an average of Q ≳ 100 which is at least a factor of 10 times better than other shape measurement methods. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0802.1528}, -author = {Kitching, T. D. and Miller, L. and Heymans, C. E. and {Van Waerbeke}, L. and Heavens, A. F.}, -doi = {10.1111/j.1365-2966.2008.13628.x}, -eprint = {0802.1528}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kitching et al. - 2008 - Bayesian galaxy shape measurement for weak lensing surveys - II. Application to simulations.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observation,Gravitational lensing,Methods: data analysis,Methods: numerical,Methods: statistical}, -number = {1}, -pages = {149--167}, -title = {{Bayesian galaxy shape measurement for weak lensing surveys - II. Application to simulations}}, -volume = {390}, -year = {2008} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N. J. and Holland, A. D. and Gow, J. P. D. and Hall, D. J. and Tutt, James H. and Burt, D. and Endicott, J.}, -doi = {10.1117/12.926804}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2012 - Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps(2).pdf:pdf}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58" in the {\$}i{\$}-band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including a {\$}\backslashsim 10{\$} per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally, we check the sensitivity of our shear calibration estimates to other cuts made on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalog are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales (∼500 kpc) in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the virial radius of the haloes while describing the infalling matter via fluxes through a spherical shell; and we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP described for the first time in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one- and two-point statistics. The peripheral and advected momenta are correlated with the spin of the embedded halo at levels of 30 and 50 per cent. The infall takes place preferentially in the plane perpendicular to the direction defined by the spin of the halo. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be ∼15 per cent. The substructures have their spin orthogonal to their velocity vector in the rest frame of the halo at a level of about 5 per cent, suggestive of an image of a flow along filamentary structures, which provides an explanation for the measured anisotropy. Using a 'synthetic' stacked halo, it is shown that the positions and orientations of satellites relative to the direction of spin of the halo are not random even in projection. The average ellipticity of stacked haloes is 10 per cent, while the alignment excess in projection reaches 2 per cent. All measured correlations are fitted by a simple three-parameter model. We conclude that a halo does not see its environment as an Isotropic perturbation, we investigate how the anisotropy is propagated inwards using perturbation theory, and we discuss briefly the implications for weak lensing, warps and the thickness of galactic discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D and Pichon, C and Colombi, S}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Devour2017, -abstract = {Accurate measurement of galaxy structures is a prerequisite for quantitative investigation of galaxy properties or evolution. Yet, the impact of galaxy inclination and dust on commonly used metrics of galaxy structure is poorly quantified. We use infrared data sets to select inclination-independent samples of disc and flattened elliptical galaxies. These samples show strong variation in S$\backslash$'{\{}e{\}}rsic index, concentration, and half-light radii with inclination. We develop novel inclination-independent galaxy structures by collapsing the light distribution in the near-infrared on to the major axis, yielding inclination-independent `linear' measures of size and concentration. With these new metrics we select a sample of Milky Way analogue galaxies with similar stellar masses, star formation rates, sizes and concentrations. Optical luminosities, light distributions, and spectral properties are all found to vary strongly with inclination: When inclining to edge-on, {\$}r{\$}-band luminosities dim by {\$}{\textgreater}{\$}1 magnitude, sizes decrease by a factor of 2, `dust-corrected' estimates of star formation rate drop threefold, metallicities decrease by 0.1 dex, and edge-on galaxies are half as likely to be classified as star forming. These systematic effects should be accounted for in analyses of galaxy properties.}, -archivePrefix = {arXiv}, -arxivId = {1702.06528}, -author = {Devour, Brian and Bell, Eric}, -doi = {10.1093/mnrasl/slx021}, -eprint = {1702.06528}, -issn = {1745-3925}, -journal = {Mnras}, -keywords = {dust,extinction,galaxies,general,photometric,techniques}, -number = {February}, -pages = {1--5}, -pmid = {18462818}, -title = {{Revealing strong bias in common measures of galaxy properties using new inclination-independent structures}}, -url = {http://arxiv.org/abs/1702.06528%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnrasl/slx021}, -volume = {000}, -year = {2017} -} -@article{Hopkins2009, -abstract = {Transformation of disks into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in halos according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the over-production of spheroids: low and intermediate-mass galaxies are predicted to be bulge-dominated (B/T{\$\sim${}}0.5 at {\textless}10{\^{}}10 M{\_}sun), with almost no bulgeless systems), even if they have avoided major mergers. Including the different physical behavior of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T{\$\sim${}}0.1 at {\textless}10{\^{}}10 M{\_}sun, with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behavior of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests.}, -archivePrefix = {arXiv}, -arxivId = {0901.4111}, -author = {Hopkins, Philip F and Somerville, Rachel S and Cox, Thomas J and Hernquist, Lars and Jogee, Shardha and Kere{\v{s}}, Dusan and Ma, Chung Pei and Robertson, Brant and Stewart, Kyle}, -doi = {10.1111/j.1365-2966.2009.14983.x}, -eprint = {0901.4111}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Galaxies: spiral}, -number = {2}, -pages = {802--814}, -title = {{The effects of gas on morphological transformation in mergers: Implications for bulge and disc demographics}}, -volume = {397}, -year = {2009} -} -@article{Birrer2018, -abstract = {We present a blind time-delay strong lensing (TDSL) cosmographic analysis of the doubly imaged quasar SDSS 1206+4332. We combine the relative time delay between the quasar images, Hubble Space Telescope imaging, the Keck stellar velocity dispersion of the lensing galaxy, and wide-field photometric and spectroscopic data of the field to constrain two angular diameter distance relations. The combined analysis is performed by forward modelling the individual data sets through a Bayesian hierarchical framework, and it is kept blind until the very end to prevent experimenter bias. After unblinding, the inferred distances imply a Hubble constant $H_0 = 68.8^{+5.4}_{-5.1}$ kms$^{-1}$Mpc$^{-1}$, assuming a flat Lambda cold dark matter cosmology with uniform prior on $\Omega_{\rm m}$ in [0.05, 0.5]. The precision of our cosmographic measurement with the doubly imaged quasar SDSS 1206+4332 is comparable with those of quadruply imaged quasars and opens the path to perform on selected doubles the same analysis as anticipated for quads. Our analysis is based on a completely independent lensing code than our previous three H0LiCOW systems and the new measurement is fully consistent with those. We provide the analysis scripts paired with the publicly available software to facilitate independent analysis. The consistency between blind measurements with independent codes provides an important sanity check on lens modelling systematics. By combining the likelihoods of the four systems under the same prior, we obtain $H_0 = 72.5^{+2.1}_{-2.3}$kms$^{-1}$Mpc$^{-1}$. This measurement is independent of the distance ladder and other cosmological probes.}, -archivePrefix = {arXiv}, -arxivId = {1809.01274}, -author = {Birrer, S. and Treu, T. and Rusu, C. E. and Bonvin, V. and Fassnacht, C. D. and Chan, J. H.H. and Agnello, A. and Shajib, A. J. and Chen, G. C.F. and Auger, M. and Courbin, F. and Hilbert, S. and Sluse, D. and Suyu, S. H. and Wong, K. C. and Marshall, P. and Lemaux, B. C. and Meylan, G.}, -doi = {10.1093/mnras/stz200}, -eprint = {1809.01274}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Birrer et al. - 2019 - H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 12064332 and a new measurement of the Hub(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmological parameters,dark energy,ravitational lensing: strong}, -number = {4}, -pages = {4726--4753}, -title = {{H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant}}, -url = {http://arxiv.org/abs/1809.01274}, -volume = {484}, -year = {2019} -} -@article{Conselice1999, -abstract = {We present a detailed study of rotational asymmetry in galaxies for both morphological and physical diagnostic purposes. An unambiguous method for computing asymmetry is developed, robust for both distant and nearby galaxies. By degrading real galaxy images, we test the reliability of this asymmetry measure over a range of observational conditions, e.g. spatial resolution and signal-to-noise (S/N). Compared to previous methods, this new algorithm avoids the ambiguity associated with choosing a center by using a minimization method, and successfully corrects for variations in S/N. There is, however, a strong relationship between the rotational asymmetry and physical resolution (distance at fixed spatial resolution); objects become more symmetric when less well-resolved. We further investigate asymmetry as a function of galactic radius an rotation. We find the asymmetry index has a strong radial dependence that differs vastly between Hubble types. As a result, a meaningful asymmetry index must be specified within a well-defined radius representative of the physical galaxy scale. We enumerate several viable alternatives, which excludes the use of isophotes. Asymmetry as a function of angle (A[phi]) is also a useful indicator of ellipticity and higher-order azimuthal structure. In general, we show the power of asymmetry as a morphological parameter lies in the strong correlation with (B-V) color for galaxies undergoing normal star formation, spanning all Hubble types from ellipticals to irregular galaxies. Interacting galaxies do not fall on this asymmetry-color ``fiducial sequence,'' as these galaxies are too asymmetric for their color. We propose to use this fact to distinguish between `normal' galaxies and galaxies undergoing an interaction or merger at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9907399}, -author = {Conselice, Christopher J and Bershady, Matthew A and Jangren, Anna}, -doi = {10.1086/308300}, -eprint = {9907399}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {GALAXIES: PHOTOMETRY,GALAXIES: STRUCTURE,Galaxies: Photometry,Galaxies: Structure}, -month = {feb}, -number = {2}, -pages = {886--910}, -primaryClass = {astro-ph}, -title = {{The Asymmetry of Galaxies: Physical Morphology for Nearby and High Redshift Galaxies}}, -url = {http://arxiv.org/abs/astro-ph/9907399%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/308300}, -volume = {529}, -year = {1999} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kilo parsecs. These stellar halos provide a fossil record of galaxy assembly histories. Using data that is both wide ({\$\sim${}}100 square degree) and deep (i{\textgreater}28.5 mag/arcsec{\^{}}2 in i-band), we present a systematic study of the stellar halos of a sample of more than 3000 galaxies at 0.3 {\textless}z {\textless}0.5 with {\$}\backslashbackslashlog M{\_}{\{}\backslashbackslashstar{\{}\backslash{\}}{\}}/M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}} {\textgreater}11.4{\$}. Our study is based on high-quality (0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP), which enables us to individually estimate surface mass density profiles to 100 kpc without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles. When this extended light is not properly accounted for as a result of shallow imaging or inadequate profile modeling, the derived stellar mass function can be significantly underestimated at the highest masses. Across our sample, the ellipticity of outer light profiles increases substantially as we probe larger radii. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass-dependence in outer color gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at late times from a series of merging events. We provide surface mass surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless}z {\textless}0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Greene2012, -abstract = {We use the Mitchell Spectrograph (formerly VIRUS-P) on the McDonald Observatory 2.7m Harlan J. Smith Telescope to search for the chemical signatures of massive elliptical galaxy assembly. The Mitchell Spectrograph is an integral-field spectrograph with a uniquely wide field of view (107x107 sq arcsec), allowing us to achieve remarkably high signal-to-noise ratios of {\$\sim${}}20-70 per pixel in radial bins of 2-2.5 times the effective radii of the eight galaxies in our sample. Focusing on a sample of massive elliptical galaxies with stellar velocity dispersions sigma* {\textgreater} 150 km/s, we study the radial dependence in the equivalent widths (EWs) of key metal absorption lines. By twice the effective radius, the Mgb EWs have dropped by {\$\sim${}}50{\%}, and only a weak correlation between sigma* and Mgb EW remains. The Mgb EWs at large radii are comparable to those seen in the centers of elliptical galaxies that are approximately an order of magnitude less massive. We find that the well-known metallicity gradients often observed within an effective radius continue smoothly to 2.5R{\_}e, while the abundance ratio gradients remain flat. Much like the halo of the Milky Way, the stellar halos of our galaxies have low metallicities and high alpha-abundance ratios, as expected for very old stars formed in small stellar systems. Our observations support a picture in which the outer parts of massive elliptical galaxies are built by the accretion of much smaller systems whose star formation history was truncated at early times.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{Savorgnan2015, -abstract = {The S$\backslash$'ersic {\$}R{\^{}}{\{}1/n{\}}{\$} model is the best approximation known to date for describing the light distribution of stellar spheroidal and disk components, with the S$\backslash$'ersic index {\$}n{\$} providing a direct measure of the central radial concentration of stars. The S$\backslash$'ersic index of a galaxy's spheroidal component, {\$}n{\_}{\{}sph{\}}{\$}, has been shown to tightly correlate with the mass of the central supermassive black hole, {\$}M{\_}{\{}BH{\}}{\$}. The {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} correlation is also expected from other two well known scaling relations involving the spheroid luminosity, {\$}L{\_}{\{}sph{\}}{\$}: the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and the {\$}M{\_}{\{}BH{\}}-L{\_}{\{}sph{\}}{\$}. Obtaining an accurate estimate of the spheroid S$\backslash$'ersic index requires a careful modelling of a galaxy's light distribution and some studies have failed to recover a statistically significant {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} correlation. With the aim of re-investigating the {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} and other black hole mass scaling relations, we performed a detailed (i.e.{\$\sim${}}bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, that had been imaged at {\$}3.6\backslashrm{\\sim{}}\backslashmu m{\$} with Spitzer. In this paper, the third of this series, we present an analysis of the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} diagrams. While early-type (elliptical+lenticular) and late-type (spiral) galaxies split into two separate relations in the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}-L{\_}{\{}sph{\}}{\$} diagrams, they reunite into a single {\$}M{\_}{\{}BH{\}} \backslashpropto n{\_}{\{}sph{\}}{\^{}}{\{}3.39 \backslashpm 0.15{\}}{\$} sequence with relatively small intrinsic scatter ({\$}\backslashepsilon \backslashsimeq 0.25 \backslashrm{\\sim{}}dex{\$}). The black hole mass appears to be closely related to the spheroid central concentration of stars, which mirrors the inner gradient of the spheroid gravitational potential.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1603.01910}, -author = {Savorgnan, Giulia A D}, -doi = {10.3847/0004-637X/821/2/88}, -eprint = {1603.01910}, -number = {2001}, -title = {{Supermassive black holes and their host spheroids III. The {\$}M{\_}{\{}BH{\}} - n{\_}{\{}sph{\}}{\$} correlation}}, -url = {http://arxiv.org/abs/1603.01910%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/821/2/88}, -year = {2016} -} -@article{Cappellari2012a, -abstract = {Much of our knowledge of galaxies comes from analysing the radiation emitted by their stars, which depends on the present number of each type of star in the galaxy. The present number depends on the stellar initial mass function (IMF), which describes the distribution of stellar masses when the population formed, and knowledge of it is critical to almost every aspect of galaxy evolution. More than 50 years after the first IMF determination, no consensus has emerged on whether it is universal among different types of galaxies. Previous studies indicated that the IMF and the dark matter fraction in galaxy centres cannot both be universal, but they could not convincingly discriminate between the two possibilities. Only recently were indications found that massive elliptical galaxies may not have the same IMF as the Milky Way. Here we report a study of the two-dimensional stellar kinematics for the large representative ATLAS 3D sample of nearby early-type galaxies spanning two orders of magnitude in stellar mass, using detailed dynamical models. We find a strong systematic variation in IMF in early-type galaxies as a function of their stellar mass-to-light ratios, producing differences of a factor of up to three in galactic stellar mass. This implies that a galaxy's IMF depends intimately on the galaxy's formation history. {\textcopyright} 2012 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.3308}, -author = {Cappellari, Michele and McDermid, Richard M. and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Crocker, Alison F. and Davies, Roger L. and Davis, Timothy A. and {De Zeeuw}, P. T. and Duc, Pierre Alain and Emsellem, Eric and Khochfar, Sadegh and Krajnovi{\"{a}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1038/nature10972}, -eprint = {1202.3308}, -file = {:C\:/Users/Jammy/Documents/Papers/IFUs/Cappellari2012IMFATLAS3d.pdf:pdf}, -issn = {00280836}, -journal = {Nature}, -number = {7395}, -pages = {485--488}, -pmid = {22538610}, -title = {{Systematic variation of the stellar initial mass function in early-type galaxies}}, -volume = {484}, -year = {2012} -} -@article{Sonnenfeld2021a, -abstract = {Context. Time-delay lensing is a powerful tool for measuring the Hubble constant H 0 . However, in order to obtain an accurate estimate of H 0 from a sample of time-delay lenses, very good knowledge of the mass structure of the lens galaxies is needed. Strong lensing data on their own are not sufficient to break the degeneracy between H 0 and the lens model parameters on a single object basis. Aims. The goal of this study is to determine whether it is possible to break the H 0 -lens structure degeneracy with the statistical combination of a large sample of time-delay lenses, relying purely on strong lensing data with no stellar kinematics information. Methods. I simulated a set of 100 lenses with doubly imaged quasars and related time-delay measurements. I fitted these data with a Bayesian hierarchical method and a flexible model for the lens population, emulating the lens modelling step. Results. The sample of 100 lenses on its own provides a measurement of H 0 with 3% precision, but with a −4% bias. However, the addition of prior information on the lens structural parameters from a large sample of lenses with no time delays, such as that considered in Paper I, allows for a 1% level inference. Moreover, the 100 lenses allow for a 0.03 dex calibration of galaxy stellar masses, regardless of the level of prior knowledge of the Hubble constant. Conclusions. Breaking the H 0 -lens model degeneracy with lensing data alone is possible, but 1% measurements of H 0 require either many more than 100 time-delay lenses or knowledge of the structural parameter distribution of the lens population from a separate sample of lenses.}, -author = {Sonnenfeld, Alessandro}, -doi = {10.1051/0004-6361/202142062}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnenfeld2021StatsI.pdf:pdf}, -issn = {0004-6361}, -journal = {A\&A}, -keywords = {fundamental parameters,galaxies,gravitational lensing,strong}, -pages = {A18}, -title = {{Statistical strong lensing I. Constraints on the inner structure of galaxies from samples of a thousand lenses}}, -volume = {651}, -year = {2021} -} -@techreport{Chiaberge2009, -author = {Chiaberge, M and Lim, P.$\sim$L. and Kozhurina-Platais, V and Sirianni, M and Mack, J}, -booktitle = {Instrument Science Report ACS 2009-01, 26 pages}, -keywords = {ACS,Advanced Camera for Surveys,HST,Hubble Space Telescope,Space Telescope Science Institute}, -month = {apr}, -title = {{Updated CTE photometric correction for WFC and HRC}}, -year = {2009} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@inproceedings{MartinNavarro2013, -author = {Mart$\backslash$'$\backslash$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Geometryeg, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Brainerd2005, -abstract = {The distribution of satellite galaxies relative to isolated host galaxies in the Sloan Digital Sky Survey (SDSS) is investigated. Host-satellite systems are selected using three different methods, yielding samples of {\$\sim${}}3300, {\$\sim${}}1600, and {\$\sim${}}950 satellites. In the plane of the sky, the distributions of all three samples show highly significant deviations from circular symmetry ({\textgreater}99.99{\%}, {\textgreater}99.99{\%}, and 99.79{\%} confidence levels, respectively), and the degree of anisotropy is a strong function of the projected radius, r p , at which the satellites are found. For r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 100 kpc, the SDSS satellites are aligned preferentially with the major axes of the hosts. This is in stark contrast to the Holmberg effect, in which satellites are aligned with the minor axes of host galaxies. The degree of anisotropy in the distribution of the SDSS satellites decreases with r p and is consistent with an isotropic distribution at of order the 1 $\sigma$ level for 250 kpc {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 500 kpc.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408559}, -author = {Brainerd, Tereasa G}, -doi = {10.1086/432713}, -eprint = {0408559}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L101----L104}, -primaryClass = {astro-ph}, -title = {{Anisotropic Distribution of SDSS Satellite Galaxies: Planar (Not Polar) Alignment}}, -url = {http://stacks.iop.org/1538-4357/628/i=2/a=L101}, -volume = {628}, -year = {2005} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd (2005), but inconsistent with several previous studies who detected a preferential minor axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Ferrero2017, -abstract = {The Tully-Fisher relation (TFR) links the stellar mass of a disc galaxy, Mstr, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling (M ∝ V3) of dark matter haloes, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to deviate substantially from a single power law and to evolve rapidly with redshift. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of $\Lambda$ cold dark matter ($\Lambda$CDM) cosmological simulations. Matching both relations requires disc sizes to satisfy constraints given by the concentration of haloes and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. $\Lambda$CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1607.03100}, -author = {Ferrero, Ismael and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw2691}, -eprint = {1607.03100}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {4}, -pages = {4736--4746}, -title = {{Size matters: Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE}}, -volume = {464}, -year = {2017} -} -@article{Smith2014, -abstract = {We use 10 387 galaxies from the Herschel Astrophysical TeraHertz Large Area Survey (HATLAS) to probe the far-infrared radio correlation (FIRC) of star-forming galaxies as a function of redshift, wavelength, and effective dust temperature. All of the sources in our 250 $\mu$m-selected sample have spectroscopic redshifts, as well as 1.4 GHz flux density estimates measured from the Faint Images of the Radio Sky at Twenty centimetres (FIRST) survey. This enables us to study not only individual sources, but also the average properties of the 250 $\mu$m-selected population using median stacking techniques.We find that individual sources detected at ≥5$\sigma$ in both the H-ATLAS and FIRST data have logarithmic flux ratios (i.e. FIRC q$\lambda$ parameters) consistent with previous studies of the FIRC. In contrast, the stacked values show larger q$\lambda$, suggesting excess far-IR flux density/luminosity in 250 $\mu$m-selected sources above what has been seen in previous analyses. In addition, we find evidence that 250 $\mu$m sources with warm dust spectral energy distributions have a larger 1.4 GHz luminosity than the cooler sources in our sample. Though we find no evidence for redshift evolution of the monochromatic FIRC, our analysis reveals significant temperature dependence. Whilst the FIRC is reasonably constant with temperature at 100 $\mu$m, we find increasing inverse correlation with temperature as we probe longer PACS and SPIRE wavelengths. These results may have important implications for the use of monochromatic dust luminosity as a star formation rate indicator in star-forming galaxies, and in the future, for using radio data to determine galaxy star formation rates.}, -archivePrefix = {arXiv}, -arxivId = {1409.2499}, -author = {Smith, D. J.B. and Jarvis, M. J. and Hardcastle, M. J. and Vaccari, M. and Bourne, N. and Dunne, L. and Ibar, E. and Maddox, N. and Prescott, M. and Vlahakis, C. and Eales, S. and Maddox, S. J. and Smith, M. W.L. and Valiante, E. and de Zotti, G.}, -doi = {10.1093/mnras/stu1830}, -eprint = {1409.2499}, -isbn = {00358711}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Infrared: ISM,Infrared: galaxies,Radio continuum: galaxies}, -number = {3}, -pages = {2232--2243}, -title = {{The temperature dependence of the far-infrared-radio correlation in the Herschel-ATLAS}}, -volume = {445}, -year = {2014} -} -@article{Milosavljevic2001, -abstract = {We investigate a model in which galactic nuclei form via the coalescence of preexisting stellar systems containing supermassive black holes. Merger simulations are carried out using N-body algorithms that can follow the formation and decay of a black hole binary and its effect on the surrounding stars down to subparsec scales. Our initial stellar systems have steep central density cusps similar to those in low-luminosity elliptical galaxies. Immediately following the merger, the density profile of the remnant is homologous with the initial density profile and the steep nuclear cusp is preserved. However, the formation of a black hole binary transfers energy to the stars and lowers the central density; continued decay of the binary creates a $\rho$$\sim$r-1 density cusp similar to those observed in bright elliptical galaxies, with a break radius that extends well beyond the sphere of gravitational influence of the black holes. Our simulations are the first to successfully produce shallow power-law cusps from mergers of galaxies with steep cusps, and our results support a picture in which the observed dependence of nuclear cusp slope on galaxy luminosity is a consequence of galaxy interactions. We follow the decay of the black hole binary over a factor of $\sim$20 in separation after formation of a hard binary, considerably farther than in previous simulations. We see almost no dependence of the binary's decay rate on number of particles in the simulation, contrary to earlier studies in which a lower initial density of stars led to a more rapid depletion of the binary's loss cone. We nevertheless argue that the decay of a black hole binary in a real galaxy would be expected to stall at separations of 0.01-1 pc unless some additional mechanism is able to extract energy from the binary. We discuss the implications of our results for the survivability of dark matter cusps.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0103350v1}, -author = {Milosavljevi{\'{c}}, Milo{\v{s}} and Merritt, David}, -doi = {10.1086/323830}, -eprint = {0103350v1}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Black Hole Physics,Galaxies: Nuclei,Stellar Dynamics}, -month = {dec}, -number = {1}, -pages = {34--62}, -primaryClass = {arXiv:astro-ph}, -title = {{Formation of Galactic Nuclei}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ApJ...563...34M&link_type=ABSTRACT%5Cnpapers3://publication/doi/10.1086/323830}, -volume = {563}, -year = {2001} -} -@article{Wardlow2013, -author = {Wardlow, Julie and Cooray, A and Bernardis, F De and Amblard, A and Arumugam, V and Aussel, H and Baker, A and Bethermin, M and Blundell, R and Bock, J and Boselli, A}, -journal = {ApJ}, -pages = {59}, -title = {{Herschel HerMES: Gravitationally Lensed Galaxies and Lensing Statistics at Submillimeter Wavelengths}}, -volume = {762}, -year = {2013} -} -@article{Murray2013, -abstract = {A multi-level clocking scheme has been developed to improve the parallel CTE of four-phase CCDs by suppressing the effects of traps located in the transport channel under barrier phases by inverting one of these phases throughout the transfer sequence. In parallel it was apparent that persistence following optical overload in Euclid VIS detectors would lead to undesirable signal released in subsequent rows and frames and that a suitable scheme for flushing this signal would be required. With care, the negatively biased electrodes during the multi-level transfer sequence can be made to pin the entire surface, row-by-row, and annihilate the problematic charges. This process can also be extended for use during integration to significantly reduce the unusable area of the detector, as per the clocked anti-blooming techniques developed many years ago; however, with the four-phase electrodes architecture of modern CCDs, we can take precautionary measures to avoid the problem of charge pumping and clock induced charge within the science frames. Clock induced charge is not all bad! We also propose the use of on-orbit trap-pumping for Euclid VIS to provide calibration input to ground based correction algorithms and as such a uniform, low noise background is require. Clock induced charge can be manipulated to provide a very suitable, low signal and noise background to the imaging array. Here we describe and present results of multi-level parallel clocking schemes for use in four-phase CCDs that could improve performance of high precision astronomy applications such as Euclid VIS. ? 2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Holland, Andrew D and Stefanov, Konstantin D and Gow, Jason P D and MacCormick, Calum and Dryer, Ben J and Allanwood, Edgar A H}, -doi = {10.1117/12.2024839}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {Blooming,CAB,CCD,CIC,CTE,Euclid VIS,Mu,[BFW}, -pages = {88600K}, -title = {{Multi-level parallel clocking of CCDs for: improving charge transfer efficiency, clearing persistence, clocked anti-blooming, and generating low-noise backgrounds for pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024839}, -volume = {8860}, -year = {2013} -} -@article{Walcher2011, -abstract = {Fitting the spectral energy distributions (SEDs) of galaxies is an almost universally used technique that has matured significantly in the last decade. Model predictions and fitting procedures have improved significantly over this time, attempting to keep up with the vastly increased volume and quality of available data. We review here the field of SED fitting, describing the modelling of ultraviolet to infrared galaxy SEDs, the creation of multiwavelength data sets, and the methods used to fit model SEDs to observed galaxy data sets. We touch upon the achievements and challenges in the major ingredients of SED fitting, with a special emphasis on describing the interplay between the quality of the available data, the quality of the available models, and the best fitting technique to use in order to obtain a realistic measurement as well as realistic uncertainties. We conclude that SED fitting can be used effectively to derive a range of physical properties of galaxies, such as redshift, stellar masses, star formation rates, dust masses, and metallicities, with care taken not to over-interpret the available data. Yet there still exist many issues such as estimating the age of the oldest stars in a galaxy, finer details ofdust properties and dust-star geometry, and the influences of poorly understood, luminous stellar types and phases. The challenge for the coming years will be to improve both the models and the observational data sets to resolve these uncertainties. The present review will be made available on an interactive, moderated web page (sedfitting.org), where the community can access and change the text. The intention is to expand the text and keep it up to date over the coming years.}, -archivePrefix = {arXiv}, -arxivId = {1008.0395}, -author = {Walcher, Jakob and Groves, Brent and Budav{\'{a}}ri, Tam{\'{a}}s and Dale, Daniel}, -doi = {10.1007/s10509-010-0458-z}, -eprint = {1008.0395}, -isbn = {0-7803-8416-4}, -issn = {0004640X}, -journal = {Astrophysics and Space Science}, -keywords = {Galaxies: ISM,Galaxies: stellar content,Methods: data analysis,Radiation mechanisms: general,Techniques: photometric,Techniques: spectroscopic}, -month = {jan}, -number = {1}, -pages = {1--51}, -pmid = {21278243}, -title = {{Fitting the integrated spectral energy distributions of galaxies}}, -volume = {331}, -year = {2010} -} -@article{Hopkins2010c, -abstract = {We present a simple estimate of the mass 'deficits' in cored spheroids, as a function of galaxy mass and radius within the galaxy. Previous attempts to measure such deficits depended on fitting some functional form to the profile at large radii extrapolating inwards; this is sensitive to the assumed functional form and does not allow for variation in nuclear profile shapes. For example, we show that literally interpreting the residuals from a single/cored Sersic function fit as implied 'deficit' can be misleading. Instead, we take advantage of larger data sets to directly construct stellar mass profiles of observed systems and measure the stellar mass enclosed in a series of physical radii (M*({\textless} R)), for samples of cusp and core spheroids at the same stellar mass. We show that there is a significant (model-independent) bimodality in this distribution of central structure for this sample at small radii. We non-parametrically measure the median offset between core and cusp populations (the 'deficit'$\Delta$M*({\textless} R)). We can then construct the scoured mass profile as a function of radius, without reference to any assumed functional form. The mass deficit rises in power-law fashion ($\Delta$M*({\textless} R) ∝R1.3-1.8) from a significant but small mass at R≲ 10 pc, to asymptote to a maximum ∼ 0.5-2 MBH at ∼ 100 pc, where MBH is the mass of the central, supermassive black hole (BH) hosted by the spheroid. At larger radii there is no statistically significant separation between populations; the upper limit to the cumulative scoured mass at ∼kpc is ∼ 2-4 MBH. This does not depend strongly on stellar mass. The dispersion in M*({\textless} R) appears larger in the core population, possibly reflecting the fact that core scouring increases the scatter in central profile shapes. We measure this broadening effect as a function of radius. The relatively low mass deficits inferred, and characteristic radii, are in good agreement with models of 'scouring' from BH binary systems. {\textcopyright}2010 The Authors. Journal compilation {\textcopyright}2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1006.0488}, -author = {Hopkins, Philip F and Hernquist, Lars}, -doi = {10.1111/j.1365-2966.2010.16915.x}, -eprint = {1006.0488}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {447--457}, -title = {{A non-parametric estimate of mass 'scoured' in galaxy cores}}, -url = {http://arxiv.org/abs/1006.0488%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2010.16915.x}, -volume = {407}, -year = {2010} -} -@article{Yan2016a, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R{\$\sim${}}2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is {\$\sim${}}73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R and Bershady, Matthew A and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R and Thomas, Daniel and Wake, David A and Weijmans, Anne-Marie and Westfall, Kyle B and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A and Blanton, Michael R and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T and Goddard, Daniel and Gunn, James E and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R and Oravetz, Daniel and Pan, Kaike and Parejko, John K and Sanchez, Sebastian F and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {6}, -pages = {197}, -title = {{SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY}}, -url = {http://arxiv.org/abs/1607.08613%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {152}, -year = {2016} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10% of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1138?key=crossref.6ebb2a01dc7b45f1fa5c66089a37542b}, -volume = {709}, -year = {2010} -} -@article{Holl2012, -abstract = {Gaia, the next astrometric mission of the European Space Agency, will use a camera composed of 106 CCDs to collect multiple observations for one billion stars. The astrometric core solution of Gaia will use the estimated location of the stellar images on the CCDs to derive the astrometric parameters (position, parallax and proper motion) of the stars. The Gaia CCDs will suffer from charge transfer inefficiency (CTI) mainly caused by radiation damage. CTI is expected to significantly degrade the quality of the collected images which ultimately affects the astrometric accuracy of Gaia. This paper is the second and last in a study aiming at characterizing and quantifying the impact of CCD radiation damage on Gaia astrometry. Here we focus on the effect of the image location errors induced by CTI on the astrometric solution. We apply the Gaia Astrometric Global Iterative Solution (AGIS) to simulated Gaia-like observations for 1 million stars including CTI-induced errors as described in the first paper. We show that a magnitude-dependent image location bias is propagated in the astrometric solution, biasing the estimation of the astrometric parameters as well as decreasing its precision. We demonstrate how the Gaia scanning law dictates this propagation and the ultimate sky distribution of the CTI-induced errors. The possibility of using the residuals of the astrometric solution to improve the calibration of the CTI effects is investigated. We also estimate the astrometric errors caused by (faint) disturbing stars preceding the stellar measurements on the CCDs. Finally, we show that, for single stars, the overall astrometric accuracy of Gaia can be preserved to within 10per cent of the CTI-free case for all magnitudes by appropriate modelling at the image location estimation level and using the solution residuals. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.1547}, -author = {Holl, B. and Prod'homme, T. and Lindegren, L. and Brown, A. G.A.}, -doi = {10.1111/j.1365-2966.2012.20429.x}, -eprint = {1110.1547}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Holl et al. - 2012 - The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solu.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: numerical,Space vehicles}, -number = {4}, -pages = {2786--2807}, -title = {{The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solution}}, -volume = {422}, -year = {2012} -} -@article{Wertz2018, -abstract = {Modern time-delay cosmography aims to infer the cosmological parameters with a competitive precision from observing a multiply imaged quasar. The success of this technique relies upon a robust modeling of the lens mass distribution. Unfortunately strong degeneracies between density profiles that lead to almost the same lensing observables may bias precise estimates of the Hubble constant. The source position transformation (SPT), which covers the well-known mass-sheet transformation (MST) as a special case, defines a new framework to investigate these degeneracies. In this paper, we present pySPT, a python package dedicated to the SPT. We describe how it can be used to evaluate the impact of the SPT on lensing observables. We review most of its capabilities and elaborate on key features that we used in a companion paper regarding SPT and time delays. The pySPT program also comes with a subpackage dedicated to simple lens modeling. This can be used to generate lensing related quantities for a wide variety of lens models independent of any SPT analysis. As a first practical application, we present a correction to the first estimate of the impact on time delays of the SPT, which has been experimentally found in a previous work between a softened power law and composite (baryons + dark matter) lenses. We find that the large deviations previously predicted have been overestimated because of a minor bug in the public lens modeling code lensmodel (v1.99), which is now fixed. We conclude that the predictions for the Hubble constant deviate by ∼7{\%}, first and foremost as a consequence of an MST. The latest version of pySPT is available on Github, a software development platform, along with some tutorials to describe in detail how making the best use of pySPT.}, -archivePrefix = {arXiv}, -arxivId = {1801.04151}, -author = {Wertz, Olivier and Orthen, Bastian}, -doi = {10.1051/0004-6361/201732242}, -eprint = {1801.04151}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Cosmological parameters,Gravitational lensing: Strong}, -pages = {1--9}, -title = {{A dedicated source-position transformation package: PySPT}}, -url = {http://arxiv.org/abs/1801.04151%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201732242}, -volume = {619}, -year = {2018} -} -@article{York2000, -abstract = {The Sloan Digital Sky Survey (SDSS) will provide the data to support detailed investigations of the distribution of luminous and non- luminous matter in the Universe: a photometrically and astrometrically calibrated digital imaging survey of pi steradians above about Galactic latitude 30 degrees in five broad optical bands to a depth of g' about 23 magnitudes, and a spectroscopic survey of the approximately one million brightest galaxies and 10^5 brightest quasars found in the photometric object catalog produced by the imaging survey. This paper summarizes the observational parameters and data products of the SDSS, and serves as an introduction to extensive technical on-line documentation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0006396}, -author = {York, Donald G. and Adelman, J. and {Anderson, Jr.}, John E. and Anderson, Scott F. and Annis, James and Bahcall, Neta A. and Bakken, J. A. and Barkhouser, Robert and Bastian, Steven and Berman, Eileen and Boroski, William N. and Bracker, Steve and Briegel, Charlie and Briggs, John W. and Brinkmann, J. and Brunner, Robert and Burles, Scott and Carey, Larry and Carr, Michael A. and Castander, Francisco J. and Chen, Bing and Colestock, Patrick L. and Connolly, A. J. and Crocker, J. H. and Csabai, Istv{\'{a}}n and Czarapata, Paul C. and Davis, John Eric and Doi, Mamoru and Dombeck, Tom and Eisenstein, Daniel and Ellman, Nancy and Elms, Brian R. and Evans, Michael L. and Fan, Xiaohui and Federwitz, Glenn R. and Fiscelli, Larry and Friedman, Scott and Frieman, Joshua A. and Fukugita, Masataka and Gillespie, Bruce and Gunn, James E. and Gurbani, Vijay K. and de Haas, Ernst and Haldeman, Merle and Harris, Frederick H. and Hayes, J. and Heckman, Timothy M. and Hennessy, G. S. and Hindsley, Robert B. and Holm, Scott and Holmgren, Donald J. and Huang, Chi-hao and Hull, Charles and Husby, Don and Ichikawa, Shin-Ichi and Ichikawa, Takashi and Ivezi{\'{c}}, {\v{Z}}eljko and Kent, Stephen and Kim, Rita S. J. and Kinney, E. and Klaene, Mark and Kleinman, A. N. and Kleinman, S. and Knapp, G. R. and Korienek, John and Kron, Richard G. and Kunszt, Peter Z. and Lamb, D. Q. and Lee, B. and Leger, R. French and Limmongkol, Siriluk and Lindenmeyer, Carl and Long, Daniel C. and Loomis, Craig and Loveday, Jon and Lucinio, Rich and Lupton, Robert H. and MacKinnon, Bryan and Mannery, Edward J. and Mantsch, P. M. and Margon, Bruce and McGehee, Peregrine and McKay, Timothy A. and Meiksin, Avery and Merelli, Aronne and Monet, David G. and Munn, Jeffrey A. and Narayanan, Vijay K. and Nash, Thomas and Neilsen, Eric and Neswold, Rich and Newberg, Heidi Jo and Nichol, R. C. and Nicinski, Tom and Nonino, Mario and Okada, Norio and Okamura, Sadanori and Ostriker, Jeremiah P. and Owen, Russell and Pauls, A. George and Peoples, John and Peterson, R. L. and Petravick, Donald and Pier, Jeffrey R. and Pope, Adrian and Pordes, Ruth and Prosapio, Angela and Rechenmacher, Ron and Quinn, Thomas R. and Richards, Gordon T. and Richmond, Michael W. and Rivetta, Claudio H. and Rockosi, Constance M. and Ruthmansdorfer, Kurt and Sandford, Dale and Schlegel, David J. and Schneider, Donald P. and Sekiguchi, Maki and Sergey, Gary and Shimasaku, Kazuhiro and Siegmund, Walter A. and Smee, Stephen and Smith, J. Allyn and Snedden, S. and Stone, R. and Stoughton, Chris and Strauss, Michael A. and Stubbs, Christopher and SubbaRao, Mark and Szalay, Alexander S. and Szapudi, Istvan and Szokoly, Gyula P. and Thakar, Anirudda R. and Tremonti, Christy and Tucker, Douglas L. and Uomoto, Alan and {Vanden Berk}, Dan and Vogeley, Michael S. and Waddell, Patrick and Wang, Shu-i and Watanabe, Masaru and Weinberg, David H. and Yanny, Brian and Yasuda, Naoki}, -doi = {10.1086/301513}, -eprint = {0006396}, -isbn = {00046256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {Cosmology: Observations,Instrumentation: Miscellaneous}, -month = {sep}, -number = {3}, -pages = {1579--1587}, -pmid = {17729145}, -primaryClass = {astro-ph}, -title = {{The Sloan Digital Sky Survey: Technical Summary}}, -url = {http://arxiv.org/abs/astro-ph/0006396%0Ahttp://dx.doi.org/10.1086/301513}, -volume = {120}, -year = {2000} -} -@article{Marinoni2016, -abstract = {We present the results of the short-term constancy monitoring of candidate GaiaSpectrophotometric Standard Stars (SPSS). We obtained time series of typically 1.24 h - with sampling periods from 1-3 min to a few hours, depending on the case - to monitor the constancy of our candidate SPSS down to 10 mmag, as required for the calibration of Gaia photometric data. We monitored 162 out of a total of 212 SPSS candidates. The observing campaign started in 2006 and finished in 2015, using 143 observing nights on nine different instruments covering both hemispheres. Using differential photometry techniques, we built light curves with a typical precision of 4 mmag, depending on the data quality. As a result of our constancy assessment, 150 SPSS candidates were validated against short-term variability, and only 12 were rejected because of variability including some widely used flux standards such as BD+174708, SA 105-448, 1740346, and HD 37725.}, -archivePrefix = {arXiv}, -arxivId = {1608.00759}, -author = {Marinoni, S. and Pancino, E. and Altavilla, G. and Bellazzini, M. and Galleti, S. and Tessicini, G. and Valentini, G. and Cocozza, G. and Ragaini, S. and Braga, V. and Bragaglia, A. and Federici, L. and Schuster, W. J. and Carrasco, J. M. and Castro, A. and Figueras, F. and Jordi, C.}, -doi = {10.1093/mnras/stw1886}, -eprint = {1608.00759}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Marinoni et al. - 2016 - The Gaia spectrophotometric standard stars survey - III. Short-term variability monitoring.pdf:pdf}, -isbn = {9788578110796}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Binaries: general,Stars: variables: general,Techniques: photometric}, -number = {4}, -pages = {3616--3627}, -pmid = {25246403}, -title = {{The Gaia spectrophotometric standard stars survey - III. Short-term variability monitoring}}, -url = {http://arxiv.org/abs/1608.00759%5Cnhttp://dx.doi.org/10.1093/mnras/stw1886}, -volume = {462}, -year = {2016} -} -@article{Li2018a, -abstract = {We investigate the discrepancy between the two-dimensional projected lensing mass and the dynam- ical mass for an ensemble of 97 strong gravitational lensing systems discovered by the Sloan Lens ACS (SLACS) Survey, the BOSS Emission-Line Lens Survey (BELLS), and the BELLS for GALaxy-Ly{\{}{\$}\backslash{\$}alpha{\}} EmitteR sYs- tems (BELLS GALLERY) Survey. We fit the lensing data to obtain the Einstein mass, and use the velocity dispersion of the lensing galaxies provided by the Sloan Digital Sky Survey (SDSS) to get the projected dynamical mass within the Einstein radius by assuming the power-law mass approximation. The discrepancy is found to be obvious and quantified by Bayesian analysis. For the singular isothermal sphere (SIS) mass model, we obtain that the Einstein mass is 20.7{\%} more than the dynamical mass, and the discrepancy increases with the redshift of the lensing galaxies. For more general power-law mass model, the discrepancy still exists within 1{\{}{\$}\backslash{\$}sigma{\}} credible region. The main reason of the the discrepancy could be mass contamination, including all invisible masses along the line of sight. In addition, the measurement errors and the approximation of the mass models could lead to part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1803.00819}, -author = {Li, Rui and Wang, Jiancheng and Shu, Yiping and Xu, Zhaoyi}, -doi = {10.3847/1538-4357/aaab50}, -eprint = {1803.00819}, -issn = {15384357}, -number = {2010}, -title = {{The discrepancy between Einstein mass and dynamical mass for SIS and power-law mass models}}, -url = {http://arxiv.org/abs/1803.00819%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaab50}, -year = {2018} -} -@article{Lovell2014, -abstract = {Well-motivated elementary particle candidates for the dark matter, such as the sterile neutrino, behave as warm dark matter (WDM). For particle masses of the order of a keV, free streaming produces a cutoffin the linear fluctuation power spectrum at a scale corresponding to dwarf galaxies. We investigate the abundance and structure of WDM haloes and subhaloes on these scales using high resolution cosmological N-body simulations of galactic haloes of mass similar to the Milky Way's. On scales larger than the free-streaming cutoff, the initial conditions have the same power spectrum and phases as one of the colddark matter (CDM) haloes previously simulated by Springel et al. as part of the Virgo consortium Aquarius project. We have simulated four haloes with WDM particle masses in the range 1.5-2.3 keV and, for one case, we have carried out further simulations at varying resolution. N-body simulations in which the power spectrum cutoffis resolved areknown to undergo artificial fragmentation in filaments producing spurious clumps which, for small masses (<107 M⊙ in our case) outnumber genuine haloes. We have developed a robust algorithm to identify these spurious objects and remove them from our halo catalogues. We find that the WDM subhalo mass function is suppressed bywell over an order magnitude relative to the CDM case for masses <109 M⊙. Requiring that there should be at least as many subhaloes as there are observed satellites in the Milky Way leads to a conservative lower limit to the (thermal equivalent) WDM particle mass of ̃1.5 keV. WDM haloes and subhaloes have cuspy density distributions that are well described by Navarro-Frenk-White or Einasto profiles. Their central densities are lower for lower WDM particle masses and none of the models we have considered suffering from the too big to fail problem recently highlighted by Boylan-Kolchin et al. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1308.1399}, -author = {Lovell, Mark R. and Frenk, Carlos S. and Eke, Vincent R. and Jenkins, Adrian and Gao, Liang and Theuns, Tom}, -doi = {10.1093/mnras/stt2431}, -eprint = {1308.1399}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: Dwarf}, -number = {1}, -pages = {300--317}, -title = {{The properties of warm dark matter haloes}}, -volume = {439}, -year = {2014} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ {\textgreater} 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright}2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{James2018, -abstract = {We present the first spatially resolved rest-frame ultraviolet (UV) study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z = 2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each $\sim$4-8 kpc2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with C III] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. Themapped C III] emission shows distinct kinematical structure, with velocity offsets of $\sim$±50 km s-1 between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionization parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing in the range -200 ≲ v (km s-1) ≲ -50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star formation rates remain relatively constant ($\sim$8-16M⊙ yr-1), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced.We measure electron densities with a range of log (Ne)= 3.92-4.36 cm-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large-scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially resolved rest-frame UV studies expected with future observatories, such as James Webb Space Telescope.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L. and Auger, Matt and Pettini, Max and Stark, Daniel P. and Belokurov, V. and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Sanderson2009, -abstract = {We study the distribution of projected offsets between the cluster X-ray centroid and the brightest cluster galaxy (BCG) for 65 X-ray-selected clusters from the Local Cluster Substructure Survey, with a median redshift of z = 0.23. We find a clear correlation between X-ray/BCG projected offset and the logarithmic slope of the cluster gas density profile at 0.04r 500($\alpha$), implying that more dynamically disturbed clusters have weaker cool cores. Furthermore, there is a close correspondence between the activity of the BCG, in terms of detected H$\alpha$ and radio emission, and the X-ray/BCG offset, with the line-emitting galaxies all residing in clusters with X-ray/BCG offsets of ≤15 kpc. Of the BCGs with $\alpha$ < -0.85 and an offset <0.02r500, 96 per cent (23/24) have optical emission and 88 per cent (21/24) are radio active, while none has optical emission outside these criteria. We also study the cluster gas fraction (fgas) within r500 and find a significant correlation with X-ray/BCG projected offset. The mean fgas of the 'small offset' clusters (<0.02r 500) is 0.106 ± 0.005 ($\sigma$ = 0.03) compared to 0.145 ± 0.009 ($\sigma$ = 0.04) for those with an offset >0.02r 500, indicating that the total mass may be systematically underestimated in clusters with larger X-ray/BCG offsets. Our results imply a link between cool core strength and cluster dynamical state consistent with the view that cluster mergers can significantly perturb cool cores, and set new constraints on models of the evolution of the intracluster medium. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0906.1808}, -author = {Sanderson, Alastair J.R. and Edge, Alastair C. and Smith, Graham P.}, -doi = {10.1111/j.1365-2966.2009.15214.x}, -eprint = {0906.1808}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sanderson, Edge, Smith - 2009 - LoCuSS The connection between brightest cluster galaxy activity, gas cooling and dynamical disturbance o.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: Clusters: general,Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,X-rays: Galaxies: Clusters}, -number = {4}, -pages = {1698--1705}, -title = {{LoCuSS: The connection between brightest cluster galaxy activity, gas cooling and dynamical disturbance of X-ray cluster cores}}, -volume = {398}, -year = {2009} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani} and Caldwell, Nelson}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and \nspectroscopic ESA cornerstone mission, currently scheduled for launch in\nlate 2011. Its primary science drivers are the composition, formation\nand evolution of the Galaxy. Gaia will not achieve its scientific\nrequirements without detailed calibration and correction for radiation\ndamage. Microscopic models of Gaia's CCDs are being developed to\nsimulate the effect of radiation damage, charge trapping, which causes\ncharge transfer inefficiency. The key to calculating the probability of\na photoelectron being captured by a trap is the 3D electron density\nwithin each CCD pixel. However, this has not been physically modelled\nfor Gaia CCD pixels. In this paper, the first of a series, we motivate\nthe need for such specialised 3D device modelling and outline how its\nfuture results will fit into Gaia's overall radiation calibration\nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Seabroke, Holland, Cropper - 2008 - Modelling radiation damage to ESA's Gaia satellite CCDs.pdf:pdf}, -isbn = {9780819472311}, -issn = {0277-786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy III}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Devour2017, -abstract = {Accurate measurement of galaxy structures is a prerequisite for quantitative investigation of galaxy properties or evolution. Yet, the impact of galaxy inclination and dust on commonly used metrics of galaxy structure is poorly quantified. We use infrared data sets to select inclination-independent samples of disc and flattened elliptical galaxies. These samples show strong variation in S$\backslash$'{\{}e{\}}rsic index, concentration, and half-light radii with inclination. We develop novel inclination-independent galaxy structures by collapsing the light distribution in the near-infrared on to the major axis, yielding inclination-independent `linear' measures of size and concentration. With these new metrics we select a sample of Milky Way analogue galaxies with similar stellar masses, star formation rates, sizes and concentrations. Optical luminosities, light distributions, and spectral properties are all found to vary strongly with inclination: When inclining to edge-on, {\$}r{\$}-band luminosities dim by {\$}{\textgreater}{\$}1 magnitude, sizes decrease by a factor of 2, `dust-corrected' estimates of star formation rate drop threefold, metallicities decrease by 0.1 dex, and edge-on galaxies are half as likely to be classified as star forming. These systematic effects should be accounted for in analyses of galaxy properties.}, -archivePrefix = {arXiv}, -arxivId = {1702.06528}, -author = {Devour, Brian and Bell, Eric}, -doi = {10.1093/mnrasl/slx021}, -eprint = {1702.06528}, -issn = {1745-3925}, -journal = {Mnras}, -keywords = {dust,extinction,galaxies,general,photometric,techniques}, -number = {February}, -pages = {1--5}, -pmid = {18462818}, -title = {{Revealing strong bias in common measures of galaxy properties using new inclination-independent structures}}, -url = {http://arxiv.org/abs/1702.06528%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnrasl/slx021}, -volume = {000}, -year = {2017} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, {\$}\backslashsigma(R){\$}, for 85 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute {\$}K{\$}-band magnitude {\$}M{\_}K {\textless} -25.3{\$} mag, or stellar mass {\$}M{\_}* {\textgreater} 4 \backslashtimes 10{\^{}}{\{}11{\}} M{\_}\backslashodot{\$}, within 108 Mpc. Our wide-field 107" {\$}\backslashtimes{\$} 107" IFS data cover radii as large as 40 kpc, for which we quantify separately the inner ({\$}{\textless}5{\$} kpc) and outer logarithmic slopes {\$}\backslashgamma{\_}{\{}\backslashrm inner{\}}{\$} and {\$}\backslashgamma{\_}{\{}\backslashrm outer{\}}{\$} of {\$}\backslashsigma(R){\$}. While {\$}\backslashgamma{\_}{\{}\backslashrm inner{\}}{\$} is mostly negative, of the 61 galaxies with sufficient radial coverage to determine {\$}\backslashgamma{\_}{\{}\backslashrm outer{\}}{\$} we find 33{\%} to have rising outer dispersion profiles ({\$}\backslashgamma{\_}{\{}\backslashrm outer{\}} {\textgreater} 0.03{\$}), 13{\%} to be flat ({\$}-0.03 {\textless} \backslashgamma{\_}{\{}\backslashrm outer{\}} {\textless} 0.03{\$}), and 54{\%} to be falling. The fraction of galaxies with rising outer profiles increases with {\$}M{\_}*{\$} and in denser galaxy environment, with the 11 most massive galaxies in our sample all having flat or rising dispersion profiles. The strongest environmental correlation is with halo mass, but weaker correlations with large-scale density and local density also exist. The average {\$}\backslashgamma{\_}{\{}\backslashrm outer{\}}{\$} is similar for brightest group galaxies, satellites, and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis {\$}h{\_}4{\$}. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{Holl2012, -abstract = {Gaia, the next astrometric mission of the European Space Agency, will use a camera composed of 106 CCDs to collect multiple observations for one billion stars. The astrometric core solution of Gaia will use the estimated location of the stellar images on the CCDs to derive the astrometric parameters (position, parallax and proper motion) of the stars. The Gaia CCDs will suffer from charge transfer inefficiency (CTI) mainly caused by radiation damage. CTI is expected to significantly degrade the quality of the collected images which ultimately affects the astrometric accuracy of Gaia. This paper is the second and last in a study aiming at characterizing and quantifying the impact of CCD radiation damage on Gaia astrometry. Here we focus on the effect of the image location errors induced by CTI on the astrometric solution. We apply the Gaia Astrometric Global Iterative Solution (AGIS) to simulated Gaia-like observations for 1 million stars including CTI-induced errors as described in the first paper. We show that a magnitude-dependent image location bias is propagated in the astrometric solution, biasing the estimation of the astrometric parameters as well as decreasing its precision. We demonstrate how the Gaia scanning law dictates this propagation and the ultimate sky distribution of the CTI-induced errors. The possibility of using the residuals of the astrometric solution to improve the calibration of the CTI effects is investigated. We also estimate the astrometric errors caused by (faint) disturbing stars preceding the stellar measurements on the CCDs. Finally, we show that, for single stars, the overall astrometric accuracy of Gaia can be preserved to within 10per cent of the CTI-free case for all magnitudes by appropriate modelling at the image location estimation level and using the solution residuals. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.1547}, -author = {Holl, B. and Prod'homme, T. and Lindegren, L. and Brown, A. G.A.}, -doi = {10.1111/j.1365-2966.2012.20429.x}, -eprint = {1110.1547}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Holl et al. - 2012 - The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solu.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: numerical,Space vehicles}, -number = {4}, -pages = {2786--2807}, -title = {{The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solution}}, -volume = {422}, -year = {2012} -} -@article{Zehavi2017, -abstract = {We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -- halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto- and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.}, -archivePrefix = {arXiv}, -arxivId = {1706.07871}, -author = {Zehavi, Idit and Contreras, Sergio and Padilla, Nelson and Smith, Nicholas J. and Baugh, Carlton M. and Norberg, Peder}, -doi = {10.3847/1538-4357/aaa54a}, -eprint = {1706.07871}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Zehavi et al. - 2018 - The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {clustering,cosmology,evolution,galaxies,halos,large-scale structure of universe,statistics,theory}, -number = {1}, -pages = {84}, -title = {{The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos}}, -url = {http://arxiv.org/abs/1706.07871%0Ahttp://dx.doi.org/10.3847/1538-4357/aaa54a}, -volume = {853}, -year = {2018} -} -@article{Report2011, -abstract = {Modelling students' behaviour in relation to tuition fees is a complex task since students' 'talent' is not common knowledge. Students observe a private noisy signal of their abilities, while university receives noisy information based on the quantitative and qualitative data provided by university applicants. In this article, we add the heterogeneity of the population to this model: we assume that this heterogeneity means that the perception of skills among a part of the population is biased and underestimates the capabilities of its members to succeed in the higher education system. Our conclusions differ from those derived in the literature and show in particular that the optimal tuition fees for a given number of students are lower than those obtained for a homogeneous population. {\textcopyright}2013 Copyright Taylor and Francis Group, LLC.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Christensen2014, -abstract = {We present a detailed comparison between the photometric properties of the bulges of two simulated galaxies and those of a uniform sample of observed galaxies. This analysis shows that the simulated galaxies have bulges with realistic surface brightnesses for their sizes and magnitude. These two field disc galaxies have rotational velocities ̃100 km s-1 and were integrated to a redshift of zero in a fully cosmological $\delta$ cold dark matter context as part of high-resolution smoothed particle hydrodynamic simulations. We performed bulge- disc decompositions of the galaxies using artificial observations, in order to conduct a fair comparison to observations. We also dynamically decomposed the galaxies and compared the star formation histories of the bulges to those of the entire galaxies. These star formation histories showed that the bulges were primarily formed before z = 1 and during periods of rapid star formation. Both galaxies have large amounts of early star formation, which is likely related to the relatively high bulge-to-disc ratios also measured for them. Unlike almost all previous cosmological simulations, the realistically concentrated bulges of these galaxies do not lead to unphysically high rotational velocities, causing them to naturally lie along the observed Tully-Fisher relation. {\textcopyright}2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1402.2702}, -author = {Christensen, C R and Brooks, A M and Fisher, D B and Governato, F and McCleary, J and Quinn, T R and Shen, S and Wadsley, J}, -doi = {10.1093/mnrasl/slu020}, -eprint = {1402.2702}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Bulges,Formation,Galaxies,Methods,Numerical,Spiral,Structure}, -number = {1}, -pages = {1--6}, -title = {{Simulating disc galaxy bulges that are consistent with observed scaling relations}}, -volume = {440}, -year = {2014} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71 825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 {\textless}z {\textless}0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 per cent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1201.0763}, -author = {Lackner, C N and Gunn, J E}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -primaryClass = {astro-ph.CO}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data%7B%5C_%7Dquery?bibcode=2012arXiv1201.0763L%7B%5C&%7Dlink%7B%5C_%7Dtype=ABSTRACT%7B%5C%25%7D5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Yang2006, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637X/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -title = {{Supermassive black holes and their host spheroids II. The red and blue sequence in the {\$}M{\_}{\{}\backslashrm BH{\}} - M{\_}{\{}\backslashrm *,sph{\}}{\$} diagram}}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -year = {2015} -} -@article{2001er, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright} 2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F.}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Steinmetz, Navarro - 2002 - The hierarchical origin of galaxy morphologies.pdf:pdf}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{Goulding2016a, -abstract = {Studies of the physical properties of local elliptical galaxies (e.g., gas temperatures, halo masses, stellar kinematics) are shedding new light on galaxy formation. Here we present the hot X-ray gas properties of 33 early-type systems within the MASSIVE galaxy survey sample that have archival Chandra X-ray observations. Through careful X-ray spectral modeling, we derive X-ray luminosities (L{\_}X) and plasma temperatures (T{\_}gas) for the diffuse gas components in these galaxies. We combine the MASSIVE sample with 41 galaxies from the ATLAS{\^{}}3D survey to investigate the X-ray and optical properties of a statistically significant sample of nearby early-type galaxies across a wide-range of environments. We deduce that all early-type galaxies (independent of galaxy mass and rotational support) follow a universal scaling law such that L{\_}X{\$\sim${}}T{\_}gas{\^{}}4.5. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, the wide-scale environment does not contribute to the intrinsic scatter ({\$\sim${}}0.5dex) within the scaling relation. We further demonstrate that the scatter in L{\_}X around both K-band luminosity (L{\_}K) and the galaxy stellar velocity dispersion is primarily driven by T{\_}gas, with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the origin of the gas directly to either the stellar mass or the galaxy potential. Indeed, our data require a steeper relation between L{\_}X, L{\_}K, and sigma{\_}e than predicted by standard mass-loss models. Finally, we find a statistically significant correlation between sigma{\_}e and T{\_}gas, suggesting that T{\_}gas is set by the galaxy potential inside the optical effective radius. We conclude that within the inner-most 10-30kpc region, early-types maintain pressure-supported hot gas, with a minimum T{\_}gas set by the virial temperature, but the majority show evidence for some additional heating.}, -archivePrefix = {arXiv}, -arxivId = {1604.01764}, -author = {Goulding, Andy D and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Bogdan, Akos and Nyland, Kristina and Blakeslee, John P and McConnell, Nicholas J and Thomas, Jens}, -doi = {10.3847/0004-637X/826/2/167}, -eprint = {1604.01764}, -issn = {0004-637X}, -title = {{The MASSIVE Survey IV.: The X-ray halos of the most massive early-type galaxies in the nearby Universe}}, -url = {http://arxiv.org/abs/1604.01764%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/826/2/167}, -year = {2016} -} -@article{Tian2017, -abstract = {We study themass discrepancy-acceleration relation (MDAR) of 57 elliptical galaxies by their Einstein rings from the Sloan Lens ACS Survey (SLACS). The mass discrepancy between the lensing mass and the baryonic mass derived from population synthesis is larger when the acceleration of the elliptical galaxy lenses is smaller. TheMDAR is also related to surface mass density discrepancy. At the Einstein ring, these lenses belong to high-surface-mass density galaxies. Similarly, we find that the discrepancy between the lensing and stellar surface mass density is small. It is consistent with the recent discovery of dynamical surface mass density discrepancy in disc galaxies where the discrepancy is smaller when surface density is larger. We also find relativistic modified Newtonian dynamics (MOND) can naturally explain the MDAR and surface mass density discrepancy in 57 Einstein rings. Moreover, the lensing mass, the dynamical mass and the stellar mass of these galaxies are consistent with each other in relativistic MOND.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1702.00183}, -author = {Tian, Yong and Ko, Chung Ming}, -doi = {10.1093/MNRAS/STX2056}, -eprint = {1702.00183}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: kinematics and dynamics,Dark matter,Galaxies: elliptical and lenticular,Gravitation,Gravitational lensing: strong}, -number = {1}, -pages = {765--771}, -title = {{Mass discrepancy-acceleration relation in Einstein rings}}, -url = {http://arxiv.org/abs/1702.00183}, -volume = {472}, -year = {2017} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of supermassive black hole (SMBH) formation and evolution is used, as in Tremmel et al., allowing us to explicitly follow the SMBH dynamics at the centre of galaxies. A high SIDM constant cross-section is chosen, $\sigma$ = 10 cm2gr-1, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in cold dark matter (CDM), with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals, the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80 per cent of the SMBH population is offcentred in the SIDM case, as opposed to the CDM case in which {\$\sim${}}90 per cent of SMBHs have reached their host's centre. SMBHs are found as far as {\$\sim${}}9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction time-scale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in core stalling. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to the SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@article{Ding2019, -abstract = {Correlations between the mass of a supermassive black hole and the properties of its host galaxy (e.g., total stellar mass (M*), luminosity (Lhost)) suggest an evolutionary connection. A powerful test of a co-evolution scenario is to measure the relations MBH-Lhost and MBH-M* at high redshift and compare with local estimates. For this purpose, we acquired HST imaging with WFC3 of 32 X-ray-selected broad-line AGN at 1.2{\textless}z{\textless}1.7 in deep survey fields. By applying state-of-the-art tools to decompose the HST images including available ACS data, we measured the host galaxy luminosity and stellar mass along with other properties through the 2D model fitting. The black hole mass was determined using the broad Halpha line, detected in the near-infrared with Subaru/FMOS, which potentially minimizes systematic effects using other indicators. We find that the observed ratio of MBH to total M* is 2.7 times larger at z{\$\sim${}}1.5 than in the local universe, while the scatter is equivalent between the two epochs. A non-evolving mass ratio is consistent with the data at the 2-3 sigma confidence level when accounting for selection effects and their uncertainties. The relationship between MBH-Lhost paints a similar picture. Therefore, our results cannot distinguish whether SMBHs and their total M* and Lhost proceed in lockstep or whether the growth of the former somewhat overshoots the latter, given the uncertainties. Based on a statistical estimate of the bulge-to-total mass fraction, the ratio MBH/M* is offset from the local value by a factor of {\$\sim${}}7 which is significant even accounting for selection effects. Taken together, these observations are consistent with a scenario in which stellar mass is subsequently transferred from an angular momentum supported component of the galaxy to the pressure supported one through secular processes or minor mergers at a faster rate than mass accretion onto the SMBH.}, -archivePrefix = {arXiv}, -arxivId = {1910.11875}, -author = {Ding, Xuheng and Silverman, John and Treu, Tommaso and Schulze, Andreas and Schramm, Malte and Birrer, Simon and Park, Daeseong and Jahnke, Knud and Bennert, Vardha N and Kartaltepe, Jeyhan S and Koekemoer, Anton M and Malkan, Matthew A and Sanders, David}, -doi = {10.3847/1538-4357/ab5b90}, -eprint = {1910.11875}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {37}, -title = {{ The Mass Relations between Supermassive Black Holes and Their Host Galaxies at 1 {\textless} z {\textless} 2 with HST -WFC3 }}, -url = {http://arxiv.org/abs/1910.11875}, -volume = {888}, -year = {2020} -} -@article{Barro2013, -abstract = {We combine high-resolution Hubble Space Telescope/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (M* {\textgreater} 1010 M⊙) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z ≳ 2, cSFGs present SFR = 100-200 M yr-1, yet their specific star formation rates (sSFR ∼ 10-9 yr -1) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (∼30{\%}) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 108 yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z ∼ 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z ≳ 2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z ≲ 2) path in which larger SFGs form extended QGs without passing through a compact state. {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1206.5000}, -author = {Barro, Guillermo and Faber, S M and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Koo, David C and Williams, Christina C and Kocevski, Dale D and Trump, Jonathan R and Mozena, Mark and McGrath, Elizabeth and {Van Der Wel}, Arjen and Wuyts, Stijn and Bell, Eric F and Croton, Darren J and Daniel, Ceverino and Dekel, Avishai and Ashby, M L N and Cheung, Edmond and Ferguson, Henry C and Fontana, Adriano and Fang, Jerome and Giavalisco, Mauro and Grogin, Norman A and Guo, Yicheng and Hathi, Nimish P and Hopkins, Philip F and Huang, Kuang Han and Koekemoer, Anton M and Kartaltepe, Jeyhan S and Lee, Kyoung Soo and Newman, Jeffrey A and Porter, Lauren A and Primack, Joel R and Ryan, Russell E and Rosario, David and Somerville, Rachel S and Salvato, Mara and Hsu, Li Ting}, -doi = {10.1088/0004-637X/765/2/104}, -eprint = {1206.5000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: high-redshift,galaxies: photometry,galaxies: starburst}, -number = {2}, -pmid = {7117407}, -title = {{Candels: The progenitors of compact quiescent galaxies at Z ∼ 2}}, -volume = {765}, -year = {2013} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and S{\'{e}}rsic index distributions obtained from two-dimensional structural fits to 40, 000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of S{\'{e}}rsic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. {\textcopyright}2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Tamura2015, -abstract = {We report the detailed modeling of the mass profile of a z = 0.2999 massive elliptical galaxy using 30 milli-arcsecond resolution 1 mm Atacama Large Millimeter/submillimeter Array (ALMA) images of the galaxy-galaxy lensing system SDP.81. The detailed morphology of the lensed multiple images of the z = 3.042 infrared-luminous galaxy, which is found to consist of tens of 100 pc-sized star-forming clumps embedded in a ∼ 2 kpc disk, are well reproduced by a lensing galaxy modeled by an isothermal ellipsoid with a 400 pc core. The core radius is consistent with that of the visible stellar light, and the mass-to-light ratio of ${\sim}\,2\,M-{\odot }\,L-{\odot }^{-1}$ is comparable to the locally measured value, suggesting that the inner 1 kpc region is dominated by luminous matter. The position of the predicted mass centroid is consistent to within 30 mas with a non-thermal source detected with ALMA, which likely traces an active galactic nucleus of the foreground elliptical galaxy. While the black hole mass and the core radius of the elliptical galaxy are degenerate, a point source mass of > 3 × 108 M mimicking a supermassive black hole is required to explain the non-detection of a central image of the background galaxy. The required mass is consistent with the prediction from the well-known correlation between black hole mass and host velocity dispersion. Our analysis demonstrates the power of high resolution imaging of strong gravitational lensing for studying the innermost mass profile and the central supermassive black hole of distant elliptical galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1503.07605}, -author = {Tamura, Yoichi and Oguri, Masamune and Iono, Daisuke and Hatsukade, Bunyo and Matsuda, Yuichi and Hayashi, Masao}, -doi = {10.1093/pasj/psv040}, -eprint = {1503.07605}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Tamura2015StrongLensALMA.pdf:pdf}, -issn = {2053051X}, -journal = {PASJ}, -keywords = {Black hole physics,Galaxies: individual (H-ATLAS J090311.6+003906),Galaxies: structure,Gravitational lensing: strong,Submillimeter: galaxies}, -number = {4}, -pages = {1--7}, -title = {{High-resolution ALMA observations of SDP.81. I. the innermost mass profile of the lensing elliptical galaxy probed by 30 milli-arcsecond images}}, -volume = {67}, -year = {2015} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of LCDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2004} -} -@article{Agertz2011, -abstract = {We study the formation of disc galaxies in a fully cosmological framework using adaptive mesh refinement simulations. We perform an extensive parameter study of the main subgrid processes that control how gas is converted into stars and the coupled effect of supernovae feedback. We argue that previous attempts to form disc galaxies have been unsuccessful because of the universal adoption of strong feedback combined with high star formation efficiencies. Unless extreme amounts of energy are injected into the interstellar medium during supernovae events, these star formation parameters result in bulge-dominated S0/Sa galaxies as star formation is too efficient at z$\sim$ 3. We show that a low efficiency of star formation more closely models the subparsec physical processes, especially at high redshift. We highlight the successful formation of extended disc galaxies with scalelengths rd= 4-5 kpc, flat rotation curves and bulge-to-disc ratios of B/D $\sim$ 1/4. Not only do we resolve the formation of a Milky Way-like spiral galaxy, we also observe the secular evolution of the disc as it forms a pseudo-bulge. The disc properties agree well with observations and are compatible with the photometric and baryonic Tully-Fisher relations, the $\Sigma$SFR-$\Sigma$gas (Kennicutt-Schmidt) relation and the observed angular momentum content of spiral galaxies. We conclude that the underlying small-scale star formation physics plays a greater role than previously considered in simulations of galaxy formation. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1004.0005}, -author = {Agertz, Oscar and Teyssier, Romain and Moore, Ben}, -doi = {10.1111/j.1365-2966.2010.17530.x}, -eprint = {1004.0005}, -isbn = {0710305311}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes,Galaxies: spiral,Methods: numerical}, -number = {2}, -pages = {1391--1408}, -pmid = {619}, -title = {{The formation of disc galaxies in a $\Lambda$CDM universe}}, -volume = {410}, -year = {2011} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 {\textless} z {\textless} 0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 percent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.0763}, -author = {Lackner, C N and Gunn, J E}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data%7B%5C_%7Dquery?bibcode=2012arXiv1201.0763L%7B%5C&%7Dlink%7B%5C_%7Dtype=ABSTRACT%7B%5C%25%7D5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Bezanson2009, -abstract = {Recent studies have shown that massive quiescent galaxies at high redshift are much more compact than present-day galaxies of the same mass. Here we compare the radial stellar density profiles and the number density of a sample of massive galaxies at z 2.3 to nearby massive elliptical galaxies. We confirm that the average stellar densities of the z 2.3 galaxies within the effective radius, $\rho$(80$d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is $1.6^{+1.2}_{-0.5}$ per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2$R_{\oplus}$ that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C. and Ford, Eric B. and Ragozzine, Darin and Morehead, Robert C.}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hsu et al. - 2018 - Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation(2).pdf:pdf}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -number = {5}, -pages = {205}, -title = {{ Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation }}, -url = {http://arxiv.org/abs/1803.10787%0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -volume = {155}, -year = {2018} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: `blue-sequence' galaxies that are rapidly forming young stars, and `red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than {\$}3\backslashbackslashtimes10{\^{}}{\{}10{\}} M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}} follow the red-sequence while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's center. We develop a simple analytic model for this interaction. In galaxies less massive than {\$}3\backslashbackslashtimes10{\^{}}{\{}10{\}} M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}}, young stars and supernovae drive a high entropy outflow that is more buoyant that any diffuse corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by a hot corona. We argue that above a halo mass of {\$}\backslashbackslashsim 10{\^{}}{\{}12{\}} M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}}, the supernova-driven outflow is no longer buoyant and star formation is unable to prevent the build up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers. We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations, and demonstrate that, so long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice. The transition mass disappears entirely, however, if star formation driven outflows are absent.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Schombert2015a, -abstract = {Using isophotal radius correlations for a sample of Two Micron All Sky Survey ellipticals, we have constructed a series of template surface brightness profiles to describe the profile shapes of ellipticals as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that ellipticals are weakly nonhomologous with respect to structure. Through comparison to the templates, it is discovered that ellipticals are divided into two families: those well matched to the templates, and a second class of ellipticals with distinctly shallower profile slopes. We refer to this second type of ellipticals as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D ellipticals cover the same range of luminosity, size, and kinematics as normal ellipticals, but maintain a signature of recent equal-mass dry mergers. We propose that normal ellipticals grow after an initial dissipation formation era by accretion of low-mass companions as outlined in hierarchical formation scenarios, while D ellipticals are the result of later equal-mass mergers producing shallow luminosity profiles.}, -archivePrefix = {arXiv}, -arxivId = {1509.08381}, -author = {Schombert, James M.}, -doi = {10.1088/0004-6256/150/5/162}, -eprint = {1509.08381}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Schombert - 2015 - The structure of galaxies. III. Two structural families of ellipticals.pdf:pdf}, -isbn = {doi:10.1088/0004-6256/150/5/162}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: photometry,galaxies: structure}, -number = {5}, -pages = {162}, -publisher = {IOP Publishing}, -title = {{The structure of galaxies. III. Two structural families of ellipticals}}, -url = {http://dx.doi.org/10.1088/0004-6256/150/5/162}, -volume = {150}, -year = {2015} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the $\Lambda$CDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no significant detection of a stellar halo, as in the case of M101, NGC 3351 and NGC 1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies in the range M200 = 8 × 1011-2 × 1012 M⊙ with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction fSH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming, and assemble their dark matter halos earlier than galaxies with similar masses. They have also accreted more low-mass satellites at earlier infall times than centrals with high fSH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretiondominated r {\$\sim${}} 45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers at higher redshifts and evolved unperturbed in the last {\$\sim${}}10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M and Sales, Laura V and Creasey, Peter and Cooper, Michael C and Bullock, James S and {Michael Rich}, R and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Iwanus2017, -abstract = {We describe and test a novel dark matter annihilation feedback (DMAF) scheme that has been implemented into the well-known cosmological simulation code GADGET-2. In the models considered here, dark matter can undergo self-annihilation/decay into radiation and baryons. These products deposit energy into the surrounding gas particles and then the dark matter/baryon fluid is self-consistently evolved under gravity and hydrodynamics. We present tests of this new feedback implementation in the case of idealized dark matter haloes with gas components for a range of halomasses, concentrations and annihilation rates. For some darkmattermodels, DMAF's ability to evacuate gas is enhanced in lower mass, concentrated haloes where the injected energy is comparable to its gravitational binding energy. Therefore, we expect the strongest signs of darkmatter annihilation to imprint themselves on to the baryonic structure of concentrated dwarf galaxies through their baryonic fraction and star formation history. Finally, we present preliminary results of the first self-consistent DMAF cosmological box simulations showing that the small-scale substructure is washed out for large annihilation rates.}, -archivePrefix = {arXiv}, -arxivId = {1707.06770}, -author = {Iwanus, N and Elahi, P J and Lewis, G F}, -doi = {10.1093/MNRAS/STX1974}, -eprint = {1707.06770}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Large-scale structure of Universe}, -number = {1}, -pages = {1214--1225}, -title = {{Dark matter annihilation feedback in cosmological simulations - I: Code convergence and idealized haloes}}, -url = {http://arxiv.org/abs/1707.06770%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1974}, -volume = {472}, -year = {2017} -} -@article{Brewer2014, -abstract = {The long-standing assumption that the stellar initial mass function (IMF) is universal has recently been challenged by a number of observations. Several studies have shown that a 'heavy' IMF (e.g. with a Salpeter-like abundance of low-mass stars and thus normalization) is preferred for massive early-type galaxies, while this IMF is inconsistent with the properties of less massive, later-type galaxies. These discoveries motivate the hypothesis that the IMF may vary (possibly very slightly) across galaxies and across components of individual galaxies (e.g. bulges versus discs). In this paper, we use a sample of 19 late-type strong gravitational lenses from the Sloan WFC Edge-on Late-type Lens Survey (SWELLS) to investigate the IMFs of the bulges and discs in late-type galaxies. We perform a joint analysis of the galaxies' total masses (constrained by strong gravitational lensing) and stellar masses (constrained by optical and near-infrared colours in the context of a stellar population synthesis model, up to an IMF normalization parameter). Using minimal assumptions apart from the physical constraint that the total stellar mass m* within any aperture must be less than the total mass mtot with in the aperture, we find that the bulges of the galaxies cannot have IMFs heavier (i.e. implying high mass per unit luminosity) than Salpeter, while the disc IMFs are not well constrained by this data set.We also discuss the necessity for hierarchical modelling when combining incomplete information about multiple astronomical objects. This modelling approach allows us to place upper limits on the size of any departures from universality. More data, including spatially resolved kinematics (as in Paper V) and stellar population diagnostics over a range of bulge and disc masses, are needed to robustly quantify how the IMF varies within galaxies. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1310.5177}, -author = {Brewer, Brendon J. and Marshal, Philip J. and Auger, Matthew W. and Treu, Tommaso and Dutton, Aaron A. and Barnab{\`{e}}, Matteo}, -doi = {10.1093/mnras/stt2026}, -eprint = {1310.5177}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies:Fundamental parameters,Galaxies:Spiral,Methods:Statistical}, -month = {jan}, -number = {2}, -pages = {1950--1961}, -title = {{The SWELLS survey - VI. Hierarchical inference of the initial mass functions of bulges and discs}}, -volume = {437}, -year = {2013} -} -@article{Lipnicky2018, -abstract = {We reportHI observations of eight spiral galaxies that are strongly lensing background sources. Our targets were selected from the Sloan WFC (Wide Field Camera) Edge-on Late-type Lens Survey (SWELLS) using the Arecibo, Karl G. Jansky Very Large Array, and Green Bank telescopes. We securely detect J1703+2451 at z = 0.063 with a signal-to-noise ratio of 6.7 and W50 = 79 ± 13 km s-1, obtaining the first detection of HI emission in a strong spiral lens. We measure a mass of MHI = (1.77 ± 0.06 -0.75+0.35) × 109M⊙ for this source. We find that this lens is a normal spiral, with observable properties that are fairly typical of spiral galaxies. For three other sources, we did not secure a detection; however, we are able to place strong constraints on the HI masses of those galaxies. The observations for four of our sources were rendered unusable due to strong radio frequency interference.}, -archivePrefix = {arXiv}, -arxivId = {1802.01588}, -author = {Lipnicky, Andrew and Chakrabarti, Sukanya and Wright, Melvyn C.H. and Blitz, Leo and Heiles, Carl and Cotton, William and Frayer, David and Blandford, Roger and Shu, Yiping and Bolton, Adam S.}, -doi = {10.1093/mnras/sty326}, -eprint = {1802.01588}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lipnicky et al. - 2018 - The first detection of neutral hydrogen in emission in a strong spiral lens(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Radio lines: galaxies}, -number = {3}, -pages = {3097--3105}, -title = {{The first detection of neutral hydrogen in emission in a strong spiral lens}}, -url = {http://arxiv.org/abs/1802.01588%0Ahttp://dx.doi.org/10.1093/mnras/sty326}, -volume = {476}, -year = {2018} -} -@article{Keeton1997, -abstract = {Galaxies modeled as singular isothermal ellipsoids with an axis ratio distribution similar to the observed axis ratio distribution of E and S0 galaxies are statistically consistent with both the observed numbers of two-image and four-image lenses and the inferred ellipticities of individual lenses. However, no four-image lens is well fit by the model (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 20{\$}), the axis ratio of the model can be significantly different from that of the observed lens galaxy, and the major axes of the model and the galaxy may be slightly misaligned. We found that models with a second, independent, external shear axis could fit the data well (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 1{\$}), while adding the same number of extra parameters to the radial mass distribution does not produce such a dramatic improvement in the fit. An independent shear axis can be produced by misalignments between the luminous galaxy and its dark matter halo, or by external shear perturbations due to galaxies and clusters correlated with the primary lens or along the line of sight. We estimate that the external shear perturbations have no significant effect on the expected numbers of two-image and four-image lenses, but that they can be important perturbations in individual lens models. However, the amplitudes of the external shears required to produce the good fits are larger than our estimates for typical external shear perturbations (10-15{\%} shear instead of 1-3{\%} shear) suggesting that the origin of the extra angular structure must be intrinsic to the primary lens galaxy in most cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610163}, -author = {Keeton, C R and Kochanek, C S and Seljak, U}, -doi = {10.1086/304172}, -eprint = {9610163}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Elliptical and Lenticular,cD,cosmology: theory}, -number = {2}, -pages = {604--620}, -primaryClass = {astro-ph}, -title = {{Shear and Ellipticity in Gravitational Lenses}}, -url = {http://arxiv.org/abs/astro-ph/9610163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/304172}, -volume = {482}, -year = {1997} -} -@article{Calanog2014a, -abstract = {We present Keck-Adaptive Optics and Hubble Space Telescope high resolution near-infrared (IR) imaging for 500 $\mu$m bright candidate lensing systems identified by the Herschel Multi-tiered Extragalactic Survey and Herschel Astrophysical Terahertz Large Area Survey. Out of 87 candidates with near-IR imaging, 15 (∼17%) display clear near-IR lensing morphologies. We present near-IR lens models to reconstruct and recover basic rest-frame optical morphological properties of the background galaxies from 12 new systems. Sources with the largest near-IR magnification factors also tend to be the most compact, consistent with the size bias predicted from simulations and previous lensing models for submillimeter galaxies (SMGs). For four new sources that also have high-resolution submillimeter maps, we test for differential lensing between the stellar and dust components and find that the 880 $\mu$m magnification factor ($\mu$880) is ∼1.5 times higher than the near-IR magnification factor ($\mu$NIR), on average. We also find that the stellar emission is ∼2 times more extended in size than dust. The rest-frame optical properties of our sample of Herschel-selected lensed SMGs are consistent with those of unlensed SMGs, which suggests that the two populations are similar.}, -author = {Calanog, J. A. and Fu, Hai and Cooray, A. and Wardlow, J. and Ma, B. and Amber, S. and Baker, A. J. and Baes, M. and Bock, J. and Bourne, N. and Bussmann, R. S. and Casey, C. M. and Chapman, S. C. and Clements, D. L. and Conley, A. and Dannerbauer, H. and {De Zotti}, G. and Dunne, L. and Dye, S. and Eales, S. and Farrah, D. and Furlanetto, C. and Harris, A. I. and Ivison, R. J. and Kim, S. and Maddox, S. J. and Magdis, G. and Messias, H. and Micha{\l}lowski, M. J. and Negrello, M. and Nightingale, J. and O'Bryan, J. M. and Oliver, S. J. and Riechers, D. and Scott, D. and Serjeant, S. and Simpson, J. and Smith, M. and Timmons, N. and Thacker, C. and Valiante, E. and Vieira, J. D.}, -doi = {10.1088/0004-637X/797/2/138}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: star formation,Gravitational lensing: strong,Submillimeter: galaxies}, -number = {2}, -title = {{Lens models of herschel-selected galaxies from high-resolution near-IR observations}}, -volume = {797}, -year = {2014} -} -@article{Anderson2010, -abstract = {We use an empirical approach to characterize the effect of charge-transfer efficiency (CTE) losses in images taken with the Wide-Field Channel of the Advanced Camera for Surveys (ACS). The study is based on profiles of warm pixels in 168 dark exposures taken between 2009 September and October. The dark exposures allow us to explore charge traps that affect electrons when the background is extremely low. We develop a model for the readout process that reproduces the observed trails out to 70 pixels. We then invert the model to convert the observed pixel values in an image into an estimate of the original pixel values. We find that when we apply this image-restoration process to science images with a variety of stars on a variety of background levels, it restores flux, position, and shape. This means that the observed trails contain essentially all of the flux lost to inefficient CTE. The Space Telescope Science Institute is currently evaluating this algorithm with the aim of optimizing it and eventually providing enhanced data products. The empirical procedure presented here should also work for other epochs (e.g., pre-SM4), though the parameters may have to be recomputed for the time when ACS was operated at a higher temperature than the current -81°C. Finally, this empirical approach may also hold promise for other instruments, such as WFPC2, STIS, the ACS's HRC, and even WFC3/UVIS.}, -archivePrefix = {arXiv}, -arxivId = {1007.3987}, -author = {Anderson, Jay and Bedin, Luigi R.}, -doi = {10.1086/656399}, -eprint = {1007.3987}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Anderson, Bedin - 2010 - An Empirical Pixel-Based Correction for Imperfect CTE. I. HST 's Advanced Camera for Surveys1(2).pdf:pdf}, -issn = {0004-6280}, -journal = {Publ. Astron. Soc. Pac.}, -keywords = {Astronomical Techniques}, -month = {sep}, -number = {895}, -pages = {1035--1064}, -title = {{An Empirical Pixel-Based Correction for Imperfect CTE. I. HST 's Advanced Camera for Surveys1}}, -url = {http://iopscience.iop.org/article/10.1086/656399}, -volume = {122}, -year = {2010} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the foreground lenses and background sources are early-type galaxies. Using imaging from Hubble Space Telescope (HST)/Advanced Camera for Studies (ACS) andKeck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population ofmassive, compact galaxies at redshifts 0.4 ≲ z ≲ 0.7, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of highredshift red nuggets or their partly evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar populations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S{\'{e}}rsic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still compact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterized by red-to-blue colour gradients as a function of radius which are stronger at low redshift - indicative of ongoing accretion - but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are pre-dominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W and Fassnacht, Christopher D and Treu, Tommaso and Brewer, Brendon J and Koopmans, L V E and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Gavazzi2012a, -abstract = {We study the relative alignment of mass and light in a sample of 16 massive early-type galaxies at z = 0.2-0.9 that act as strong gravitational lenses. The sample was identified from deep multi-band images obtained as part of the Canada-France-Hawaii Telescope Legacy Survey and as part of the Strong Lensing Legacy Survey (SL2S). Higher resolution follow-up imaging is available for a subset of 10 systems. We construct gravitational lens models and infer total enclosed mass, elongation, and position angle of the mass distribution. By comparison with the observed distribution of light we infer that there is a substantial amount of external shear with mean value 〈$\gamma$ ext〉 = 0.12 ± 0.05, arising most likely from the environment of the SL2S lenses. In a companion paper, we combine these measurements with follow-up Keck spectroscopy to study the evolution of the stellar and dark matter content of early-type galaxies as a function of cosmic time. {\textcopyright} 2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1202.3852}, -author = {Gavazzi, Rapha{\"{e}}l and Treu, Tommaso and Marshall, Philip J. and Brault, Florence and Ruff, Andrea}, -doi = {10.1088/0004-637X/761/2/170}, -eprint = {1202.3852}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Gavazzi2012SL2SI.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {galaxies: fundamental parameters,gravitational lensing: strong}, -number = {2}, -title = {{The SL2S galaxy-scale gravitational lens sample. I. the alignment of mass and light in massive early-type galaxies at z = 0.2-0.9}}, -volume = {761}, -year = {2012} -} -@article{Loudas2022, -abstract = {The nature of dark matter (DM) is still under intense debate. Sub-galactic scales are particularly critical, as different, currently viable DM models make diverse predictions on the expected abundance and density profile of DM haloes on these scales. We investigate the ability of sub-galactic DM haloes to act as strong lenses on background compact sources, producing gravitational lensing events on milli-arcsecond scales (milli-lenses), for different DM models. For each DM scenario, we explore whether a sample of $\sim$ 5000 distant sources is sufficient to detect at least one milli-lens. We develop a semi-analytical model to estimate the milli-lensing optical depth as a function of the source's redshift for various DM models. We employ the Press-Schechter formalism, as well as results from recent N-body simulations to compute the halo mass function, taking into account the appropriate spherically averaged density profile of haloes for each DM model. We treat the lensing system as a point-mass lens and invoke the effective surface mass density threshold to calculate the fraction of a halo that acts as a gravitational lens. We study three classes of dark matter models: cold DM, warm DM, and self-interacting DM. We find that haloes consisting of warm DM turn out to be optically thin for strong gravitational milli-lensing (zero expected lensing events). CDM haloes may produce lensing events depending on the steepness of the concentration-mass relation. Self-interacting DM haloes can efficiently act as gravitational milli-lenses only if haloes experience gravothermal collapse, resulting in highly dense central cores.}, -archivePrefix = {arXiv}, -arxivId = {2209.13393}, -author = {Loudas, Nick and Pavlidou, Vasiliki and Casadio, Carolina and Tassis, Kostas}, -eprint = {2209.13393}, -file = {:C\:/Users/Jammy/Documents/Papers/Substructure/Loudas2022MiliLensing.pdf:pdf}, -keywords = {cosmology,dark matter,galaxies,gravitational lensing,haloes,methods,semi-analytical,strong}, -title = {{Discriminating power of milli-lensing observations for dark matter models}}, -url = {http://arxiv.org/abs/2209.13393}, -year = {2022} -} -@article{Blumenthal1986, -abstract = {Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in. radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.}, -author = {Blumenthal, G R and Faber, S M and Flores, R and Primack, J R}, -doi = {10.1086/163867}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -pages = {27}, -title = {{Contraction of dark matter galactic halos due to baryonic infall}}, -volume = {301}, -year = {2002} -} -@article{Yang2019, -abstract = {Using the Atacama Large Millimeter/submillimeter Array (ALMA), we report high angular-resolution observations of the redshift z = 3.63 galaxy H -ATLAS J083051.0+013224 (G09v1.97), one of the most luminous strongly lensed galaxies discovered by the Herschel -Astrophysical Terahertz Large Area Survey ( H -ATLAS). We present 0.″2−0.″4 resolution images of the rest-frame 188 and 419 $\mu$ m dust continuum and the CO(6–5), H 2 O(2 11 −2 02 ), and J up = 2 H 2 O + line emission. We also report the detection of H 2 O(2 11 −2 02 ) in this source. The dust continuum and molecular gas emission are resolved into a nearly complete ∼1. ″ 5 diameter Einstein ring plus a weaker image in the center, which is caused by a special dual deflector lensing configuration. The observed line profiles of the CO(6–5), H 2 O(2 11 −2 02 ), and J up = 2 H 2 O + lines are strikingly similar. In the source plane, we reconstruct the dust continuum images and the spectral cubes of the CO, H 2 O, and H 2 O + line emission at sub-kiloparsec scales. The reconstructed dust emission in the source plane is dominated by a compact disk with an effective radius of 0.7 ± 0.1 kpc plus an overlapping extended disk with a radius twice as large. While the average magnification for the dust continuum is $\mu$ ∼ 10−11, the magnification of the line emission varies from 5 to 22 across different velocity components. The line emission of CO(6–5), H 2 O(2 11 −2 02 ), and H 2 O + have similar spatial and kinematic distributions. The molecular gas and dust content reveal that G09v1.97 is a gas-rich major merger in its pre-coalescence phase, with a total molecular gas mass of ∼10 11 M ⊙ . Both of the merging companions are intrinsically ultra-luminous infrared galaxies (ULIRGs) with infrared luminosities L IR reaching ≳4 × 10 12 L ⊙ , and the total L IR of G09v1.97 is (1.4 ± 0.7)×10 13 L ⊙ . The approaching southern galaxy (dominating from V = −400 to −150 km s −1 relative to the systemic velocity) shows no obvious kinematic structure with a semi-major half-light radius of a s = 0.4 kpc, while the receding galaxy (0 to 350 km s −1 ) resembles an a s = 1.2 kpc rotating disk. The two galaxies are separated by a projected distance of 1.3 kpc, bridged by weak line emission (−150 to 0 km s −1 ) that is co-spatially located with the cold dust emission peak, suggesting a large amount of cold interstellar medium (ISM) in the interacting region. As one of the most luminous star-forming dusty high-redshift galaxies, G09v1.97 is an exceptional source for understanding the ISM in gas-rich starbursting major merging systems at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {1903.00273}, -author = {Yang, C and Gavazzi, R and Beelen, A and Cox, P and Omont, A and Lehnert, M D and Gao, Y and Ivison, R J and Swinbank, A M and Barcos-Mu{\~{n}}oz, L and Neri, R and Cooray, A and Dye, S and Eales, S and Fu, H and Gonz{\'{a}}lez-Alfonso, E and Ibar, E and Micha{\l}owski, M J and Nayyeri, H and Negrello, M and Nightingale, J and P{\'{e}}rez-Fournon, I and Riechers, D A and Smail, I and van der Werf, P}, -doi = {10.1051/0004-6361/201833876}, -eprint = {1903.00273}, -keywords = {galaxies,gravitational lensing,high-redshift,ism,molecules,radio lines,strong,submillimeter}, -pages = {23--42}, -title = {{CO, H2O, H2O+ line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales}}, -url = {http://arxiv.org/abs/1903.00273}, -volume = {138}, -year = {2019} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR $\eta$(z) using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of 102 SGL with the measurement of corresponding velocity dispersion $\sigma$0 and Einstein radius $\theta$E. In addition, we also use a dataset of 12 two image lensing systems containing the measure of time delay $\Delta$ t between source images. Jointly these two datasets give us the angular diameter distance DAol of the lens. Further, for luminosity distance, we use the 740 observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ($\eta$=1) within 2$\sigma$ confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R F L}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Velliscig2015b, -abstract = {We report results for the alignments of galaxies in the EAGLE and cosmo-OWLS hydrodynamical cosmological simulations as a function of galaxy separation (-1 ≤ log10(r/[h-1Mpc]) ≤ 2) and halo mass (10.7 ≤ log10(M200/[h-1M⊙]) ≤ 15). We focus on two classes of alignments: the orientations of galaxies with respect to either the directions to, or the orientations of, surrounding galaxies. We find that the strength of the alignment is a strongly decreasing function of the distance between galaxies. For galaxies hosted by the mostmassive haloes in our simulations the alignment can remain significant up to $\sim$ 100Mpc. Galaxies hosted by more massive haloes show stronger alignment. At a fixed halo mass, more aspherical or prolate galaxies exhibit stronger alignments. The spatial distribution of satellites is anisotropic and significantly aligned with the major axis of the main host halo. The major axes of satellite galaxies, when all stars are considered, are preferentially aligned towards the centre of themain host halo. The predicted projected direction-orientation alignment, Εg+(rp), is in broad agreement with recent observations.We find that the orientation-orientation alignment is weaker than the orientation-direction alignment on all scales. Overall, the strength of galaxy alignments depends strongly on the subset of stars that are used to measure the orientations of galaxies and it is always weaker than the alignment of dark matter haloes. Thus, alignment models that use halo orientation as a direct proxy for galaxy orientation overestimate the impact of intrinsic galaxy alignments.}, -archivePrefix = {arXiv}, -arxivId = {1507.06996}, -author = {Velliscig, Marco and Cacciato, Marcello and Schaye, Joop and Hoekstra, Henk and Bower, Richard G. and Crain, Robert A. and van Daalen, Marcel P. and Furlong, Michelle and McCarthy, I. G. and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stv2198}, -eprint = {1507.06996}, -isbn = {1326-5377 (Electronic)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: large-scale structure of the Universe,Cosmology: theory,Galaxies: formation,galaxies: haloes}, -month = {dec}, -number = {3}, -pages = {3328--3340}, -title = {{Intrinsic alignments of galaxies in the EAGLE and cosmo-OWLS simulations}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.454.3328V}, -volume = {454}, -year = {2015} -} -@book{Graham2011, -abstract = {A century ago, in 1911 and 1913, Plummer and then Reynolds introduced their models to describe the radial distribution of stars in “nebulae.”� This article reviews the progress since then, providing both an historical perspective and a contemporary review of the stellar structure of bulges, disks, and elliptical galaxies. The quantification of galaxy nuclei, such as central mass deficits and excess nuclear light, plus, briefly, the structure of dark matter halos and cD galaxy envelopes, are discussed. Issues pertaining to spiral galaxies including dust, bulge-to-disk ratios, bulgeless galaxies, bars, and the identification of pseudobulges are also reviewed. An array of modern scaling relations involving sizes, luminosities, surface brightnesses, and stellar concentrations are presented, many of which are shown to be curved. These “redshift zero” relations not only quantify the behavior and nature of galaxies in the Universe today but are the modern benchmark for evolutionary studies of galaxies, whether based on observations, N-body simulations, or semi-analytical modeling. For example, it is shown that some of the recently discovered compact elliptical galaxies at 1. 5 < z < 2. 5 may be the bulges of modern disk galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1108.0997}, -author = {Graham, Alister W.}, -booktitle = {Planets, Stars and Stellar Systems: Volume 6: Extragalactic Astronomy and Cosmology}, -doi = {10.1007/978-94-007-5609-0_2}, -eprint = {1108.0997}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Graham - 2013 - Elliptical and disk galaxy structure and modern scaling laws(2).pdf:pdf}, -isbn = {9789400756090}, -keywords = {Core-S{\'{e}}rsicmodel,Dark matter halos,Edwin,Einasto model,Galaxy: Bars,Galaxy: Bulge-disk ratios,Galaxy: Bulgeless,Galaxy: Compact,Galaxy: Dust,Galaxy: Elliptical,Galaxy: Nuclei,Galaxy: Pseudobulges,Galaxy: Scaling relations,Galaxy: Spiral,Galaxy: Structure,Galaxy: cdahalos,Galaxy:Central mass deficits,Galaxy:Elliptical,Hubble,JosephB,Reynolds,Sarsic model}, -pages = {91--139}, -title = {{Elliptical and disk galaxy structure and modern scaling laws}}, -url = {http://arxiv.org/abs/1108.0997%0Ahttp://dx.doi.org/10.1007/978-94-007-5609-0_2}, -volume = {6}, -year = {2013} -} -@article{Nightingale2024, -abstract = {The cold dark matter (DM) model predicts that every galaxy contains thousands of DM subhaloes;{\~{a}}lmost{\~{a}}ll other DM models include{\~{a}} physical process that smooths{\~{a}}way the subhaloes. The subhaloes{\~{a}}re invisible, but could be detected via strong gravitational lensing, if they lie on the line of sight to{\~{a}} multiply imaged background source,{\~{a}}nd perturb its{\~{a}}pparent shape. We present{\~{a}} predominantly{\~{a}}utomated strong lens{\~{a}}nalysis framework,{\~{a}}nd scan for DM subhaloes in Hubble Space Telescope imaging of 54 strong lenses. We identify five DM subhalo candidates, including two especially compelling candidates (one pre viously kno wn in SLACS0946 + 1006) where{\~{a}} subhalo is fa v oured{\~{a}}fter{\~{a}}ll of our tests for systematics. We find that the detectability of subhaloes depends upon the{\~{a}}ssumed parametric form for the lens galaxy's mass distribution, especially its degree of{\~{a}}zimuthal freedom. Using separate components for DM{\~{a}}nd stellar mass reveals two DM subhalo candidates{\~{a}}nd remo v es four false positives compared to the single power-law mass model that is common in the literature. We identify 45 lenses without substructures, the number of which is key to statistical tests{\~{a}}ble to rule out models of, for example, warm or self-interacting DM. Our full{\~{a}}nalysis results{\~{a}}re{\~{a}}vailable{\~{a}}t ht tps://github.com/Jammy2211/aut olens subhalo.}, -archivePrefix = {arXiv}, -arxivId = {2209.10566}, -author = {Nightingale, James W. and He, Qiuhan and Cao, Xiaoyue and Amvrosiadis, Aristeidis and Etherington, Amy and Frenk, Carlos S. and Hayes, Richard G. and Robertson, Andrew and Cole, Shaun and Lange, Samuel and Li, Ran and Massey, Richard}, -doi = {10.1093/mnras/stad3694}, -eprint = {2209.10566}, -file = {:C\:/Users/Jammy/Documents/Papers/Substructure/Nightingale2022Scanm.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxy: structure,dark matter,gravitational lensing: strong}, -number = {4}, -pages = {10480--10506}, -title = {{Scanning for dark matter subhaloes in Hubble Space Telescope imaging of 54 strong lenses}}, -url = {http://arxiv.org/abs/2209.10566}, -volume = {527}, -year = {2024} -} -@article{Eichner2012, -abstract = {We study the Sloan Lens ACS (SLACS) survey strong-lensing system SDSS J1430+4105 at zl = 0.285. The lensed source (zs = 0.575) of this system has a complex morphology with several subcomponents. Its subcomponents span a radial range from 4 to 10kpc in the plane of the lens. Therefore, we can constrain the slope of the total projected mass profile around the Einstein radius from lensing alone. We measure a density profile that is slightly but not significantly shallower than isothermal at the Einstein radius. We decompose the mass of the lensing galaxy into a de Vaucouleurs component to trace the stars and an additional dark component. The spread of multiple-image components over a large radial range also allows us to determine the amplitude of the de Vaucouleurs and dark matter components separately. We get a mass-to-light ratio of M de Vauc LB≈(5.5±1.5)M⊙L⊙,B and a dark matter fraction within the Einstein radius of ≈20 to 40 per cent. Modelling the star formation history assuming composite stellar populations at solar metallicity to the galaxy's photometry yields a mass-to-light ratio of M{star, open}, salp LB≈4.0-1.3+0.6M⊙L⊙,B and M{star, open}, chab LB≈2.3-0.8+0.3M⊙L⊙,B for Salpeter and Chabrier initial mass functions, respectively. Hence, the mass-to-light ratio derived from lensing is more Salpeter like, in agreement with results for massive Coma galaxies and other nearby massive early-type galaxies. We examine the consequences of the galaxy group in which the lensing galaxy is embedded, showing that it has little influence on the mass-to-light ratio obtained for the de Vaucouleurs component of the lensing galaxy. Finally, we decompose the projected, azimuthally averaged 2D density distribution of the de Vaucouleurs and dark matter components of the lensing signal into spherically averaged 3D density profiles. We can show that the 3D dark and luminous matter density within the Einstein radius (REin ≈ 0.6 Reff) of this SLACS galaxy is similar to the values of Coma galaxies with the same velocity dispersions. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1209.2140}, -author = {Eichner, Thomas and Seitz, Stella and Bauer, Anne}, -doi = {10.1111/j.1365-2966.2012.22003.x}, -eprint = {1209.2140}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: haloes,Galaxies: individual: SDSS J1430+4105,Gravitational lensing: strong}, -number = {3}, -pages = {1918--1939}, -title = {{Golden gravitational lensing systems from the Sloan Lens ACS Survey - II. SDSS J1430+4105: A precise inner total mass profile from lensing alone}}, -volume = {427}, -year = {2012} -} -@article{Ferrarese2000, -abstract = {The masses of supermassive black holes correlate almost perfectly with the velocity dispersions of their host bulges, M(BH) $\sim$ sigma^alpha, where alpha =4.8 +/- 0.5$. The relation is much tighter than the relation between M(BH) and bulge luminosity, with a scatter no larger than expected on the basis of measurement error alone. Black hole masses estimated by Magorrian et al. (1998) lie systematically above the M(BH)-sigma relation defined by more accurate mass estimates, some by as much as two orders of magnitude. The tightness of the M(BH)-sigma relation implies a strong link between black hole formation and the properties of the stellar bulge.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0006053}, -author = {Ferrarese, Laura and Merritt, David}, -doi = {10.1086/312838}, -eprint = {0006053}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ferrarese, Merritt - 2000 - A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies.pdf:pdf}, -isbn = {0004-637X}, -issn = {0004637X}, -journal = {ApJL}, -keywords = {Black Hole Physics,Galaxies: Evolution,Galaxies: Kinematics and Dynamics}, -month = {aug}, -number = {1}, -pages = {L9--L12}, -pmid = {24453339}, -primaryClass = {astro-ph}, -title = {{A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies}}, -url = {http://arxiv.org/abs/astro-ph/0006053%0Ahttp://dx.doi.org/10.1086/312838}, -volume = {539}, -year = {2000} -} -@article{Duffy2010, -abstract = {The back-reaction of baryons on the dark matter halo density profile is of great interest, not least because it is an important systematic uncertainty when attempting to detect the dark matter. Here, we draw on a large suite of high-resolution cosmological hydrodynamical simulations to systematically investigate this process and its dependence on the baryonic physics associated with galaxy formation. The effects of baryons on the dark matter distribution are typically not well described by adiabatic contraction models. In the inner 10 per cent of the virial radius the models are only successful if we allow their parameters to vary with baryonic physics, halo mass and redshift, thereby removing all predictive power. On larger scales the profiles from dark matter only simulations consistently provide better fits than adiabatic contraction models, even when we allow the parameters of the latter models to vary. The inclusion of baryons results in significantly more concentrated density profiles if radiative cooling is efficient and feedback is weak. The dark matter halo concentration can in that case increase by as much as 30 (10) per cent on galaxy (cluster) scales. The most significant effects occur in galaxies at high redshift, where there is a strong anticorrelation between the baryon fraction in the halo centre and the inner slope of both the total and the dark matter density profiles. If feedback is weak, isothermal inner profiles form, in agreement with observations of massive, early-type galaxies. However, we find that active galactic nuclei (AGN) feedback, or extremely efficient feedback from massive stars, is necessary to match observed stellar fractions in groups and clusters, as well as to keep the maximum circular velocity similar to the virial velocity as observed for disc galaxies. These strong feedback models reduce the baryon fraction in galaxies by a factor of 3 relative to the case with no feedback. The AGN is even capable of reducing the baryon fraction by a factor of 2 in the inner region of group and cluster haloes. This in turn results in inner density profiles which are typically shallower than isothermal and the halo concentrations tend to be lower than in the absence of baryons. We therefore conclude that the disagreement between the concentrations inferred from observations of groups of galaxies and predictions from simulations that was identified by Duffy et al. is not alleviated by the inclusion of baryons. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1001.3447}, -author = {Duffy, Alan R. and Schaye, Joop and Kay, Scott T. and Vecchia, Claudio Dalla and Battye, Richard A. and Booth, C. M.}, -doi = {10.1111/j.1365-2966.2010.16613.x}, -eprint = {1001.3447}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Gravitation,Hydrodynamics,Methods: numerical}, -number = {4}, -pages = {2161--2178}, -title = {{Impact of baryon physics on dark matter structures: A detailed simulation study of halo density profiles}}, -volume = {405}, -year = {2010} -} -@article{Rizzo2021, -abstract = {There is a large consensus that gas in high-z galaxies is highly turbulent, because of a combination of stellar feedback processes and gravitational instabilities driven by mergers and gas accretion. In this paper, we present the analysis of a sample of five Dusty Star Forming Galaxies (DSFGs) at 4 z 5. Taking advantage of the magnifying power of strong gravitational lensing, we quantified their kinematic and dynamical properties from ALMA observations of their [C ii] emission line. We combined the dynamical measurements obtained for these galaxies with those obtained from previous studies to build the largest sample of z ∼4.5 galaxies with high-quality data and sub-kpc spatial resolutions, so far. We found that all galaxies in the sample are dynamically cold, with rotation-to-random motion ratios, V/$\sigma$, between 7 and 15. The relation between their velocity dispersions and their star formation rates indicates that stellar feedback is sufficient to sustain the turbulence within these galaxies and no further mechanisms are needed. In addition, we performed a rotation curve decomposition to infer the relative contribution of the baryonic (gas, stars) and dark matter components to the total gravitational potentials. This analysis allowed us to compare the structural properties of the studied DSFGs with those of their descendants, the local early type galaxies. In particular, we found that five out of six galaxies of the sample show the dynamical signature of a bulge, indicating that the spheroidal component is already in place at z ∼4.5.}, -archivePrefix = {arXiv}, -arxivId = {2102.05671}, -author = {Rizzo, Francesca and Vegetti, Simona and Fraternali, Filippo and Stacey, Hannah R. and Powell, Devon}, -doi = {10.1093/mnras/stab2295}, -eprint = {2102.05671}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Rizzo2021DSFTSample.pdf:pdf}, -isbn = {0113084617}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {galaxies: ISM,galaxies: evolution,galaxies: high-redshift,galaxies: kinematics and dynamics,gravitational lensing: strong,submillimetre: galaxies}, -number = {3}, -pages = {3952--3984}, -title = {{Dynamical properties of z 4.5 dusty star-forming galaxies and their connection with local early-type galaxies}}, -volume = {507}, -year = {2021} -} -@article{Wang2012, -abstract = {Recent studies suggest that only three of the 12 brightest satellites of the Milky Way (MW) inhabit dark matter haloes with maximum circular velocity, V max, exceeding $\sim$30 kms -1. This is in apparent contradiction with the $\Lambda$ cold dark matter (CDM) simulations of the Aquarius Project, which suggest that MW-sized haloes should have at least eight subhaloes with V max > 30 kms -1. The absence of luminous satellites in such massive subhaloes is thus puzzling and may present a challenge to the $\Lambda$CDM paradigm. We note, however, that the number of massive subhaloes depends sensitively on the (poorly known) virial mass of the MW, and that their scarcity makes estimates of their abundance from a small simulation set like Aquarius uncertain. We use the Millennium Simulation series and the invariance of the scaled subhalo velocity function (i.e. the number of subhaloes as a function of $\nu$, the ratio of the subhalo V max to the host halo virial velocity, V 200) to secure improved estimates of the abundance of rare massive subsystems. In the range 0.1 < $\nu$ < 0.5, N sub(>$\nu$) is approximately Poisson distributed about an average given by 〈N sub〉 = 10.2($\nu$/0.15) -3.11. This is slightly lower than that in Aquarius haloes, but consistent with recent results from the Phoenix Project. The probability that a $\Lambda$CDM halo has three or fewer subhaloes with V max above some threshold value, V th, is then straightforward to compute. It decreases steeply both with decreasing V th and with increasing halo mass. For V th = 30 kms -1, $\sim$40 per cent of M halo = 10 12M ⊙ haloes pass the test; fewer than $\sim$5 per cent do so for M halo ≳2 × 10 12M ⊙ and the probability effectively vanishes for M halo ≳3 × 10 12M ⊙. Rather than a failure of $\Lambda$CDM, the absence of massive subhaloes might simply indicate that the MW is less massive than is commonly thought. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1203.4097}, -author = {Wang, Jie and Frenk, Carlos S. and Navarro, Julio F. and Gao, Liang and Sawala, Till}, -doi = {10.1111/j.1365-2966.2012.21357.x}, -eprint = {1203.4097}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxy: abundances,Galaxy: halo}, -number = {4}, -pages = {2715--2721}, -title = {{The missing massive satellites of the Milky Way}}, -volume = {424}, -year = {2012} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright}2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{Rasmussen2016, -author = {Rasmussen, Carl Edward}, -pages = {1--13}, -title = {{Factor Graphs and message passing Key concepts}}, -year = {2016} -} -@article{Gunn1965, -abstract = {Not Available}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {Gunn, James E and Peterson, Bruce A}, -doi = {10.1086/148444}, -eprint = {arXiv:1011.1669v3}, -isbn = {doi:10.1086/148444}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {nov}, -pages = {1633}, -pmid = {25246403}, -title = {{On the Density of Neutral Hydrogen in Intergalactic Space.}}, -url = {http://adsabs.harvard.edu/doi/10.1086/148444}, -volume = {142}, -year = {2002} -} -@article{Wang2013, -abstract = {We investigate the spatial distribution of galactic satellites in high-resolution simulations of structure formation in the $\Lambda$ cold dark matter ($\Lambda$CDM) model: the Aquarius dark matter simulations of individual haloes and the Millennium-II simulation of a large cosmological volume. To relate the simulations to observations of the Milky Way we use two alternative models to populate dark haloes with 'visible' galaxies: a semi-analytic model of galaxy formation and an abundance matching technique. We find that the radial density profile of massive satellites roughly follows that of the dark matter halo (unlike the distribution of dark matter subhaloes). Furthermore, our two galaxy formation models give resultsconsistent with the observed profile of the 11 classical satellites of the Milky Way. Our simulations predict that larger, fainter samples of satellites should still retain this profile at least up to samples of 100 satellites. The angular distribution of the classical satellites of the Milky Way is known to be highly anisotropic. Depending on the exact measure of flattening, 5-10 per cent of satellite systems in our simulations are as flat as the Milky Way's and this fraction does not change when we correct for possible obscuration of satellites by the Galactic disc. A moderate flattening ofsatellite systems is a general property of $\Lambda$CDM, best understood as the consequence of preferential accretion along filaments of the cosmic web. Accretion of a single rich group of satellites can enhance the flattening due to such anisotropic accretion. We verify that a typical Milky Way-mass cold dark matter halo does not acquire its 11 most massive satellites from a small number of rich groups. Single-group accretion becomes more likely for less massive satellites. Our model predictions should be testable with forthcoming studies of satellite systems in other galaxies and surveys of fainter satellites in the MilkyWay. {\textcopyright} 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1206.1340}, -author = {Wang, Jie and Frenk, Carlos S. and Cooper, Andrew P.}, -doi = {10.1093/mnras/sts442}, -eprint = {1206.1340}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang, Frenk, Cooper - 2013 - The spatial distribution of galactic satellites in the $\Lambda$ cold dark matter cosmology(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxy: formation,Galaxy: structure,Methods: numerical}, -number = {2}, -pages = {1502--1513}, -title = {{The spatial distribution of galactic satellites in the $\Lambda$ cold dark matter cosmology}}, -volume = {429}, -year = {2013} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A. and Birnboim, Y. and Engel, G. and Freundlich, J. and Goerdt, T. and Mumcuoglu, M. and Neistein, E. and Pichon, C. and Teyssier, R. and Zinger, E.}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel et al. - 2009 - Cold streams in early massive hot haloes as the main mode of galaxy formation.pdf:pdf}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/19158792}, -volume = {457}, -year = {2009} -} -@article{Gadotti2008a, -abstract = {We have performed 2D bulge/bar/disc decompositions using g, r and i-band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for the bulge-to-total ratio than the global S{\'{e}}rsic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour-magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between the bulge S{\'{e}}rsic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass-size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass-size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0810.1953}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2008.14257.x}, -eprint = {0810.1953}, -isbn = {0372-9311 (Print){\$}\backslash{\$}r0372-9311 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {1531--1552}, -pmid = {20063786}, -title = {{Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: A Sloan Digital Sky Survey perspective}}, -url = {http://arxiv.org/abs/0810.1953%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2008.14257.x}, -volume = {393}, -year = {2009} -} -@article{Algorry2016, -abstract = {We examine the properties of barred disc galaxies in a LCDM cosmological hydrodynamical simulation from the EAGLE project. Our study follows the formation of 269 discs identified at z = 0 in the stellar mass range 10.6 {\textless} log Mstr /M {\textless} 11. These discs show a wide range of bar strengths, from unbarred discs to weak bars to strongly barred systems (= 20{\%}). Bars in these systems develop after redshift = 1.3, on timescales that depend sen- sitively on the strength of the pattern. Strong bars develop relatively quickly (in a few Gyr, = 10 disc rotation periods) in systems that are disc dominated, gas poor, and have declining rotation curves. Weak bars develop more slowly in systems where the disc is less gravitation- ally important, and are still growing at z = 0. Unbarred galaxies are comparatively gas-rich discs whose rotation speeds do not exceed the maximum circular velocity of the halos they inhabit. Bar lengths compare favourably with observations, ranging from 0.2 to 0.8 times the radius containing 90{\%} of the stars. Bars slow down remarkably quickly as they grow, causing the inner regions of the surrounding dark halo to expand. At z = 0 strong bars have corota- tion radii roughly ten times the bar length. Such slow bars are inconsistent with the few cases where pattern speeds have been measured or inferred observationally, a discrepancy that, if confirmed, might prove a challenge for disc galaxy formation in LCDM.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1609.05909}, -author = {Algorry, David G and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx1008}, -eprint = {1609.05909}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {disc,formation,galaxies,galaxy,kinematics and dynamics}, -number = {1}, -pages = {1054--1064}, -title = {{Barred galaxies in the EAGLE cosmological hydrodynamical simulation}}, -url = {http://arxiv.org/abs/1609.05909%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1008}, -volume = {469}, -year = {2017} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ({\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashgamma{\}}{\$}), we find that, although the zero cosmic curvature is still included within {\$}2 \backslashsigma{\$} confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile {\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashalpha{\}}{\$} to be different from that of the total-mass density profile {\$}\backslashnu\backslashsim r{\^{}}{\{}-\backslashdelta{\}}{\$}, a weaker constraint on the curvature ({\$}\backslashOmega{\_}k{\textless}0.197{\$} at 68$\backslash${\%} confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of {\$}\backslashDelta \backslashOmega{\_}k\backslashsimeq 10{\^{}}{\{}-3{\}}{\$}, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{Keeton1997, -abstract = {Galaxies modeled as singular isothermal ellipsoids with an axis ratio distribution similar to the observed axis ratio distribution of E and S0 galaxies are statistically consistent with both the observed numbers of two-image and four-image lenses and the inferred ellipticities of individual lenses. However, no four-image lens is well fit by the model (typical $\chi^2/N_{dof} \sim 20$), the axis ratio of the model can be significantly different from that of the observed lens galaxy, and the major axes of the model and the galaxy may be slightly misaligned. We found that models with a second, independent, external shear axis could fit the data well (typical $\chi^2/N_{dof} \sim 1$), while adding the same number of extra parameters to the radial mass distribution does not produce such a dramatic improvement in the fit. An independent shear axis can be produced by misalignments between the luminous galaxy and its dark matter halo, or by external shear perturbations due to galaxies and clusters correlated with the primary lens or along the line of sight. We estimate that the external shear perturbations have no significant effect on the expected numbers of two-image and four-image lenses, but that they can be important perturbations in individual lens models. However, the amplitudes of the external shears required to produce the good fits are larger than our estimates for typical external shear perturbations (10-15% shear instead of 1-3% shear) suggesting that the origin of the extra angular structure must be intrinsic to the primary lens galaxy in most cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610163}, -author = {Keeton, C. R. and Kochanek, C. S. and Seljak, U.}, -doi = {10.1086/304172}, -eprint = {9610163}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Keeton, Kochanek, Seljak - 1997 - Shear and Ellipticity in Gravitational Lenses(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Elliptical and Lenticular,cD,cosmology: theory}, -number = {2}, -pages = {604--620}, -primaryClass = {astro-ph}, -title = {{Shear and Ellipticity in Gravitational Lenses}}, -url = {http://arxiv.org/abs/astro-ph/9610163%0Ahttp://dx.doi.org/10.1086/304172}, -volume = {482}, -year = {1997} -} -@article{De-Lucia:2006aa, -abstract = {There is a growing body of evidence indicating young ages, 8 ± 3 Gyrs, for elliptical galaxies and significant age gradients with a younger population residing at the centre. The data appear to be consistent with a scenario where elliptical galaxies are assembled hierarchically with low luminosity galaxies forming first. Late star formation, associated with the last merging event and usually involving only a small fraction of the galaxy mass, could then account for the low age estimates of some luminous galaxies.}, -author = {Davies, Roger L.}, -doi = {10.1017/s0074180900232130}, -issn = {0074-1809}, -journal = {Symposium - International Astronomical Union}, -month = {feb}, -pages = {37--45}, -title = {{The Star Formation History of Elliptical Galaxies}}, -volume = {171}, -year = {1996} -} -@article{Morishita2018, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Seabroke2011, -abstract = {Gaia will only achieve its unprecedented measurement accuracy requirements with detailed calibration and correction for radiation damage. We present our Silvaco 3D engineering software model of the Gaia CCD pixel and two of its applications for Gaia: (1) physically interpreting supplementary buried channel (SBC) capacity measurements (pocket-pumping and first pixel response) in terms of e2v manufacturing doping alignment tolerances; and (2) deriving electron densities within a charge packet as a function of the number of constituent electrons and 3D position within the charge packet as input to microscopic models being developed to simulate radiation damage. {\textcopyright} EAS, EDP Sciences 2011.}, -archivePrefix = {arXiv}, -arxivId = {1009.2431}, -author = {Seabroke, G. M. and Prod'homme, T. and Hopkinson, G. and Burt, D. and Robbins, M. and Holland, A.}, -doi = {10.1051/eas/1045077}, -eprint = {1009.2431}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Seabroke et al. - 2011 - Modelling Gaia CCD pixels with silvaco 3D engineering software.pdf:pdf}, -isbn = {9782759806089}, -issn = {16334760}, -journal = {EAS Publications Series}, -pages = {433--436}, -title = {{Modelling Gaia CCD pixels with silvaco 3D engineering software}}, -url = {http://www.eas-journal.org/10.1051/eas/1045077}, -volume = {45}, -year = {2011} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Pillepich2017, -abstract = {We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multi-mode feedback. In this paper we give a comprehensive description of the physical and numerical advances which form the core of the IllustrisTNG (The Next Generation) framework. We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content, and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black hole driven kinetic feedback at low accretion rates, magnetohydrodynamics, and improvements to the numerical scheme. Using a suite of (25 Mpc {\$}h{\^{}}{\{}-1{\}}{\$}){\$}{\^{}}3{\$} cosmological boxes we assess the outcome of the new model at our fiducial resolution. The presence of a self-consistently amplified magnetic field is shown to have an important impact on the stellar content of {\$}10{\^{}}{\{}12{\}} M{\_}{\{}\backslashrm sun{\}}{\$} haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low mass end of the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {1703.02970}, -author = {Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R{\"{u}}diger and Hernquist, Lars and Torrey, Paul and Vogelsberger, Mark and Weinberger, Rainer and Marinacci, Federico}, -doi = {10.1093/mnras/stx2656}, -eprint = {1703.02970}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {4077--4106}, -title = {{Simulating galaxy formation with the IllustrisTNG model}}, -url = {http://arxiv.org/abs/1703.02970%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx2656}, -volume = {473}, -year = {2018} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Hsueh2018, -abstract = {The flux ratios in the multiple images of gravitationally lensed quasars can provide evidence for dark matter substructure in the halo of the lensing galaxy if the flux ratios differ from those predicted by a smooth model of the lensing galaxy mass distribution. However, it is also possible that baryonic structures in the lensing galaxy, such as edge-on discs, can produce fluxratio anomalies. In this work, we present the first statistical analysis of flux-ratio anomalies due to baryons from a numerical simulation perspective. We select galaxies with various morphological types in the Illustris simulation and ray trace through the simulated haloes, which include baryons in the main lensing galaxies but exclude any substructures, in order to explore the pure baryonic effects. Our ray-tracing results show that the baryonic components can be a major contribution to the flux-ratio anomalies in lensed quasars and that edge-on disc lenses induce the strongest anomalies.We find that the baryonic components increase the probability of finding high flux-ratio anomalies in the early-type lenses by about 8 per cent and by about 10-20 per cent in the disc lenses. The baryonic effects also induce astrometric anomalies in 13 per cent of the mock lenses. Our results indicate that the morphology of the lens galaxy becomes important in the analysis of flux-ratio anomalies when considering the effect of baryons, and that the presence of baryons may also partially explain the discrepancy between the observed (high) anomaly frequency and what is expected due to the presence of subhaloes as predicted by the cold dark matter simulations.}, -archivePrefix = {arXiv}, -arxivId = {1707.07680}, -author = {Hsueh, Jen Wei and Despali, Giulia and Vegetti, Simona and Xu, Dandan and Fassnacht, Christopher D. and Metcalf, R. Benton}, -doi = {10.1093/mnras/stx3320}, -eprint = {1707.07680}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hsueh et al. - 2018 - Flux-ratio anomalies from discs and other baryonic structures in the Illustris simulation(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {2438--2451}, -title = {{Flux-ratio anomalies from discs and other baryonic structures in the Illustris simulation}}, -volume = {475}, -year = {2018} -} -@article{Adams2010, -abstract = {Many data are naturally modeled by an unobserved hierarchical structure. In this paper we propose a flexible nonparametric prior over unknown data hierarchies. The approach uses nested stick-breaking processes to allow for trees of unbounded width and depth, where data can live at any node and are infinitely exchangeable. One can view our model as providing infinite mixtures where the components have a dependency structure corresponding to an evolutionary diffusion down a tree. By using a stick-breaking approach, we can apply Markov chain Monte Carlo methods based on slice sampling to perform Bayesian inference and simulate from the posterior distribution on trees. We apply our method to hierarchical clustering of images and topic modeling of text data.}, -archivePrefix = {arXiv}, -arxivId = {1006.1062}, -author = {Adams, Ryan Prescott and Ghahramani, Zoubin and Jordan, Michael I}, -eprint = {1006.1062}, -journal = {Advances in Neural Information Processing Systems}, -month = {jun}, -title = {{Tree-Structured Stick Breaking Processes for Hierarchical Data}}, -url = {http://arxiv.org/abs/1006.1062}, -volume = {23}, -year = {2010} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P_KS \simeq 1.5 \times 10^{-4}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability \simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R. and Kravtsov, Andrey V. and Gnedin, Oleg Y. and Klypin, Anatoly A.}, -doi = {10.1086/431355}, -eprint = {0502496}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Zentner et al. - 2005 - The Anisotropic Distribution of Galactic Satellites.pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Xie:2015aa, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -month = {feb}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Aretxaga2011, -abstract = {We present a 0.72deg2 contiguous 1.1-mm survey in the central area of the Cosmological Evolution Survey field carried out to a 1$\sigma$≈ 1.26mJybeam-1 depth with the AzTEC camera mounted on the 10-m Atacama Submillimeter Telescope Experiment. We have uncovered 189 candidate sources at a signal-to-noise ratio (S/N) ≥ 3.5, out of which 129, with S/N ≥ 4, can be considered to have little chance of being spurious (≲2per cent). We present the number counts derived with this survey, which show a significant excess of sources when compared to the number counts derived from the $\sim$0.5deg2 area sampled at similar depths in the Submillimetre Common-User Bolometer Array (SCUBA) HAlf Degree Extragalactic Survey (SHADES). They are, however, consistent with those derived from fields that were considered too small to characterize the overall blank-field population. We identify differences to be more significant in the S1.1mm≳ 5mJy regime, and demonstrate that these excesses in number counts are related to the areas where galaxies at redshifts z≲ 1.1 are more densely clustered. The positions of optical-infrared galaxies in the redshift interval 0.6 ≲z≲ 0.75 are the ones that show the strongest correlation with the positions of the 1.1-mm bright population (S1.1mm≳ 5mJy), a result which does not depend exclusively on the presence of rich clusters within the survey sampled area. The most likely explanation for the observed excess in number counts at 1.1-mm is galaxy-galaxy and galaxy-group lensing at moderate amplification levels, which increases in amplitude as one samples larger and larger flux densities. This effect should also be detectable in other high-redshift populations. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -author = {Aretxaga, I. and Wilson, G. W. and Aguilar, E. and Alberts, S. and Scott, K. S. and Scoville, N. and Yun, M. S. and Austermann, J. and Downes, T. P. and Ezawa, H. and Hatsukade, B. and Hughes, D. H. and Kawabe, R. and Kohno, K. and Oshima, T. and Perera, T. A. and Tamura, Y. and Zeballos, M.}, -doi = {10.1111/j.1365-2966.2011.18989.x}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Aretxaga2011millimetersurveyCOSMOS.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmology: miscellaneous,Galaxies: evolution,Submillimetre: galaxies,Surveys}, -number = {4}, -pages = {3831--3850}, -title = {{AzTEC millimetre survey of the COSMOS field - III. Source catalogue over 0.72 deg2 and plausible boosting by large-scale structure}}, -volume = {415}, -year = {2011} -} -@article{Costantin2017, -abstract = {Context. The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. Aims. We aim to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. Methods. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the i-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new (B=A, C=A) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. Results. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations of 25° ≤ $\theta$ ≤ 65° we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66{\%}), with a smaller fraction of prolate spheroids (19{\%}), and triaxial ellipsoids (15{\%}). The majority of triaxial bulges are in barred galaxies (75{\%}). Moreover, we found that bulges with low S{\'{e}}rsic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, bulges in late-type galaxies or in less massive galaxies have no preference for being oblate, prolate, or triaxial. On the contrary, bulges with high S{\'{e}}rsic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. Conclusions. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L and M{\'{e}}ndez-Abreu, J and Corsini, E M and Eliche-Moral, M C and Tapia, T and Morelli, L and Elena, Dalla Bont{\`{a}} and Pizzella, A}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -volume = {609}, -year = {2018} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies, in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the SDSS in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on the UV-optical colour {\$}NUV-r{\$}. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings that green valley galaxies have intermediate morphologies, moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of green valley galaxies, we find that they tend to be more massive in the field than in denser environments. On average, green valley galaxies account for {\$}\backslashbackslashsim 20\backslashbackslash{\{}\backslash{\%}{\}}{\$} of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming low mass galaxies. Green valley galaxies have average star formation histories intermediate between passive and star forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time, and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brooks, Christensen - 2015 - Bulge formation via mergers in cosmological simulations.pdf:pdf}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Hopkins2011b, -abstract = {Feedback from massive stars is believed to play a critical role in shaping the galaxy mass function, the structure of the interstellar medium (ISM) and the low efficiency of star formation, but the exact form of the feedback is uncertain. In this paper, the first in a series, we present and test a novel numerical implementation of stellar feedback resulting from momentum imparted to the ISM by radiation, supernovae and stellar winds. We employ a realistic cooling function, and find that a large fraction of the gas cools to ≲100K, so that the ISM becomes highly inhomogeneous. Despite this, our simulated galaxies reach an approximate steady state, in which gas gravitationally collapses to form giant 'molecular' clouds (GMCs), dense clumps and stars; subsequently, stellar feedback disperses the GMCs, repopulating the diffuse ISM. This collapse and dispersal cycle is seen in models of Small Magellanic Cloud (SMC)-like dwarfs, the Milky Way and z{\$\sim${}} 2 clumpy disc analogues. The simulated global star formation efficiencies are consistent with the observed Kennicutt-Schmidt relation. Moreover, the star formation rates are nearly independent of the numerically imposed high-density star formation efficiency, density threshold and density scaling. This is a consequence of the fact that, in our simulations, star formation is regulated by stellar feedback limiting the amount of very dense gas available for forming stars. In contrast, in simulations without stellar feedback, i.e. under the action of only gravity and gravitationally induced turbulence, the ISM experiences runaway collapse to very high densities. In these simulations without feedback, the global star formation rates exceed observed galactic star formation rates by 1-2 orders of magnitude, demonstrating that stellar feedback is crucial to the regulation of star formation in galaxies. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1101.4940}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2011.19306.x}, -eprint = {1101.4940}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation}, -number = {2}, -pages = {950--973}, -title = {{Self-regulated star formation in galaxies via momentum input from massive stars}}, -volume = {417}, -year = {2011} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance $\Lambda$ cold dark matter cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for 'radio' feedback from those active galactic nuclei that lie at the centre of a quasi-static X-ray-emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models that might explain the accretion rate scalings required for our phenomenological 'radio mode' model to be successful. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J and Springel, Volker and White, Simon D M and {De Lucia}, G and Frenk, C S and Gao, L and Jenkins, A and Kauffmann, G and Navarro, J F and Yoshida, N}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) 'CMASS' sample at z {\$\sim${}} 0.5. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogues which include selection effects, reproduce the overall SMF, the projected two-point correlation function wp, the CMASS dn/dz, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of 'age matching' and show that these effects are markedly different compared to the ones explored by Hearin et al. at lower stellar masses. We construct two models, one in which galaxy colour is stochastic ('AbM' model) as well as a model which contains assembly bias effects ('AgM' model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colours are not a stochastic process in high-mass haloes. Our results suggest that the colours of galaxies in high-mass haloes are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P and Bundy, Kevin and Zentner, Andrew R and Behroozi, Peter S and Reid, Beth A and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L and White, Martin and Schneider, Donald P}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Cautun2015a, -abstract = {We investigate the angular and kinematic distributions of satellite galaxies around a large sample of bright isolated primaries in the spectroscopic and photometric catalogues of the Sloan Digital Sky Survey (SDSS). We detect significant anisotropy in the spatial distribution of satellites. To test whether this anisotropy could be related to the rotating discs of satellites recently found by Ibata et al. in a sample of SDSS galaxies, we repeat and extend their analysis. Ibata et al. found an excess of satellites on opposite sides of their primaries having anticorrelated radial velocities. We find that this excess is sensitive to small changes in the sample selection criteria which can greatly reduce its significance. In addition, we find no evidence for correspondingly correlated velocities for satellites observed on the same side of their primaries, which would be expected for rotating discs of satellites. We conclude that the detection of rotating planes of satellites in the observational sample of Ibata et al. is not robust to changes in the sample selection criteria. We compare our data to the $\Lambda$ cold dark matter Millennium simulations populated with galaxies according to the semi-analytic model of Guo et al. We find excellent agreement with the spatial distribution of satellites in the SDSS data and the lack of a strong signal from coherent rotation.}, -archivePrefix = {arXiv}, -arxivId = {1410.7778}, -author = {Cautun, Marius and Wang, Wenting and Frenk, Carlos S and Sawala, Till}, -doi = {10.1093/mnras/stv490}, -eprint = {1410.7778}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {3}, -pages = {2576--2587}, -title = {{A new spin on discs of satellite galaxies}}, -volume = {449}, -year = {2015} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by an internal driver and a positive feedback mechanism, which creates regular geometric and/or temporal patterns and decreases the entropy, in contrast to random processes. Here we investigate for the first time a comprehensive number of 16 self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous {\{}$\backslash$sl order out of chaos{\}}, during the evolution from an initially disordered system to an ordered stationary system, via quasi-periodic limit-cycle dynamics, harmonic mechanical resonances, or gyromagnetic resonances. The internal driver can be gravity, rotation, thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational instability, the Rayleigh-B$\backslash$'enard convection instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or loss-cone instability. Physical models of astrophysical self-organization processes involve hydrodynamic, MHD, and N-body formulations of Lotka-Volterra equation systems.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C M and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G and Scargle, Jeffrey D and Melatos, Andrew and Wagoner, Robert V and Trimble, Virginia and Green, William H}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Fassnacht1999, -abstract = {We have discovered a new gravitational lens in the Cosmic Lens All-Sky Survey (CLASS). B2045+265 is a four-image system with a maximum separation of 1.9 arcsec. A fifth radio component is detected, but its radio spectrum and its positional coincidence with infrared emission from the lensing galaxy strongly suggests that it is the radio core of the lensing galaxy. This implies that the B2045+265 system consists of a flat-spectrum radio source being lensed by another flat-spectrum radio source. Infrared images detect the lensed images of the background source and the lensing galaxy. The lensed images have relative positions and flux densities that are consistent with those seen at radio wavelengths. Spectra of the system reveal a lens redshift of z{\_}l=0.8673 and a source redshift of z{\_}s=1.28. The image splitting and system redshifts imply that the projected mass inside the Einstein radius of the lensing galaxy is M{\_}E=4.7x10{\^{}}{\{}11{\}} h{\^{}}{\{}-1{\}} M{\_}sun. An estimate of the light emitted inside the Einstein radius gives a mass-to-light ratio in the rest frame B band of (M/L{\_}B){\_}E = 20 h (M/L{\_}B){\_}sun. Both the mass and mass-to-light ratio are higher than what is seen in nearby Sa galaxies. In fact, the implied rotation velocity for the lensing galaxy is two to three times higher than what is seen in nearby spirals. The large projected mass inside the Einstein ring radius may be the result of a significant amount of dark matter in the system, perhaps from a compact group of galaxies; however, it may also arise from a misidentification of the source redshift. A simple model of the gravitational potential of the lens reproduces the image positions well, but further modeling is required to satisfy the constraints from the image flux density ratios. With further observations and modeling, this lens may yield an estimate of H{\_}0.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9811167}, -author = {Fassnacht, C D and Blandford, R D and Cohen, J G and Matthews, K and Pearson, T J and Readhead, A C S and Womble, D S and Myers, S T and Browne, I W A and Jackson, N J and Marlow, D R and Wilkinson, P N and Koopmans, L V E and de Bruyn, A G and Schilizzi, R T and Bremer, M and Miley, G}, -doi = {10.1086/300724}, -eprint = {9811167}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {COSMOLOGY: DISTANCE SCALE,COSMOLOGY: GRAVITATIONAL LENSING,GALAXIES: DISTANCES AND REDSHIFTS,GALAXIES: QUASARS: INDIVIDUAL: ALPHANUMERIC: B204}, -month = {feb}, -number = {2}, -pages = {658--670}, -pmid = {740917}, -primaryClass = {astro-ph}, -title = {{B2045+265: A New Four-Image Gravitational Lens from CLASS}}, -url = {http://arxiv.org/abs/astro-ph/9811167%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/300724}, -volume = {117}, -year = {1998} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a $\Lambda$CDM concordance cosmology. To that extent we use a large N-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as a function of halo mass and galaxy colour. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by ∼40° (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the colour of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the colour of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion. {\textcopyright} 2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X. and {Van Den Bosch}, Frank C. and Yang, Xiaohu and Mao, Shude and Mo, H. J. and Li, Cheng and Jing, Y. P.}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kang et al. - 2007 - The alignment between satellites and central galaxies Theory versus observations.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@article{Murray2013a, -abstract = {Pocket-pumping is an established technique for identifying the locations of charge trapping sites within the transport channels of CCDs. Various parameters of the pumping process can be manipulated to increase the efficiency, or allow characterisation of the trap sites effective during nominal operating modes. A CCD273 was irradiated in a triangular region by protons to a 10 MeV equivalent fluence of 1.2E9 p.cm-2, ensuring a suitably low trap density for the development of an automated trap recognition algorithm. X-rays of 5, 898 eV were incident on the CCD above the region irradiated with the triangle, such that events could be analysed having passed through an increasing length of irradiated silicon and hence number of trapping sites as a function of column number. Here we present the relationship between the number of traps identified by pocket pumping within the parallel transport channels of a CCD273 and the amount of signal that is deferred by the trapping process during readout. {\textcopyright}2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Hall, David and Holland, Andrew D}, -doi = {10.1117/12.2024826}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {SPIE Optical Engineering + Applications}, -keywords = {ccd,cic,cte,eper,euclid vis,fpr,multi-level,pocket pumping,trap pumping,tri-level}, -number = {0}, -pages = {88600H}, -title = {{The relationship between pumped traps and signal loss in buried channel CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024826}, -volume = {44}, -year = {2013} -} -@article{Stinson2013, -abstract = {We introduce the Making Galaxies In a Cosmological Context (MAGICC) programme of smoothed particle hydrodynamics simulations. We describe a parameter study of galaxy formation simulations of an L* galaxy that uses early stellar feedback combined with supernova feedback to match the stellar mass-halo mass relationship. While supernova feedback alone can reduce star formation enough to match the stellar mass-halo mass relationship, the galaxy forms too many stars before z = 2 to match the evolution seen using abundance matching. Our early stellar feedback is purely thermal and thus operates like an ultraviolet ionization source as well as providing some additional pressure from the radiation of massive, young stars. The early feedback heats gas to >106 K before cooling it to 104 K. The pressure from this hot gas creates a more extended disc and prevents more star formation prior to z = 1 than supernova feedback alone. The resulting disc galaxy has a flat rotation curve, an exponential surface brightness profile, and matches a wide range of disc scaling relationships. The disc forms from the inside-out with an increasing exponential scale length as the galaxy evolves. Overall, early stellar feedback helps to simulate galaxies that match observational results at low and high redshifts. {\textcopyright} 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1208.0002}, -author = {Stinson, G. S. and Brook, C. and Macci{\`{o}}, A. V. and Wadsley, J. and Quinn, T. R. and Couchman, H. M.P.}, -doi = {10.1093/mnras/sts028}, -eprint = {1208.0002}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Formation-galaxies,Hydrodynamics-galaxies,ISM}, -month = {jan}, -number = {1}, -pages = {129--140}, -title = {{Making galaxies in a cosmological context: The need for early stellar feedback}}, -volume = {428}, -year = {2013} -} -@article{DiCintio2014b, -abstract = {Some tumor-specific near-infrared (NIR) fluorescent dyes such as indocyanine green (ICG), IDRye800CW, and 5-aminolevulinic acid have been used clinically for detecting tumor margins or micro-cancer lesions. In this study, we evaluated the physicochemical properties of liposomally formulated phospholipid-conjugated ICG, denoted by LP-iDOPE, as a clinically translatable NIR imaging nanoparticle for brain tumors. We also confirmed its brain-tumor-specific biodistribution and its characteristics as the intra-operative NIR imaging nanoparticles for brain tumor surgery. These properties of LP-iDOPE may enable neurosurgeons to achieve more accurate identification and more complete resection of brain tumor.}, -archivePrefix = {arXiv}, -arxivId = {1404.5959}, -author = {Suganami, Akiko and Iwadate, Yasuo and Shibata, Sayaka and Yamashita, Masamichi and Tanaka, Tsutomu and Shinozaki, Natsuki and Aoki, Ichio and Saeki, Naokatsu and Shirasawa, Hiroshi and Okamoto, Yoshiharu and Tamura, Yutaka}, -doi = {10.1016/j.ijpharm.2015.10.001}, -eprint = {1404.5959}, -isbn = {0378-5173}, -issn = {18733476}, -journal = {International Journal of Pharmaceutics}, -keywords = {Brain tumor surgery,Indocyanine green (ICG),Intra-operative imaging,Liposome,Near-infrared (NIR)}, -month = {jul}, -number = {2}, -pages = {401--406}, -pmid = {26453781}, -title = {{Liposomally formulated phospholipid-conjugated indocyanine green for intra-operative brain tumor detection and resection}}, -volume = {496}, -year = {2015} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centers of typical {\$\sim${}}L* and lower-mass spheroids exhibit power law 'cusps' with {\$}\backslashbackslashSigma \backslashbackslashpropto R{\^{}}(-n){\$}, where 0.5{\textless}n{\textless}1 for radii {\$\sim${}}1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for or strongly modify the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m=1 lopsided/eccentric disk instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*({\textless}R){\textless}{\textless}M{\_}BH. When the stellar surface density profile is comparatively shallow with n{\textless}1/2, the modes cannot efficiently propagate to R=0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than n=1, the inwards propagation of eccentricity is strongly damped, suppressing inflow and bringing n down again. Together these results produce an equilibrium slope of 1/2 {\textless}n {\textless}1 in the potential of the central black hole. These physical arguments are supported by nonlinear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 < z < 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* > 1011M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J125, i814, v606 HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V. A. and Dunlop, J. S. and McLure, R. J. and Cirasuolo, M. and Buitrago, F. and Bowler, R. A.A. and Targett, T. A. and Bell, E. F. and McIntosh, D. H. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Hartley, W. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and McGrath, E. J.}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 < z < 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.1736}, -volume = {444}, -year = {2014} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and \nspectroscopic ESA cornerstone mission, currently scheduled for launch in\nlate 2011. Its primary science drivers are the composition, formation\nand evolution of the Galaxy. Gaia will not achieve its scientific\nrequirements without detailed calibration and correction for radiation\ndamage. Microscopic models of Gaia's CCDs are being developed to\nsimulate the effect of radiation damage, charge trapping, which causes\ncharge transfer inefficiency. The key to calculating the probability of\na photoelectron being captured by a trap is the 3D electron density\nwithin each CCD pixel. However, this has not been physically modelled\nfor Gaia CCD pixels. In this paper, the first of a series, we motivate\nthe need for such specialised 3D device modelling and outline how its\nfuture results will fit into Gaia's overall radiation calibration\nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Seabroke, Holland, Cropper - 2008 - Modelling radiation damage to ESA's Gaia satellite CCDs.pdf:pdf}, -isbn = {9780819472311}, -issn = {0277-786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy III}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Refregier2004, -abstract = {Effectively harvesting ambient mechanical energy is the key for realizing self-powered and autonomous electronics, which addresses limitations of batteries and thus has tremendous applications in sensor networks, wireless devices, and wearable/implantable electronics, etc. Here, a thin-film-based micro-grating triboelectric nanogenerator (MG-TENG) is developed for high-efficiency power generation through conversion of mechanical energy. The shape-adaptive MG-TENG relies on sliding electrification between complementary micro-sized arrays of linear grating, which offers a unique and straightforward solution in harnessing energy from relative sliding motion between surfaces. Operating at a sliding velocity of 10 m/s, a MG-TENG of 60 cm2 in overall area, 0.2 cm3 in volume and 0.6 g in weight can deliver an average output power of 3 W (power density of 50 mW cm-2 and 15 W cm-3) at an overall conversion efficiency of ∼50%, making it a sufficient power supply to regular electronics, such as light bulbs. The scalable and cost-effective MG-TENG is practically applicable in not only harvesting various mechanical motions but also possibly power generation at a large scale. A thin-film-based micro-grating triboelectric nanogenerator (MG-TENG) is developed for conversion of mechanical energy at an efficiency of 50%. The MG-TENG generates a power density of 50 mW/cm2 and 15 W/cm3, making it a sufficient power supply to regular electronics, such as light bulbs. The scalable and cost-effective MG-TENG is practically applicable in not only harvesting various mechanical motions but also possibly power generation at a large scale. {\textcopyright} 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0304419}, -author = {Zhu, Guang and Zhou, Yu Sheng and Bai, Peng and Meng, Xian Song and Jing, Qingshen and Chen, Jun and Wang, Zhong Lin}, -doi = {10.1002/adma.201400021}, -eprint = {0304419}, -isbn = {1521-4095}, -issn = {15214095}, -journal = {Advanced Materials}, -keywords = {energy conversion,energy generation,self-powered,triboelectric effect}, -month = {jun}, -number = {23}, -pages = {3788--3796}, -pmid = {24692147}, -primaryClass = {astro-ph}, -title = {{A shape-adaptive thin-film-based approach for 50% high-efficiency energy generation through micro-grating sliding electrification}}, -url = {http://stacks.iop.org/1538-3881/127/i=6/a=3102}, -volume = {26}, -year = {2014} -} -@article{Sales2012a, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Blumenthal1986, -abstract = {Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in. radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.}, -author = {Blumenthal, G. R. and Faber, S. M. and Flores, R. and Primack, J. R.}, -doi = {10.1086/163867}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Astronomical Models,Baryons,Galactic Evolution,Galactic Rotation,Galactic Structure,Gravitational Collapse,Halos,Interstellar Matter,Many Body Problem,Mass Distribution,Missing Mass (Astrophysics),Spiral Galaxies}, -month = {feb}, -pages = {27}, -title = {{Contraction of dark matter galactic halos due to baryonic infall}}, -volume = {301}, -year = {1986} -} -@article{Johnston2016, -abstract = {With the availability of large integral field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, howgalaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present bulge-disc decomposition of IFU data cubes (BUDDI), a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GALFITM, a modified form of GALFIT which can fit multiwaveband images simultaneously. The benefit of this technique over traditional multiwaveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the Sloan Digital Sky Survey-IV Mapping Nearby Galaxies atAPO(MaNGA)survey with redshifts z {\textless} 0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec full width at half-maximum and field of view of {\textgreater} 22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from theMaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data.}, -archivePrefix = {arXiv}, -arxivId = {1611.00609}, -author = {Johnston, Evelyn J and H{\"{a}}u{\ss}ler, Boris and Arag{\'{o}}n-Salamanca, Alfonso and Merrifield, Michael R and Bamford, Steven and Bershady, Matthew A and Bundy, Kevin and Drory, Niv and Fu, Hai and Law, David and Nitschelm, Christian and Thomas, Daniel and Lopes, Alexandre Roman and Wake, David and Yan, Renbin}, -doi = {10.1093/mnras/stw2823}, -eprint = {1611.00609}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content,Galaxies: structure}, -number = {2}, -pages = {2317--2341}, -title = {{SDSS-IV MaNGA: Bulge-disc decomposition of IFU data cubes (BUDDI)}}, -url = {http://arxiv.org/abs/1611.00609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2823}, -volume = {465}, -year = {2017} -} -@article{Pontzen2017, -abstract = {We show how the interplay between active galactic nuclei (AGNs) and merger history determines whether a galaxy quenches star formation (SF) at high redshift. We first simulate, in a full cosmological context, a galaxy of total dynamical mass Mvir = 1012M⊙ at z = 2. Then we systematically alter the accretion history of the galaxy by minimally changing the linear overdensity in the initial conditions. This 'genetic modification' approach allows the generation of three sets of $\Lambda$ CDM initial conditions leading to maximum merger ratios of 1:10, 1:5 and 2:3, respectively. The changes leave the final halo mass, large-scale structure and local environment unchanged, providing a controlled numerical experiment. Interaction between the AGN physics and mergers in the three cases leads, respectively, to a star-forming, temporarily quenched and permanently quenched galaxy. However, the differences do not primarily lie in the black hole accretion rates, but in the kinetic effects of the merger: the galaxy is resilient against AGN feedback unless its gaseous disc is first disrupted. Typical accretion rates are comparable in the three cases, falling below 0.1M⊙ yr-1, equivalent to around 2 per cent of the Eddington rate or 10-3 times the pre-quenching star formation rate, in agreement with observations. This low level of black hole accretion can be sustained even when there is insufficient dense cold gas for SF. Conversely, supernova feedback is too distributed to generate outflows in high-mass systems, and cannot maintain quenching over periods longer than the halo gas cooling time.}, -archivePrefix = {arXiv}, -arxivId = {1607.02507}, -author = {Pontzen, Andrew and Tremmel, Michael and Roth, Nina and Peiris, Hiranya V and Saintonge, Am{\'{e}}lie and Volonteri, Marta and Quinn, Tom and Governato, Fabio}, -doi = {10.1093/mnras/stw2627}, -eprint = {1607.02507}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: star formation,Galaxies: stellar content}, -number = {1}, -pages = {547--558}, -title = {{How to quench a galaxy}}, -volume = {465}, -year = {2017} -} -@article{Townsley2002, -abstract = {The front-illuminated (FI) CCDs in the Advanced CCD Imaging Spectrometer (ACIS) on the Chandra X-ray Observatory (Chandra) were damaged in the extreme environment of the Earth's radiation belts, causing charge traps that result in enhanced charge transfer inefficiency (CTI) during parallel readout. This causes row-dependent gain, event grade 'morphing' (spatial redistribution of charge) and energy resolution degradation. The ACIS back-illuminated (BI) CCDs also exhibit pronounced CTI due to their manufacturing. It is mild enough that position-dependent energy resolution is not seen, but it is present in both parallel and serial registers. This CTI also changes the gain and event grades, in a spatially complicated way as parallel and serial CTI interact. Given these realities, we have developed and tuned a phenomenological model of CTI for both FI and BI CCDs and incorporated it into our Monte Carlo simulations of the ACIS CCDs. It models charge loss and the spatial redistribution of charge (trailing), thus reproducing the spatially dependent gain and grade distribution seen in all ACIS CCDs and the row-dependent energy resolution seen in the FI devices. Here we explore the evidence for CTI, compare our simulations to data, and present a technique for CTI correction based on forward modeling. {\textcopyright} 2001 Elsevier Science B.V. All Rights Reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0111031}, -author = {Townsley, L. K. and Broos, P. S. and Nousek, J. A. and Garmire, G. P.}, -doi = {10.1016/S0168-9002(01)02156-8}, -eprint = {0111031}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Townsley et al. - 2002 - Modeling charge transfer inefficiency in the Chandra Advanced CCD Imaging Spectrometer.pdf:pdf}, -issn = {01689002}, -journal = {Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment}, -keywords = {CCD,Charge transfer inefficiency,Monte Carlo simulation}, -number = {3}, -pages = {751--784}, -primaryClass = {astro-ph}, -title = {{Modeling charge transfer inefficiency in the Chandra Advanced CCD Imaging Spectrometer}}, -volume = {486}, -year = {2002} -} -@article{Weijmans2014, -abstract = {We use the ATLAS3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation $\sigma$q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and $\sigma$q = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrizations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P T and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F and Davies, Roger L and Davis, Timothy A and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular,Galaxies,Structure,cD- galaxies}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Yan2016, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R{\$\sim${}}2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is {\$\sim${}}73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R and Bershady, Matthew A and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R and Thomas, Daniel and Wake, David A and Weijmans, Anne-Marie and Westfall, Kyle B and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A and Blanton, Michael R and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T and Goddard, Daniel and Gunn, James E and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R and Oravetz, Daniel and Pan, Kaike and Parejko, John K and Sanchez, Sebastian F and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {6}, -pages = {197}, -title = {{SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY}}, -url = {http://arxiv.org/abs/1607.08613%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {152}, -year = {2016} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Read2005, -abstract = {Dwarf spheroidal galaxies have shallow central dark matter density profiles, low angular momentum and approximately exponential surface brightness distributions. Through N-body simulations and analytic calculations we investigate the extent to which these properties can be generated from 'typical' ACDM galaxies, which differ in all of these properties, by the dynamical consequences of feedback. We find that, for a wide range of initial conditions, one impulsive mass-loss event will naturally produce a surface brightness profile in the remaining stellar component of a dwarf spheroidal galaxy (dSph) which is well-fitted over many scalelengths by an exponential, in good qualitative agreement with observations of Local Group dSphs. Furthermore, two impulsive mass-loss phases, punctuated by significant gas re-accretion, are found to be sufficient to transform a central density cusp in the dark matter profile into a near-constant density core. This may then provide the missing link between current cosmological simulations, which predict a central cusp in the dark matter density profile, and current observations, which find much shallower central density profiles. We also look at the angular momentum history of dSphs and demonstrate that if these galaxies have spent most of their lifetime in tidal isolation from massive galaxies then they cannot have formed from high angular momentum gas discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0409565}, -author = {Read, J. I. and Gilmore, G.}, -doi = {10.1111/j.1365-2966.2004.08424.x}, -eprint = {0409565}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Evolution,Galaxies,Galaxies: dwarf,Galaxies: haloes,Galaxies: kinematics and dynamics,Galaxies: structure}, -month = {jan}, -number = {1}, -pages = {107--124}, -primaryClass = {astro-ph}, -title = {{Mass loss from dwarf spheroidal galaxies: The origins of shallow dark matter cores and exponential surface brightness profiles}}, -volume = {356}, -year = {2005} -} -@article{Li2017, -abstract = {We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier $\rm ATLAS^{3D}$ results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients.}, -archivePrefix = {arXiv}, -arxivId = {1703.04894}, -author = {Li, Hongyu and Ge, Junqiang and Mao, Shude and Cappellari, Michele and Long, R. J. and Li, Ran and Emsellem, Eric and Dutton, Aaron A. and Li, Cheng and Bundy, Kevin and Thomas, Daniel and Drory, Niv and Lopes, Alexandre Roman}, -doi = {10.3847/1538-4357/aa662a}, -eprint = {1703.04894}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Li et al. - 2017 - SDSS-IV MaNGA Variation of the Stellar Initial Mass Function in Spiral and Early-type Galaxies.pdf:pdf}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {77}, -title = {{SDSS-IV MaNGA: Variation of the Stellar Initial Mass Function in Spiral and Early-type Galaxies}}, -url = {http://arxiv.org/abs/1703.04894%0Ahttp://dx.doi.org/10.3847/1538-4357/aa662a}, -volume = {838}, -year = {2017} -} -@article{Krajnovic2013, -abstract = {We analyse the morphological structures in galaxies of the ATLAS3D sample by fitting a single S{\'{e}}rsic profile and decomposing all non-barred objects (180 of 260 objects) in two components parametrized by an exponential and a general S{\'{e}}rsic function. The aim of this analysis is to look for signatures of discs in light distributions of nearby early-type galaxies and compare them to kinematic properties. Using S{\'{e}}rsic index from single-component fits for a distinction between slow and fast rotators, or even late- and early-type galaxies, is not recommended. Assuming that objects with n > 3 are slow rotators (or ellipticals), there is only a 22 per cent probability to correctly classify objects as slow rotators (or 37 per cent of previously classified as ellipticals). We show that exponential sub-components, as well as light profiles fitted with only a single component of a low S{\'{e}}rsic index, can be linked with the kinematic evidence for discs in early-type galaxies. The median disc-to-total light ratio for fast and slow rotators is 0.41 and 0.0, respectively. Similarly, the median S{\'{e}}rsic indices of the bulge (general S{\'{e}}rsic component) are 1.7 and 4.8 for fast and slow rotators, respectively. Overall, discs or disc-like structures are present in 83 per cent of early-type galaxies which do not have bars, and they show a full range of disc-to-total light ratios. Discs in early-type galaxies contribute with about 40 per cent to the total mass of the analysed (non-barred) objects. The decomposition into discs and bulges can be used as a rough approximation for the separation between fast and slow rotators, but it is not a substitute, as there is only a 59 per cent probability to correctly recognize slow rotators. We find trends between the angular momentum and the disc-to-total light ratios and the S{\'{e}}rsic index of the bulge, in the sense that high angular momentum galaxies have large disc-to-total light ratios and small bulge indices, but there is none between the angular momentum and the global S{\'{e}}rsic index. We investigate the inclination effects on the decomposition results and confirm that strong exponential profiles can be distinguished even at low inclinations, but medium-size discs are difficult to quantify using photometry alone at inclinations lower than ∼50°. Kinematics (i.e. projected angular momentum) remains the best approach to mitigate the influence of the inclination effects.We also find weak trends with mass and environmental density, where disc-dominated galaxies are typically less massive and found at all densities, including the densest region sampled by the ATLAS3D sample. {\textcopyright} 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1210.8167}, -author = {Krajnovi{\'{c}}, Davor and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Emsellem, Eric and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1093/mnras/sts315}, -eprint = {1210.8167}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Krajnovi{\'{c}} et al. - 2013 - The ATLAS3D project - XVII. Linking photometric and kinematic signatures of stellar discs in early-type galaxi.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: bulges,Galaxies:elliptical and lenticular,Galaxies:kinematics and dynamics,Galaxies:structure,cD}, -number = {3}, -pages = {1768--1795}, -title = {{The ATLAS3D project - XVII. Linking photometric and kinematic signatures of stellar discs in early-type galaxies}}, -volume = {432}, -year = {2013} -} -@article{Vika2014, -abstract = {Bulge-disc decomposition is a valuable tool for understanding galaxies. However, achieving robust measurements of component properties is difficult, even with high-quality imaging, and it becomes even more so with the imaging typical of large surveys. In this paper, we consider the advantages of a new, multiband approach to galaxy fitting. We perform automated bulge-disc decompositions for 163 nearby galaxies, by simultaneously fitting multiple images taken in five photometric filters. We show that we are able to recover structural measurements that agree well with various other works, and confirm a number of key results. We additionally use our results to illustrate the link between total S{\'{e}}rsic index and bulge-disc structure, and demonstrate that the visually classification of lenticular galaxies is strongly dependent on the inclination of their disc component. By simulating the same set of galaxies as they would appear if observed at a range of redshifts, we are able to study the behaviour of bulge-disc decompositions as data quality diminishes. We examine how our multiband fits perform, and compare to the results of more conventional, single-band methods.Multiband fitting improves the measurement of all parameters, but particularly the bulge-to-total flux ratio and component colours. We therefore encourage the use of this approach with future surveys.}, -archivePrefix = {arXiv}, -arxivId = {1408.4070}, -author = {Vika, Marina and Bamford, Steven P. and H{\"{a}}u{\ss}ler, Boris and Rojas, Alex L.}, -doi = {10.1093/mnras/stu1696}, -eprint = {1408.4070}, -isbn = {978-054-922-7717717}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure,Methods: data analysis,Techniques: image processing}, -month = {nov}, -number = {4}, -pages = {3603--3621}, -pmid = {11747826}, -title = {{MegaMorph - multiwavelength measurement of galaxy structure: Physically meaningful bulge-disc decomposition of galaxies near and far}}, -volume = {444}, -year = {2014} -} -@article{Shu2015, -abstract = {We present observational results from a new Hubble Space Telescope (HST) Snapshot program to extend the methods of the Sloan Lens ACS (SLACS) Survey to lower lens-galaxy masses. We discover 40 new galaxy-scale strong lenses, which we supplement with 58 previously discovered SLACS lenses. In addition, we determine the posterior PDFs of the Einstein radius for 33 galaxies (18 new and 15 from legacy SLACS data) based on single lensed images. We find a less-than-unity slope of 0.64 ± 0.06 for the - relation, which corresponds to a 6$\sigma$ evidence that the total mass-density profile of early-type galaxies varies systematically in the sense of being shallower at higher lens-galaxy velocity dispersions. The trend is only significant when single-image systems are considered, highlighting the importance of including both "lenses" and "nonlenses" for an unbiased treatment of the lens population when extending to lower mass ranges. By scaling simple stellar-population models to the HST I-band data, we identify a strong trend of increasing dark-matter fraction at higher velocity dispersions, which can be alternatively interpreted as a trend in the stellar initial mass function (IMF) normalization. Consistent with previous findings and the suggestion of a nonuniversal IMF, we find that a Salpeter IMF is ruled out for galaxies with velocity dispersion less than 180 km s-1. Considered together, our mass-profile and dark-matter fraction trends with increasing galaxy mass could both be explained by an increasing relative contribution on kiloparsec scales from a dark-matter halo with a spatial profile more extended than that of the stellar component.}, -archivePrefix = {arXiv}, -arxivId = {1407.2240}, -author = {Shu, Yiping and Bolton, Adam S. and Brownstein, Joel R. and Montero-Dorta, Antonio D. and Koopmans, L{\'{e}}on V.E. and Treu, Tommaso and Gavazzi, Rapha{\"{e}}l and Auger, Matthew W. and Czoske, Oliver and Marshall, Philip J. and Moustakas, Leonidas A.}, -doi = {10.1088/0004-637X/803/2/71}, -eprint = {1407.2240}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Shu2012SLACSXII.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {Dark matter,Galaxies: Evolution,Gravitational lensing: Strong,Methods: Statistical,Techniques: Image processing}, -number = {2}, -pages = {1--17}, -publisher = {IOP Publishing}, -title = {{The Sloan Lens ACS survey. XII. Extending strong lensing to lower masses}}, -url = {http://dx.doi.org/10.1088/0004-637X/803/2/71}, -volume = {803}, -year = {2015} -} -@article{Piontek2009, -abstract = {We present a systematic study of stellar feedback processes in simulations of disc galaxy formation. Using a dark matter halo with properties similar to the ones for the Milky Way's stellar halo, we perform a comparison of different methods of distributing energy related to feedback processes to the surrounding gas. A most promising standard model is applied to haloes spanning a range of masses in order to compare the results to disc galaxy scaling relations. With few exceptions we find little or no angular momentum deficiency for our galaxies and a good agreement with the angular momentum-size relation. Our galaxies are in good agreement with the baryonic Tully-Fisher relation and the slope of the photometric Tully-Fisher relation is reproduced. We find a zero-point offset of 0.7-1 mag, depending on the employed IMF. Applying the standard model to Milky Way-type haloes with different assembly histories, we show that a quiet assembly history does not guarantee the formation of a disc. We also study our standard feedback model in combination with additional physical processes like a UV background, kinetic feedback, a delayed energy deposition as expected for type Ia supernovae, mass return and metal-dependent cooling. Only a combination of effects yields a real improvement of the resulting galaxy by reducing the bulge, while including metal-dependent cooling increases the bulge again. We find that in general the stellar mass fraction of our galaxies is too high. In an ad hoc experiment we show that an removal of the bulge could reconcile this. However, the fit of the Tully-Fisher relation can only be improved by delaying the star formation, but not suppressing it completely. Our models do not seem to be efficient enough to achieve either effect. A mechanism to create bulge-less disc galaxies in simulations therefore remains elusive. We conclude that disc formation is a complex, highly interconnected problem that is difficult to handle in a controlled manner. We expect a solution to be coming from a combination of small effects rather than one large breakthrough. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0909.4167}, -author = {Piontek, Franziska and Steinmetz, Matthias}, -doi = {10.1111/j.1365-2966.2010.17637.x}, -eprint = {0909.4167}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: spiral,Galaxies: structure,Hydrodynamics,Methods: numerical}, -number = {4}, -pages = {2625--2642}, -title = {{The modelling of feedback processes in cosmological simulations of disc galaxy formation}}, -url = {http://arxiv.org/abs/0909.4156}, -volume = {410}, -year = {2011} -} -@article{Greco2017, -abstract = {We present a catalog of extended low-surface-brightness galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first {\$}{\{}\backslashsim{\}}{\$}200 deg{\$}{\^{}}2{\$} of the survey, we have uncovered 781 LSBGs, spanning red ({\$}g-i\backslashgeq0.64{\$}) and blue ({\$}g-i{\textless}0.64{\$}) colors and a wide range of morphologies. Since we focus on extended galaxies ({\$}r{\_}\backslashmathrm{\{}eff{\}}=2.5{\$}-{\$}14{\^{}}{\{}\backslashprime\backslashprime{\}}{\$}), our sample is likely dominated by low-redshift objects. We define LSBGs to have mean surface brightnesses {\$}\backslashbar{\{}\backslashmu{\}}{\_}\backslashmathrm{\{}eff{\}}(g){\textgreater}24.3{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, which allows nucleated galaxies into our sample. As a result, the central surface brightness distribution spans a wide range of {\$}\backslashmu{\_}0(g)=18{\$}-{\$}27.4{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, with 50{\%} and 95{\%} of galaxies fainter than 24.3 and 22 mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, respectively. Furthermore, the surface brightness distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well-characterized by single-component S$\backslash$'{\{}e{\}}rsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We crossmatch our sample with existing optical, HI, and ultraviolet catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, ranging from dwarf spheroidals and ultra-diffuse galaxies in nearby groups to gas-rich irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the LSBG population.}, -archivePrefix = {arXiv}, -arxivId = {1709.04474}, -author = {Greco, Johnny P and Greene, Jenny E and Strauss, Michael A and MacArthur, Lauren A and Flowers, Xzavier and Goulding, Andy D and Huang, Song and Kim, Ji Hoon and Komiyama, Yutaka and Leauthaud, Alexie and Leisman, Lukas and Lupton, Robert H and Sif{\'{o}}n, Crist{\'{o}}bal and Wang, Shiang-Yu}, -doi = {10.3847/1538-4357/aab842}, -eprint = {1709.04474}, -issn = {15384357}, -keywords = {dwarf,galaxies,general,keywords}, -title = {{Illuminating Low-Surface-Brightness Galaxies with the Hyper Suprime-Cam Survey}}, -url = {http://arxiv.org/abs/1709.04474%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aab842}, -year = {2017} -} -@article{Wang2018b, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}} \backslashleqslant M{\_}{\{}\backslashast{\}} \backslashleqslant 10{\^{}}{\{}11.9{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashlangle\backslashgamma{\^{}}{\{}\backslashprime{\}}\backslashrangle = 2.003 \backslashpm 0.008{\$} and a standard deviation of {\$}\backslashsigma{\_}{\{}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashgamma{\_}{\{}\backslashmathrm{\{}mw{\}}{\}}{\^{}}{\{}\backslashprime{\}}-f{\_}{\{}\backslashmathrm{\{}DM{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -keywords = {cd,elliptical and lenticular,evolution,formation,galaxies,kine-,matics and dynamics,stellar content}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -year = {2018} -} -@article{James2018, -abstract = {We present the first spatially resolved rest-frame ultraviolet (UV) study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z = 2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each {\$\sim${}}4-8 kpc2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with C III] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. Themapped C III] emission shows distinct kinematical structure, with velocity offsets of {\$\sim${}}±50 km s-1 between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionization parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing in the range -200 ≲ v (km s-1) ≲ -50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star formation rates remain relatively constant ({\$\sim${}}8-16M⊙ yr-1), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced.We measure electron densities with a range of log (Ne)= 3.92-4.36 cm-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large-scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially resolved rest-frame UV studies expected with future observatories, such as James Webb Space Telescope.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L and Auger, Matt and Pettini, Max and Stark, Daniel P and Belokurov, V and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Shao2016, -abstract = {The spatial distribution of the satellite populations of the Milky Way and Andromeda are puzzling in that they are nearly perpendicular to the disks of their central galaxies. To understand the origin of such configurations we study the alignment of the central galaxy, satellite system and dark matter halo in the largest of the "Evolution and Assembly of GaLaxies and their Environments" (EAGLE) simulation. We find that centrals and their satellite systems tend to be well aligned with their haloes, with a median misalignment angle of {\$}33{\^{}}{\{}\backslashbackslashcirc{\{}\backslash{\}}{\}}{\$} in both cases. While the centrals are better aligned with the inner {\$}10{\$} kpc halo, the satellite systems are better aligned with the entire halo indicating that satellites preferentially trace the outer halo. The central - satellite alignment is weak (median misalignment angle of {\$}52{\^{}}{\{}\backslashbackslashcirc{\{}\backslash{\}}{\}}{\$}) and we find that around {\$}20\backslashbackslash{\{}\backslash{\%}{\}}{\$} of systems have a misalignment angle larger than {\$}78{\^{}}{\{}\backslashbackslashcirc{\{}\backslash{\}}{\}}{\$}, which is the value for the Milky Way. The central - satellite alignment is a consequence of the tendency of both components to align with the dark matter halo. As a consequence, when the central is parallel to the satellite system, it also tends to be parallel to the halo. In contrast, if the central is perpendicular to the satellite system, as in the case of the Milky Way and Andromeda, then the central - halo alignment is much weaker. Dispersion-dominated (spheroidal) centrals have a stronger alignment with both their halo and their satellites than rotation-dominated (disk) centrals. We also found that the halo, the central galaxy and the satellite system tend to be aligned with the surrounding large-scale distribution of matter, with the halo being the better aligned of the three.}, -archivePrefix = {arXiv}, -arxivId = {1605.01728}, -author = {Shao, Shi and Cautun, Marius and Frenk, Carlos S and Gao, Liang and Crain, Robert A and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw1247}, -eprint = {1605.01728}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3772--3783}, -title = {{Alignments between galaxies, satellite systems and haloes}}, -volume = {460}, -year = {2016} -} -@article{Alexander2019, -abstract = {Dark matter substructure has the potential to discriminate between broad classes of dark matter models. With this in mind, we construct novel solutions to the equations of motion governing condensate dark matter candidates, namely axion Bose-Einstein condensates and superfluids. These solutions are highly compressed along one axis and thus have a disk-like geometry. We discuss linear stability of these solutions, consider the astrophysical implications as a large-scale dark disk or as small scale substructure, and find a characteristic signal in strong gravitational lensing. This adds to the growing body of work that indicates that the morphology of dark matter substructure is a powerful probe of the nature of dark matter.}, -archivePrefix = {arXiv}, -arxivId = {1901.03694}, -author = {Alexander, Stephon and Bramburger, Jason J and McDonough, Evan}, -doi = {10.1016/j.physletb.2019.134871}, -eprint = {1901.03694}, -issn = {03702693}, -journal = {Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics}, -pages = {1--7}, -title = {{Dark disk substructure and superfluid dark matter}}, -url = {http://arxiv.org/abs/1901.03694}, -volume = {797}, -year = {2019} -} -@article{Greene2017, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, Jenny E and Leauthaud, Alexie and Emsellem, Eric and Ge, J and Arag'on-Salamanca, A and Greco, J P and Lin, Y -T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -pages = {1--23}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -year = {2017} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as ‘notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude (≤50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 ≤ G ≤ 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G M and Prod'homme, T and Murray, N J and Crowley, C and Hopkinson, G and Brown, A G A and Kohley, R and Holland, A}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Hsu2018, -abstract = {We present a new framework to characterize the occurrence rates of planet candidates identified by Kepler based on hierarchical Bayesian modeling, Approximate Bayesian Computing (ABC), and sequential importance sampling. For this study we adopt a simple 2-D grid in planet radius and orbital period as our model and apply our algorithm to estimate occurrence rates for Q1-Q16 planet candidates orbiting around solar-type stars. We arrive at significantly increased planet occurrence rates for small planet candidates ({\$}R{\_}p{\textless}1.25 R{\_}{\{}\backslashoplus{\}}{\$}) at larger orbital periods ({\$}P{\textgreater}80{\$}d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is {\$}1.6{\^{}}{\{}+1.2{\}}{\_}{\{}-0.5{\}}{\$} per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2{\$}R{\_}{\{}\backslashoplus{\}}{\$} that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C and Ford, Eric B and Ragozzine, Darin and Morehead, Robert C}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -issn = {0004-6256}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -title = {{Improving the Accuracy of Planet Occurrence Rates from Kepler using Approximate Bayesian Computation}}, -url = {http://arxiv.org/abs/1803.10787%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -year = {2018} -} -@article{Li2016a, -abstract = {The defining characteristic of the cold dark matter (CDM) hypothesis is the presence of a very large number of low-mass haloes, too small to have made a visible galaxy. Other hypotheses for the nature of the dark matter, such as warm dark matter (WDM), predict a much smaller number of such low-mass haloes. Strong lensing systems offer the possibility of detecting small-mass haloes through the distortions they induce in the lensed image. Here, we show that the main contribution to the image distortions comes from haloes along the line of sight rather than subhaloes in the lens as has normally been assumed so far. These interlopers enhance the differences between the predictions of CDM and WDM models. We derive the total perturber mass function, including both subhaloes and interlopers, and show that measurements of approximately 20 strong lens systems with a detection limit of Mlow = 107 h−1 M☉ would distinguish (at 3$\sigma$) between CDM and a WDM model consisting of 7 keV sterile neutrinos such as those required to explain the recently detected 3.5 keV X-ray emission line from the centres of galaxies and clusters.}, -archivePrefix = {arXiv}, -arxivId = {1612.06227}, -author = {Li, Ran and Frenk, Carlos S. and Cole, Shaun and Wang, Qiao and Gao, Liang}, -doi = {10.1093/mnras/stx554}, -eprint = {1612.06227}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Li et al. - 2017 - Projection effects in the strong lensing study of subhaloes.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: haloes,Gravitational lensing: strong}, -number = {2}, -pages = {1426--1432}, -title = {{Projection effects in the strong lensing study of subhaloes}}, -url = {http://arxiv.org/abs/1612.06227%0Ahttp://dx.doi.org/10.1093/mnras/stx554}, -volume = {468}, -year = {2017} -} -@article{Krist2004a, -author = {Krist, John and Hook, Richard and Tim, Tiny}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Krist, Hook, Tim - 2004 - The Tiny Tim User ' s Guide.pdf:pdf}, -journal = {Changes}, -number = {June}, -pages = {1--35}, -title = {{The Tiny Tim User ' s Guide}}, -url = {http://tinytim.stsci.edu/static/tinytim.pdf%5Cnpapers2://publication/uuid/994E8BF5-B9AC-489B-A26F-2AE8BC664FEE}, -year = {2004} -} -@article{Cooper2010, -abstract = {Objective: To establish the relationship between the complexity of treatment for hepatitis C and patient satisfaction. Method: An observational, prospective, single-center study, which included HCV patients treated between October 2014 and February 2016. The primary endpoint was the assessment of satisfaction with treatment, measured by the HCV-ESTAR questionnaire, structured into two dimensions: clinical and lifestyle satisfaction, on a 0-60 score. A reliability analysis was performed. The data collected were: treatment prescribed for HCV, concomitant medication, and Sustained Viral Response. The complexity index of the complete pharmacotherapy was calculated by the computer application MRCI. T-Student was used to identify the complexity of treatment as a marker of dissatisfaction. Results: The study included 171 patients (83.0{\%} male). The mean satisfaction score was 47.9±7.5. The reliability of the complete questionnaire was high (Cronbach alpha, 0.864; intraclass coefficient, 0.843). There was correlation between the Complexity Index and satisfaction (P{\textless}0.05). A reduction of 5 points in the Complexity Index increased fourfold the value of satisfaction with treatment (p{\textless}0.0001). Similarly, a reduction in 12 points in the Concomitant Medication Index doubled the satisfaction (p=0.028). Regarding the overall complexity, 10 points less doubled the satisfaction (p{\textless}0.05). Finally, patients with higher values of satisfaction presented a higher response rate (p=0.029).}, -archivePrefix = {arXiv}, -arxivId = {0910.3211}, -author = {{De Las Aguas Robustillo Cort{\'{e}}s}, Mar{\'{i}}a and Gonz{\'{a}}lez, Carmen Victoria Almeida and Verdugo, Ram{\'{o}}n Morillo}, -doi = {10.7399/fh.2017.41.4.10701}, -eprint = {0910.3211}, -isbn = {9780735407862}, -issn = {21718695}, -journal = {Farmacia Hospitalaria}, -keywords = {Hepatitis C,Medication complexity index,Pharmaceutical care,Satisfaction}, -number = {4}, -pages = {470--478}, -pmid = {26086087}, -title = {{Relationship between pharmacotherapy complexity and patient satisfaction with treatment for hepatitis C}}, -volume = {41}, -year = {2017} -} -@article{Lacki2014, -abstract = {Star-forming galaxies could be major contributors to the cosmic GeV $\gamma$-ray background, and they are expected to be MeV-dim because of the "pion bump" falling off below ∼100 MeV. However, there are very few observations of galaxies in the MeV range and other emission processes could be present. We investigate the MeV background from star-forming galaxies by running one-zone models of cosmic ray populations, including inverse Compton and bremsstrahlung, as well as nuclear lines (including 26Al), emission from core-collapse supernovae, and positron annihilation emission, in addition to the pionic emission. We use the Milky Way and M82 as templates of normal and starburst galaxies and compare our models to radio and GeV-TeV $\gamma$-ray data. We find that (1) higher gas densities in high-z normal galaxies lead to a strong pion bump, (2) starbursts may have significant MeV emission if their magnetic field strengths are low, and (3) cascades can contribute to the MeV emission of starbursts if they emit mainly hadronic $\gamma$-rays. Our fiducial model predicts that most of the unresolved GeV background is from star-forming galaxies, but this prediction is uncertain by an order of magnitude. About ∼2% of the claimed 1 MeV background is diffuse emission from star-forming galaxies; we place a firm upper limit of ≲ 10% based on the spectral shape of the background. The star formation contribution is constrained to be small because its spectrum is peaked, while the observed background is steeply falling with energy through the MeV-GeV range. {\textcopyright} 2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1206.0772}, -author = {Lacki, Brian C. and Horiuchi, Shunsaku and Beacom, John F.}, -doi = {10.1088/0004-637X/786/1/40}, -eprint = {1206.0772}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmic rays,galaxies: starburst,gamma rays: diffuse background,gamma rays: galaxies}, -number = {1}, -pages = {40}, -title = {{The star-forming galaxy contribution to the cosmic MeV and GeV gamma-ray background}}, -url = {http://stacks.iop.org/0004-637X/786/i=1/a=40?key=crossref.c81353df05b3cd5fe566d21d49012eb8}, -volume = {786}, -year = {2014} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter (CDM) galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes possess a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a $\Lambda$CDM universe. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R. and Eke, Vincent R. and Frenk, Carlos S. and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lovell et al. - 2011 - The link between galactic satellite orbits and subhalo accretion(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{Blei2017a, -abstract = {One of the core problems of modern statistics is to approximate difficult-to-compute probability densities. This problem is especially important in Bayesian statistics, which frames all inference about unknown quantities as a calculation involving the posterior density. In this article, we review variational inference (VI), a method from machine learning that approximates probability densities through optimization. VI has been used in many applications and tends to be faster than classical methods, such as Markov chain Monte Carlo sampling. The idea behind VI is to first posit a family of densities and then to find a member of that family which is close to the target density. Closeness is measured by Kullback–Leibler divergence. We review the ideas behind mean-field variational inference, discuss the special case of VI applied to exponential family models, present a full example with a Bayesian mixture of Gaussians, and derive a variant that uses stochastic optimization to scale up to massive data. We discuss modern research in VI and highlight important open problems. VI is powerful, but it is not yet well understood. Our hope in writing this article is to catalyze statistical research on this class of algorithms. Supplementary materials for this article are available online.}, -archivePrefix = {arXiv}, -arxivId = {1601.00670}, -author = {Blei, David M. and Kucukelbir, Alp and McAuliffe, Jon D.}, -doi = {10.1080/01621459.2017.1285773}, -eprint = {1601.00670}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Blei, Kucukelbir, McAuliffe - 2017 - Variational Inference A Review for Statisticians.pdf:pdf}, -issn = {1537274X}, -journal = {Journal of the American Statistical Association}, -keywords = {Algorithms,Computationally intensive methods,Statistical computing}, -number = {518}, -pages = {859--877}, -title = {{Variational Inference: A Review for Statisticians}}, -volume = {112}, -year = {2017} -} -@article{Geometryem, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M{\textless}inf{\textgreater}*{\textless}/inf{\textgreater} {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M{\textless}inf{\textgreater}⊙{\textless}/inf{\textgreater} galaxies at 1 {\textless} z {\textless} 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 {\textless} z {\textless} 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{Cappellari2011, -abstract = {The Atlas3D project is a multi-wavelength survey combined with a theoretical modeling effort. The observations span from the radio to the millimeter and optical, and provide multi-colour imaging, two-dimensional kinematics of the atomic (HI), molecular (CO) and ionized gas (Hbeta, [OIII] and [NI]), together with the kinematics and population of the stars (Hbeta, Fe5015 and Mgb), for a carefully selected, volume-limited (1.16*10{\^{}}5 Mpc{\^{}}3) sample of 260 early-type (elliptical E and lenticular S0) galaxies (ETGs). The models include semi-analytic, N-body binary mergers and cosmological simulations of galaxy formation. Here we present the science goals for the project and introduce the galaxy sample and the selection criteria. The sample consists of nearby (D{\textless}42 Mpc) morphologically-selected ETGs extracted from a parent sample of 871 galaxies (8{\%} E, 22{\%} S0 and 70{\%} spirals) brighter than M{\_}K{\textless}-21.5 mag (stellar mass M{\_}Star{\textgreater}6*10{\^{}}9 M{\_}Sun). We analyze possible selection biases and we conclude that the parent sample is essentially complete and statistically representative of the nearby galaxy population. We present the size-luminosity relation for the spirals and ETGs and show that the ETGs in the Atlas3D sample define a tight red sequence in a colour-magnitude diagram, with few objects in the transition from the blue cloud. We describe the strategy of the SAURON integral-field observations and the extraction of the stellar kinematics with the pPXF method. We give an overview of the characteristics of the other main datasets already available for our sample and of the ongoing modelling projects.}, -archivePrefix = {arXiv}, -arxivId = {1012.1551}, -author = {Cappellari, Michele and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Mcdermid, Richard M and Scott, Nicholas and {Verdoes Kleijn}, G A and Young, Lisa M and Alatalo, Katherine and Bacon, R and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M and Davies, Roger L and Davis, Timothy A and de Zeeuw, P T and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and Lablanche, Pierre Yves and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Serra, Paolo and Weijmans, Anne Marie}, -doi = {10.1111/j.1365-2966.2010.18174.x}, -eprint = {1012.1551}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: distances and redshifts,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {2}, -pages = {813--836}, -title = {{The ATLAS 3D project - I. A volume-limited sample of 260 nearby early-type galaxies: Science goals and selection criteria}}, -volume = {413}, -year = {2011} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR {\$}\backslashbackslasheta(z){\$} using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of {\$}102{\$} SGL with the measurement of corresponding velocity dispersion {\$}\backslashbackslashsigma{\{}\backslash{\_}{\}}0{\$} and Einstein radius {\$}\backslashbackslashtheta{\{}\backslash{\_}{\}}E{\$}. In addition, we also use a dataset of {\$}12{\$} two image lensing systems containing the measure of time delay {\$}\backslashbackslashDelta t{\$} between source images. Jointly these two datasets give us the angular diameter distance {\$}D{\_}{\{}A{\_}{\{}ol{\}}{\}}{\$} of the lens. Further, for luminosity distance, we use the {\$}740{\$} observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ({\$}\backslashbackslasheta=1{\$}) within {\$}2\backslashbackslashsigma{\{}\backslash{\$}{\}} confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R F L}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@inproceedings{Grogin2010b, -author = {Grogin, N A and Lim, P L and Maybhate, A and Hook, R N and Loose, M}, -booktitle = {2010 HST Calibration Workshop}, -month = {jul}, -pages = {1--12}, -title = {{Post-SM4 ACS / WFC Bias Striping : Characterization And Mitigation}}, -year = {2010} -} -@article{Fergus2014, -abstract = {High dynamic range imagers aim to block or eliminate light from a very bright primary star in order to make it possible to detect and measure far fainter companions; in real systems, a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronagraph. The model uses principal components analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles, but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of the order of a percent of the brightness of the speckles, or up to 10-7 times the brightness of the primary star. This outperforms existing methods by a factor of two to three and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Tenneti2016, -abstract = {We study the shapes and intrinsic alignments of discs and elliptical galaxies in the MassiveBlack-II (MBII) and Illustris cosmological hydrodynamic simulations, with volumes of (100 h-1 Mpc)3and (75 h-1 Mpc)3, respectively. We find that simulated disc galaxies are more oblate in shape and more misaligned with the shape of their host dark matter subhalo when compared with ellipticals. The discmajor axis is found to be oriented towards the location of nearby elliptical galaxies. We also find that the discs are thinner in MBII and misalignments with dark matter halo orientations are smaller in both discs and ellipticals when compared with Illustris. As a result, the intrinsic alignment correlation functions at fixed mass have a higher amplitude in MBII than in Illustris. Finally, at scales above {\$\sim${}}0.1 h-1 Mpc, the intrinsic alignment two-point correlation functions for disc galaxies in both simulations are consistent with a null detection, unlike those for ellipticals. Despite significant differences in the treatments of hydrodynamics and baryonic physics in the simulations, we find that the w$\delta$ + correlation function scales similarly with transverse separation. However, the less massive galaxies show different scale dependence in the ellipticity-direction correlation. This result indicates that, while hydrodynamic simulations are a promising tool to study intrinsic alignments, further study is needed to understand the impact of differences in the implementations of hydrodynamics and baryonic feedback.}, -archivePrefix = {arXiv}, -arxivId = {1510.07024}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana}, -doi = {10.1093/mnras/stw1823}, -eprint = {1510.07024}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies,Gravitational lensing: weak,Hydrodynamics,Kinematics and dynamics,Methods,Numerical}, -number = {3}, -pages = {2668--2680}, -title = {{Intrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris simulations}}, -volume = {462}, -year = {2016} -} -@article{Cole2011, -abstract = {We consider the infall of a massive clump into a dark matter halo as a simple and extreme model for the effect of baryonic physics (neglected in gravity-only simulations of large-scale structure formation) on the dark matter. We find that such an infalling clump is extremely efficient in altering the structure of the halo and reducing its central density: a clump of 1 per cent the mass of the halo can remove about twice its own mass from the inner halo and transform a cusp into a core or weaker cusp. If the clump is subsequently removed, mimicking a galactic wind, the central halo density is further reduced and the mass removed from the inner halo doubled. Lighter clumps are even more efficient: the ratio of removed mass to clump mass increases slightly towards smaller clump masses. This process becomes more efficient the more radially anisotropic the initial dark matter velocities are. While such a clumpy infall may be somewhat unrealistic, it demonstrates that the baryons need to transfer only a small fraction of their initial energy to the dark matter via dynamical friction to explain the discrepancy between predicted dark matter density profiles and those inferred from observations of dark-matter-dominated galaxies. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1105.4050}, -author = {Cole, David R. and Dehnen, Walter and Wilkinson, Mark I.}, -doi = {10.1111/j.1365-2966.2011.19110.x}, -eprint = {1105.4050}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxies: haloes,Galaxies: kinematics and dynamics,Galaxies: structure}, -month = {sep}, -number = {2}, -pages = {1118--1134}, -title = {{Weakening dark matter cusps by clumpy baryonic infall}}, -volume = {416}, -year = {2011} -} -@article{Barrufet2023, -abstract = {Over the last few years, both Atacama Large Millimeter/submillimeter Array (ALMA) and Spitzer observations have revealed a population of likely massive galaxies at z > 3 that was too faint to be detected in Hubble Space Telescope (HST) rest-frame ultraviolet imaging. However, due to the very limited photometry for individual galaxies, the true nature of these so-called HSTdark galaxies has remained elusive. Here, we present the first sample of such galaxies observed with very deep, high-resolution NIRCam imaging from the Early Release Science programme CEERS. 30 HST-dark sources are selected based on their red colours across 1.6–4.4 $\mu$m. Their physical properties are derived from 12-band multiwavelength photometry, including ancillary HST imaging. We find that these galaxies are generally heavily dust-obscured (AV ∼ 2 mag), massive (log (M/M☉) ∼ 10), star-forming sources at z ∼ 2-8 with an observed surface density of ∼0.8 arcmin-2. This suggests that an important fraction of massive galaxies may have been missing from our cosmic census at z > 3 all the way into the Epoch of Reionization. The HST-dark sources lie on the main sequence of galaxies and add an obscured star formation rate density of 3.2+1.8-1.3 × 10-3 M☉ yr-1 Mpc-3 at z ∼ 7, showing likely presence of dust in the Epoch of Reionization. Our analysis shows the unique power of JWST to reveal this previously missing galaxy population and to provide a more complete census of galaxies at z = 2-8 based on rest-frame optical imaging.}, -archivePrefix = {arXiv}, -arxivId = {2207.14733}, -author = {Barrufet, L and Oesch, P A and Weibel, A and Brammer, G and Bezanson, R and Bouwens, R and Fudamoto, Y and Gonzalez, V and Gottumukkala, R and Illingworth, G and Heintz, K E and Holden, B and Labbe, I and Magee, D and Naidu, R. P. and Nelson, E. and Stefanon, M. and Smit, R. and van Dokkum, P. and Weaver, J. R. and Williams, C. C.}, -doi = {10.1093/mnras/stad947}, -eprint = {2207.14733}, -file = {:C\:/Users/Jammy/Documents/Papers/High_Redshift_galaxies/Barrufet2023HSTDark.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {galaxies: high-redshift,infrared: galaxies}, -number = {1}, -pages = {449--456}, -title = {{Unveiling the nature of infrared bright, optically dark galaxies with early JWST data}}, -volume = {522}, -year = {2023} -} -@article{Li2008, -abstract = {We analyze properties of subhalos/substructures resolved in a dark matter simulation of a Milky Way-like halo in a $\Lambda$CDM cosmology. We explore possible links between subhalos and the Galactic satellites and find: 1) The infall patterns of subhalos are slightly elongated along the major axis of the galaxy halo and are clumpy on smaller scales. 2) The Great disk defined by MW satellites (Kroupa et al. 2005) is easily reproduced in our simulations without recurring to sophisticated galaxy formation recipes and is purely due to their highly centrally concentrated distribution around the Galaxy.}, -archivePrefix = {arXiv}, -arxivId = {0807.2780}, -author = {Li, Yang Shyang and Helmi, Amina}, -doi = {10.1007/978-1-4020-5573-7_53}, -eprint = {0807.2780}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Li, Helmi - 2007 - Infall of substructures onto a milky way-like dark halo.pdf:pdf}, -isbn = {0000000000000}, -issn = {15706605}, -journal = {Astrophysics and Space Science Proceedings}, -keywords = {Dark matter,Galaxies: Dwarf,Galaxies: Kinematics and dynamics,Galaxy: Formation,Methods: Numerical}, -number = {202409}, -pages = {311--314}, -title = {{Infall of substructures onto a milky way-like dark halo}}, -volume = {385}, -year = {2007} -} -@article{Dye2014, -abstract = {We have determined the mass density radial profiles of the first five strong gravitational lens systems discovered by the Herschel Astrophysical Terahertz Large Area Survey. We present an enhancement of the semilinear lens inversion method of Warren & Dye which allows simultaneous reconstruction of several different wavebands and apply this to dual-band imaging of the lenses acquired with the Hubble Space Telescope. The five systems analysed here have lens redshifts which span a range 0.22 ≤ z ≤ 0.94. Our findings are consistent with other studies by concluding that: (1) the logarithmic slope of the total mass density profile steepens with decreasing redshift; (2) the slope is positively correlated with the average total projected mass density of the lens contained within half the effective radius and negatively correlated with the effective radius; (3) the fraction of dark matter contained within half the effective radius increases with increasing effective radius and increases with redshift. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1311.5893}, -author = {Dye, S. and Negrello, M. and Hopwood, R. and Nightingale, J. W. and Bussmann, R. S. and Amber, S. and Bourne, N. and Cooray, A. and Dariush, A. and Dunne, L. and Eales, S. A. and Gonzalez-Nuevo, J. and Ibar, E. and Ivison, R. J. and Maddox, S. and Valiante, E. and Smith, M.}, -doi = {10.1093/mnras/stu305}, -eprint = {1311.5893}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: evolution,Galaxies: structure}, -number = {3}, -pages = {2013--2025}, -title = {{Herschel*-ATLAS: Modelling the first strong gravitational lenses}}, -volume = {440}, -year = {2014} -} -@article{Faber1997, -abstract = {We analyze Hubble Space Telescope surface-brightness profiles of 61 elliptical galaxies and spiral bulges (hot galaxies). Luminous hot galaxies have cuspy cores with steep outer power-law profiles that break at r {\$\sim${}} r{\_}b to shallow inner profiles with logslope less than 0.3. Faint hot galaxies show steep, largely featureless power-law profiles at all radii and lack cores. The centers of power-law galaxies are up to 1000 times denser in mass and luminosity than the cores of large galaxies at a limiting radius of 10 pc. At intermediate magnitudes (-22.0 {\textless} M{\_}V {\textless} -20.5), core and power-law galaxies coexist, and there is a range in r{\_}b at a given luminosity of at least two orders of magnitude. Central properties correlate with global rotation and shape: core galaxies tend to be boxy and slowly rotating, whereas power-law galaxies tend to be disky and rapidly rotating. The dense power-law centers of disky, rotating galaxies are consistent with their formation in gas-rich mergers. The parallel proposition that cores are simply the by-products of gas-free stellar mergers is less compelling. For example, core galaxies accrete small, dense, gas-free galaxies at a rate sufficient to fill in low-density cores if the satellites survived and sank to the center. An alternative model for core formation involves the orbital decay of massive black holes (BHs): the BH may heat and eject stars from the center, eroding a power law if any exists and scouring out a core. An average BH mass per spheroid of 0.002 times the stellar mass yields reasonably good agreement with the masses and radii of observed cores and in addition is consistent with the energetics of AGNs and kinematic detections of BHs in nearby galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610055}, -author = {Faber, S M and Tremaine, Scott and Ajhar, Edward A and Byun, Yong-Ik and Dressler, Alan and Gebhardt, Karl and Grillmair, Carl and Kormendy, John and Lauer, Tod R and Richstone, Douglas}, -doi = {10.1086/118606}, -eprint = {9610055}, -issn = {00046256}, -journal = {ApJ}, -keywords = {GALAXIES: EARLY-TYPE,GALAXIES: NUCLEI}, -month = {nov}, -pages = {1771}, -pmid = {17255088}, -primaryClass = {astro-ph}, -title = {{The Centers of Early-Type Galaxies with HST. IV. Central Parameter Relations}}, -url = {http://arxiv.org/abs/astro-ph/9610055%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/118606}, -volume = {114}, -year = {1996} -} -@article{Gavazzi2014, -abstract = {We present RINGFINDER, a tool for finding galaxy-scale strong gravitational lenses in multi-band imaging data. By construction, the method is sensitive to configurations involving a massive foreground ETG and a faint, background, blue source. RINGFINDER detects the presence of blue residuals embedded in an otherwise smooth red light distribution by difference imaging in two bands. The method is automated for efficient application to current and future surveys, having originally been designed for the 150 deg2 Canada-France-Hawaii Telescope Legacy Survey (CFHTLS). We describe each of the steps of RINGFINDER. We then carry out extensive simulations to assess completeness and purity. For sources with magnification $\mu$ > 4, RINGFINDER reaches 42% (25%) completeness and 29% (86%) purity before (after) visual inspection. The completeness of RINGFINDER is substantially improved in the particular range of Einstein radii 0.″8 ≤ R Ein ≤ 2.″0 and lensed images brighter than g = 22.5, where it can be as high as 70%. RINGFINDER does not introduce any significant bias in the source or deflector population. We conclude by presenting the final catalog of RINGFINDER CFHTLS galaxy-scale strong lens candidates. Additional information obtained with Hubble Space Telescope and Keck adaptive optics high-resolution imaging, and with Keck and Very Large Telescope spectroscopy, is used to assess the validity of our classification and measure the redshift of the foreground and the background objects. From an initial sample of 640,000 ETGs, RINGFINDER returns 2500 candidates, which we further reduce by visual inspection to 330 candidates. We confirm 33 new gravitational lenses from the main sample of candidates, plus an additional 16 systems taken from earlier versions of RINGFINDER. First applications are presented in the Strong Lensing Legacy Survey galaxy-scale lens sample paper series. {\textcopyright} 2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1041}, -author = {Gavazzi, Rapha{\"{e}}l and Marshall, Philip J. and Treu, Tommaso and Sonnenfeld, Alessandro}, -doi = {10.1088/0004-637X/785/2/144}, -eprint = {1403.1041}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Gavazzi2014Ringfinder.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,gravitational lensing: strong,methods: data analysis,methods: statistical,surveys,techniques: miscellaneous}, -month = {apr}, -number = {2}, -pages = {144}, -title = {{Ringfinder: Automated detection of galaxy-scale gravitational lenses in ground-based multi-filter imaging data}}, -url = {http://arxiv.org/abs/1403.1041}, -volume = {785}, -year = {2014} -} -@article{Brewer2016, -abstract = {We introduce a Bayesian solution to the problem of inferring the density profile of strong gravitational lenses when the lens galaxy may contain multiple dark or faint substructures. The source and lens models are based on a superposition of an unknown number of non-negative basis functions (or "blobs") whose form was chosen with speed as a primary criterion. The prior distribution for the blobs' properties is specified hierarchically, so the mass function of substructures is a natural output of the method. We use reversible jump Markov Chain Monte Carlo (MCMC) within Diffusive Nested Sampling (DNS) to sample the posterior distribution and evaluate the marginal likelihood of the model, including the summation over the unknown number of blobs in the source and the lens. We demonstrate the method on two simulated data sets: one with a single substructure, and one with ten. We also apply the method to the g-band image of the "Cosmic Horseshoe" system, and find evidence for more than zero substructures. However, these have large spatial extent and probably only point to misspecifications in the model (such as the shape of the smooth lens component or the point spread function), which are difficult to guard against in full generality.}, -archivePrefix = {arXiv}, -arxivId = {1508.00662}, -author = {Brewer, Brendon J and Huijser, David and Lewis, Geraint F}, -doi = {10.1093/mnras/stv2370}, -eprint = {1508.00662}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {data analysis,gravitational lensing,methods,strong}, -month = {jan}, -number = {2}, -pages = {1819--1829}, -title = {{Trans-Dimensional Bayesian Inference for Gravitational Lens Substructures}}, -url = {http://arxiv.org/abs/1508.00662}, -volume = {455}, -year = {2015} -} -@article{Cooper2010, -abstract = {Objective: To establish the relationship between the complexity of treatment for hepatitis C and patient satisfaction. Method: An observational, prospective, single-center study, which included HCV patients treated between October 2014 and February 2016. The primary endpoint was the assessment of satisfaction with treatment, measured by the HCV-ESTAR questionnaire, structured into two dimensions: clinical and lifestyle satisfaction, on a 0-60 score. A reliability analysis was performed. The data collected were: treatment prescribed for HCV, concomitant medication, and Sustained Viral Response. The complexity index of the complete pharmacotherapy was calculated by the computer application MRCI. T-Student was used to identify the complexity of treatment as a marker of dissatisfaction. Results: The study included 171 patients (83.0{\%} male). The mean satisfaction score was 47.9±7.5. The reliability of the complete questionnaire was high (Cronbach alpha, 0.864; intraclass coefficient, 0.843). There was correlation between the Complexity Index and satisfaction (P{\textless}0.05). A reduction of 5 points in the Complexity Index increased fourfold the value of satisfaction with treatment (p{\textless}0.0001). Similarly, a reduction in 12 points in the Concomitant Medication Index doubled the satisfaction (p=0.028). Regarding the overall complexity, 10 points less doubled the satisfaction (p{\textless}0.05). Finally, patients with higher values of satisfaction presented a higher response rate (p=0.029).}, -archivePrefix = {arXiv}, -arxivId = {0910.3211}, -author = {{De Las Aguas Robustillo Cort{\'{e}}s}, Mar{\'{i}}a and Gonz{\'{a}}lez, Carmen Victoria Almeida and Verdugo, Ram{\'{o}}n Morillo}, -doi = {10.7399/fh.2017.41.4.10701}, -eprint = {0910.3211}, -isbn = {9780735407862}, -issn = {21718695}, -journal = {Farmacia Hospitalaria}, -keywords = {Hepatitis C,Medication complexity index,Pharmaceutical care,Satisfaction}, -number = {4}, -pages = {470--478}, -pmid = {26086087}, -title = {{Relationship between pharmacotherapy complexity and patient satisfaction with treatment for hepatitis C}}, -volume = {41}, -year = {2017} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N. J. and Holland, A. D. and Gow, J. P. D. and Hall, D. J. and Tutt, James H. and Burt, D. and Endicott, J.}, -doi = {10.1117/12.926804}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2012 - Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps(2).pdf:pdf}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Barnabe2009, -abstract = {We present the first detailed analysis of the mass and dynamical structure of a sample of six early-type lens galaxies, selected from the Sloan Lens ACS Survey, in the redshift range 0.08 ≲ z ≲ 0.33. Both Hubble Space Telescope/Advanced Camera for Surveys (ACS) high-resolution imaging and Very Large Telescope Visible Multi-Object Spectrograph (VIMOS) integral-field spectroscopy are available for these systems. The galaxies are modelled - under the assumptions of axial symmetry and two-integral stellar distribution function - by making use of the cauldron code, which self-consistently combines gravitational lensing and stellar dynamics and is fully embedded within the framework of Bayesian statistics. The principal results of this study are: (i) all galaxies in the sample are well described by a simple axisymmetric power-law profile for the total density, with a logarithmic slope $\gamma$′ very close to isothermal (〈$\gamma$′〉 = 1.98 ± 0.05 and an intrinsic spread close to 5 per cent) showing no evidence of evolution over the probed range of redshift; (ii) the axial ratio of the total density distribution is rounder than 0.65 and in all cases, except for a fast rotator, does not deviate significantly from the flattening of the intrinsic stellar distribution; (iii) the dark matter fraction within the effective radius has a lower limit of about 15-30 per cent; (iv) the sample galaxies are only mildly anisotropic, with |$\delta$| ≤ 0.16 and (v) the physical distinction among slow and fast rotators, quantified by the v/$\sigma$ ratio and the intrinsic angular momentum, is already present at z ≳ 0.1. Altogether, early-type galaxies at z = 0.08-0.33 are found to be markedly smooth and almost isothermal systems, structurally and dynamically very similar to their nearby counterparts. This work confirms the effectiveness of the combined lensing and dynamics analysis as a powerful technique for the study of early-type galaxies beyond the local Universe. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0904.3861}, -author = {Barnab{\`{e}}, Matteo and Czoske, Oliver and Koopmans, L{\'{e}}on V.E. and Treu, Tommaso and Bolton, Adam S. and Gavazzi, Rapha{\"{e}}l}, -doi = {10.1111/j.1365-2966.2009.14941.x}, -eprint = {0904.3861}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: kinematics and dynamics,Galaxies: structure,Gravitational lensing}, -month = {oct}, -number = {1}, -pages = {21--36}, -title = {{Two-dimensional kinematics of SLACS lenses - II. Combined lensing and dynamics analysis of early-type galaxies at z = 0.08-0.33}}, -volume = {399}, -year = {2009} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Kruk2017, -abstract = {We use multiwavelength Sloan Digital Sky Survey (SDSS) images and Galaxy Zoo morphologies to identify a sample of $\sim$270 late-type galaxies with an off-centre bar. We measure offsets in the range 0.2-2.5 kpc between the photometric centres of the stellar disc and stellar bar. The measured offsets correlate with global asymmetries of the galaxies, with those with largest offsets showing higher lopsidedness. These findings are in good agreement with predictions from simulations of dwarf-dwarf tidal interactions producing off-centre bars. We find that the majority of galaxies with off-centre bars are of Magellanic type, with a median mass of 109.6M⊙, and 91 per cent of them having M⊙ < 3 × 1010M⊙, the characteristic mass at which galaxies start having higher central concentrations attributed to the presence of bulges. We conduct a search for companions to test the hypothesis of tidal interactions, but find that a similar fraction of galaxies with offset bars have companions within 100 kpc as galaxies with centred bars. Although this may be due to the incompleteness of the SDSS spectroscopic survey at the faint end, alternative scenarios that give rise to offset bars such as interactions with dark companions or the effect of lopsided halo potentials should be considered. Future observations are needed to confirm possible low-mass companion candidates and to determine the shape of the dark matter halo, in order to find the explanation for the off-centre bars in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1705.00007}, -author = {Kruk, Sandor J. and Lintott, Chris J. and Simmons, Brooke D. and Bamford, Steven P. and Cardamone, Carolin N. and Fortson, Lucy and Hart, Ross E. and H{\"{a}}u{\ss}ler, Boris and Masters, Karen L. and Nichol, Robert C. and Schawinski, Kevin and Smethurst, Rebecca J.}, -doi = {10.1093/mnras/stx1026}, -eprint = {1705.00007}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kruk et al. - 2017 - Galaxy Zoo Finding offset discs and bars in SDSS galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: dwarf,Galaxies: evolution,Galaxies: interactions,Galaxies: irregular,Galaxies: structure}, -number = {3}, -pages = {3363--3373}, -title = {{Galaxy Zoo: Finding offset discs and bars in SDSS galaxies}}, -url = {http://arxiv.org/abs/1705.00007%0Ahttp://dx.doi.org/10.1093/mnras/stx1026}, -volume = {469}, -year = {2017} -} -@article{Xie2015, -abstract = {Recent work has suggested that the amplitude of the size mass relation of massive early type galaxies evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive early type galaxies. We find this model is able to reproduce the amplitude of present day amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark halos at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than {\$}10{\^{}}{\{}11.4{\}}M{\_}{\{}\backslashodot{\}}{\$}. At lower masses, low mass ratio mergers play a more important role. In situ star formation contribute more to the size growth than it does to stellar mass growth. We also find that, for ETGs identified at {\$}z=2{\$}, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {SPIE High Energy, Optical and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Xu2015, -abstract = {A power-law density model, i.e. $\rho$(r) ∝ r-$\gamma$', has been commonly employed in strong gravitational lensing studies, including the so-called time-delay technique used to infer the Hubble constant H0. However, since the radial scale at which strong lensing features are formed corresponds to the transition from the dominance of baryonic matter to dark matter, there is no known reason why galaxies should follow a power law in density. The assumption of a power law artificially breaks the mass-sheet degeneracy, a well-known invariance transformation in gravitational lensing which affects the product of Hubble constant and time delay and can therefore cause a bias in the determination of H0 from the time-delay technique. In this paper, we use the Illustris hydrodynamical simulations to estimate the amplitude of this bias, and to understand how it is related to observational properties of galaxies. Investigating a large sample of Illustris galaxies that have velocity dispersion $\sigma$SIE ≤ 160 km s-1 at redshifts below z = 1, we find that the bias on H0 introduced by the power-law assumption can reach 20-50 per cent, with a scatter of 10-30 per cent (rms). However, we find that by selecting galaxies with an inferred power-law model slope close to isothermal, it is possible to reduce the bias on H0 to ≲ 5 per cent and the scatter to ≲ 10 per cent. This could potentially be used to form less biased statistical samples for H0 measurements in the upcoming large survey era.}, -archivePrefix = {arXiv}, -arxivId = {1507.07937}, -author = {Xu, Dandan and Sluse, Dominique and Schneider, Peter and Springel, Volker and Vogelsberger, Mark and Nelson, Dylan and Hernquist, Lars}, -doi = {10.1093/mnras/stv2708}, -eprint = {1507.07937}, -isbn = {1466-2094}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {1}, -pages = {739--755}, -title = {{Lens galaxies in the illustris simulation: Power-law models and the bias of the Hubble constant from time delays}}, -volume = {456}, -year = {2016} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for {\$\sim${}}20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Iwanus2017, -abstract = {We describe and test a novel dark matter annihilation feedback (DMAF) scheme that has been implemented into the well-known cosmological simulation code GADGET-2. In the models considered here, dark matter can undergo self-annihilation/decay into radiation and baryons. These products deposit energy into the surrounding gas particles and then the dark matter/baryon fluid is self-consistently evolved under gravity and hydrodynamics. We present tests of this new feedback implementation in the case of idealized dark matter haloes with gas components for a range of halomasses, concentrations and annihilation rates. For some darkmattermodels, DMAF's ability to evacuate gas is enhanced in lower mass, concentrated haloes where the injected energy is comparable to its gravitational binding energy. Therefore, we expect the strongest signs of darkmatter annihilation to imprint themselves on to the baryonic structure of concentrated dwarf galaxies through their baryonic fraction and star formation history. Finally, we present preliminary results of the first self-consistent DMAF cosmological box simulations showing that the small-scale substructure is washed out for large annihilation rates.}, -archivePrefix = {arXiv}, -arxivId = {1707.06770}, -author = {Iwanus, N and Elahi, P J and Lewis, G F}, -doi = {10.1093/MNRAS/STX1974}, -eprint = {1707.06770}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Large-scale structure of Universe}, -number = {1}, -pages = {1214--1225}, -title = {{Dark matter annihilation feedback in cosmological simulations - I: Code convergence and idealized haloes}}, -url = {http://arxiv.org/abs/1707.06770%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1974}, -volume = {472}, -year = {2017} -} -@article{Mao1998, -abstract = {We discuss whether one should expect that multiply imaged QSOs can be understood with 'simple' lens models that contain only a few parameters. Whereas for many lens systems such simple mass models yield a remarkably good description of the observed properties, there are some systems which are notoriously difficult to understand quantitatively. We argue that at least in one case (B 1422 + 231) these difficulties are not (solely) due to a 'wrong' parametrization of the lens model, but that the discrepancy between observed and model-predicted flux ratios is due to substructure in the lens. As in microlensing for optical fluxes, such substructure can distort also the radio flux ratios predicted by 'simple' mass models, in particular for highly magnified images, without appreciably changing image positions. Substructure also does not change the time delay significantly, and therefore has little effect on the determination of the Hubble constant using time delays. We quantify these statements with several simple scenarios for substructure, and propose a strategy to model lens systems in which substructure is suspected.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9707187}, -author = {Mao, Shude and Schneider, Peter}, -doi = {10.1046/j.1365-8711.1998.01319.x}, -eprint = {9707187}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing,Quasars: general}, -month = {apr}, -number = {3}, -pages = {587--594}, -primaryClass = {astro-ph}, -title = {{Evidence for substructure in lens galaxies?}}, -url = {http://www.mendeley.com/research/no-title-avail/%5Cnhttp://arxiv.org/abs/astro-ph/9707187%5Cnhttp://doi.wiley.com/10.1046/j.1365-8711.1998.01319.x}, -volume = {295}, -year = {1998} -} -@article{Khochfar2011, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* {\textgreater} 1010.5 Msun contributing ˜20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between ˜50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z {\textgreater} 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) {\textgreater} 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z {\textless} 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive ({\textgreater}1010 Msun) fast rotators being more than one order of magnitude more frequent at z˜ 2.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M and Cappellari, Michele and Davies, Roger L and Davis, Timothy A and de Zeeuw, P T and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: structure,cD}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS 3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Murray2013, -abstract = {A multi-level clocking scheme has been developed to improve the parallel CTE of four-phase CCDs by suppressing the effects of traps located in the transport channel under barrier phases by inverting one of these phases throughout the transfer sequence. In parallel it was apparent that persistence following optical overload in Euclid VIS detectors would lead to undesirable signal released in subsequent rows and frames and that a suitable scheme for flushing this signal would be required. With care, the negatively biased electrodes during the multi-level transfer sequence can be made to pin the entire surface, row-by-row, and annihilate the problematic charges. This process can also be extended for use during integration to significantly reduce the unusable area of the detector, as per the clocked anti-blooming techniques developed many years ago; however, with the four-phase electrodes architecture of modern CCDs, we can take precautionary measures to avoid the problem of charge pumping and clock induced charge within the science frames. Clock induced charge is not all bad! We also propose the use of on-orbit trap-pumping for Euclid VIS to provide calibration input to ground based correction algorithms and as such a uniform, low noise background is require. Clock induced charge can be manipulated to provide a very suitable, low signal and noise background to the imaging array. Here we describe and present results of multi-level parallel clocking schemes for use in four-phase CCDs that could improve performance of high precision astronomy applications such as Euclid VIS. ? 2013 SPIE.}, -author = {Murray, Neil J. and Burt, David J. and Holland, Andrew D. and Stefanov, Konstantin D. and Gow, Jason P. D. and MacCormick, Calum and Dryer, Ben J. and Allanwood, Edgar A. H.}, -doi = {10.1117/12.2024839}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2013 - Multi-level parallel clocking of CCDs for improving charge transfer efficiency, clearing persistence, clocked ant.pdf:pdf}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {[BFW, Blooming, CAB, CCD, CIC, CTE, Euclid VIS, Mu}, -pages = {88600K}, -title = {{Multi-level parallel clocking of CCDs for: improving charge transfer efficiency, clearing persistence, clocked anti-blooming, and generating low-noise backgrounds for pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024839}, -volume = {8860}, -year = {2013} -} -@article{Bruce2012, -abstract = {We have used high-resolution, HST WFC3/IR, near-infrared imaging to conduct a detailed bulge-disk decomposition of the morphologies of ≃ 200 of the most massive (M * {\textgreater} 1011 M{\textperiodcentered}) galaxies at 1 {\textless} z {\textless} 3 in the CANDELS-UDS field. We find that, while such massive galaxies at low redshift are generally bulge-dominated, at redshifts 1{\textless}z{\textless}2 they are predominantly mixed bulge+disk systems, and by z {\textgreater} 2 they are mostly disk-dominated. Interestingly, we find that while most of the quiescent galaxies are bulge-dominated, a significant fraction (25-40{\%}) of the most quiescent galaxies, have disk-dominated morphologies. Thus, our results suggest that the physical mechanisms which quench star-formation activity are not simply connected to those responsible for the morphological transformation of massive galaxies. {\textcopyright}2013 International Astronomical Union.}, -archivePrefix = {arXiv}, -arxivId = {1206.4322}, -author = {Bruce, V A and Dunlop, J S and Cirasuolo, M and McLure, R J and Targett, T A and Bell, E F and Croton, D J and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Kocevski, D D and Koekemoer, A M and Koo, D C and Lai, K and Lotz, J M and McGrath, E J and Newman, J A and {Van Der Wel}, A}, -doi = {10.1017/S1743921313004237}, -eprint = {1206.4322}, -isbn = {9781107033849}, -issn = {17439213}, -journal = {Proceedings of the International Astronomical Union}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: high-redshift,galaxies: structure}, -month = {dec}, -number = {S295}, -pages = {49--52}, -title = {{The morphologies of massive galaxies at 1{\textless}z{\textless}3 in the CANDELS-UDS field: Compact bulges, and the rise and fall of massive disks}}, -volume = {8}, -year = {2012} -} -@article{Skottfelta, -author = {Skottfelt, Jesper and Hall, David J and Dryer, Ben and Lee-payne, Zoe and Holland, Andrew D and Ccd, Euclid}, -file = {:C\:/Users/Jammy/Documents/Papers/CTI/Euclid_TP_serial.pdf:pdf}, -title = {{Trap pumping schemes for the Euclid CCD273 detector II : Serial register}} -} -@article{Siverd2009, -abstract = {We identify, categorize, and quantify alignment effects among host and satellite galaxies using a spectroscopically-confirmed, low-redshift (z{\textless}0.23) galaxy sample from the Sloan Digital Sky Survey Data Release 6. Consistent with other recent findings, we find that satellite galaxies (SGs) of red, centrally concentrated (elliptical) host galaxies (HGs) with radial velocity separation |Delta{\_}V|{\textless}600 km/s preferentially reside near the projected major axes of their HGs. Among these, this preference is strongest for highly concentrated, red SGs. We find that fractional anisotropy increases with decreasing $\backslash$Delta{\_}V and Delta{\_}R and is nearly 40{\%} greater among the closest SGs (Delta{\_}R{\textless}250 kpc/h) relative to more distant (Delta{\_}R{\textgreater}500 kpc/h) SGs. For highly concentrated SGs at small ({\textless}300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to {\textless}15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby ({\textless}40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ({\$\sim${}}3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R J and Ryden, B S and Gaudi, B S}, -eprint = {0903.2264}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M * = 1010.2 to 1012.0 M . We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority (≳75{\%}) of elliptical galaxies is not well described by a single S{\'{e}}rsic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (Re ∼ 1 kpc) inner component with luminosity fraction f 0.1-0.15; an intermediate-scale (Re 2.5 kpc) middle component with f 0.2-0.25; and a dominant (f = 0.6), extended (Re 10 kpc) outer envelope. All subcomponents have average S{\'{e}}rsic indices n 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies. {\textcopyright}2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C and Peng, Chien Y and Li, Zhao Yu and Barth, Aaron J}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work done to interpret this phenomena has found that it is due to the non-spherical nature of dark matter halos. However, most studies over-predict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shape of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations that satellites galaxies without associated subhalos ('orphan galaxies') are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region.}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W P and Kang, X and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%7B%5C%25%7D5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem%7B%5C&%7Dsid=IOPP%7B%5C%25%7D3Ajnl%7B%5C_%7Dref%7B%5C&%7Dspage=305%7B%5C&%7Dtitle=ArA%7B%5C&%7Dvolume=5%7B%5C&%7Ddate=1969%7B%5C&%7Dv%7B%5C}, -volume = {786}, -year = {2014} -} -@article{Robotham2017, -abstract = {We present PROFIT, a new code for Bayesian two-dimensional photometric galaxy profile modelling. PROFIT consists of a low-level C++ library (libprofit), accessible via a command-line interface and documented API, along with high-level R (PROFIT) and PYTHON (PyProFit) interfaces (available at github.com/ICRAR/libprofit, github.com/ICRAR/ProFit, and github.com/ICRAR/pyprofit, respectively). R PROFIT is also available pre-built from CRAN; however, this version will be slightly behind the latest GitHub version. libprofit offers fast and accurate two-dimensional integration for a useful number of profiles, including S{\'{e}}rsic, Core-S{\'{e}}rsic, broken-exponential, Ferrer, Moffat, empirical King, point-source, and sky, with a simple mechanism for adding new profiles. We show detailed comparisons between libprofit and GALFIT. libprofit is both faster and more accurate than GALFIT at integrating the ubiquitous S{\'{e}}rsic profile for the most common values of the S{\'{e}}rsic index n (0.5 < n < 8). The high-level fitting code PROFIT is tested on a sample of galaxies with both SDSS and deeper KiDS imaging. We find good agreement in the fit parameters, with larger scatter in best-fitting parameters from fitting images from different sources (SDSS versus KiDS) than from using different codes (PROFIT versus GALFIT). A large suite of Monte Carlo-simulated images are used to assess prospects for automated bulge-disc decomposition with PROFIT on SDSS, KiDS, and future LSST imaging. We find that the biggest increases in fit quality come from moving from SDSS- to KiDS-quality data, with less significant gains moving from KiDS to LSST.}, -archivePrefix = {arXiv}, -arxivId = {1611.08586}, -author = {Robotham, A. S.G. and Taranu, D. S. and Tobar, R. and Moffett, A. and Driver, S. P.}, -doi = {10.1093/mnras/stw3039}, -eprint = {1611.08586}, -file = {:C\:/Users/Jammy/Documents/Papers/Profit2019.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: statistics,Galaxies: structure,Methods: data analysis,Methods: statistical,Techniques: photometric}, -number = {2}, -pages = {1513--1541}, -title = {{Profit: Bayesian profile fitting of galaxy images}}, -volume = {466}, -year = {2017} -} -@article{Geometryek, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Ding2021, -abstract = {Galight is a Python-based open-source package that can be used to perform two-dimensional model fitting of optical and near-infrared images to characterize the light distribution of galaxies with components including a disk, bulge, bar, and quasar. The decomposition of stellar components has been demonstrated in published studies of inactive galaxies and quasar host galaxies observed by the Hubble Space Telescope and Subaru's Hyper Suprime-Cam. Galight utilizes the image modeling capabilities of lenstronomy while redesigning the user interface for the analysis of large samples of extragalactic sources. The package is user-friendly with some automatic features such as determining the cutout size of the modeling frame, searching for PSF-stars in field-of-view, estimating the noise map of the data, identifying all the objects to set the initial model, and associated parameters to fit them simultaneously. These features minimize the manpower and allow the automatic fitting tasks. The software is distributed under the MIT license. The source code, installation guidelines, and example notebooks code can be found at https://galight.readthedocs.io/en/latest/}, -archivePrefix = {arXiv}, -arxivId = {2111.08721}, -author = {Ding, Xuheng and Birrer, Simon and Treu, Tommaso and Silverman, John D.}, -eprint = {2111.08721}, -file = {:C\:/Users/Jammy/Documents/Papers/Gallight.pdf:pdf}, -keywords = {data analysis,galaxies,image processing,methods,photometry,techniques}, -title = {{Galaxy shapes of Light (GaLight): a 2D modeling of galaxy images}}, -url = {http://arxiv.org/abs/2111.08721}, -volume = {8583}, -year = {2021} -} -@article{Liao2016, -abstract = {The standard galaxy formation theory assumes that baryons and dark matter are initially well-mixed before becoming segregated due to radiative cooling. We use non-radiative hydrodynamical simulations to explicitly examine this assumption and find that baryons and dark matter can also be segregated because of different physics obeyed by gas and dark matter during the build-up of the halo. As a result, baryons in many haloes do not originate from the same Lagrangian region as the dark matter. When using the fraction of corresponding dark matter and gas particles in the initial conditions (the "paired fraction") as a proxy of the dark matter and gas segregation strength of a halo, on average about {\$}25{\$} percent of the baryonic and dark matter of the final halo are segregated in the initial conditions. This is at odds with the assumption of the standard galaxy formation model. A consequence of this effect is that the baryons and dark matter of the same halo initially experience different tidal torques and thus their angular momentum vectors are often misaligned. The degree of the misalignment is largely preserved during later halo assembly and can be understood with the tidal torque theory. The result challenges the precision of some semi-analytical approaches which utilize dark matter halo merger trees to infer properties of gas associated to dark matter haloes.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.07592}, -author = {Liao, Shihong and Gao, Liang and Frenk, Carlos S and Guo, Qi and Wang, Jie}, -doi = {10.1093/mnras/stx1391}, -eprint = {1610.07592}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {2}, -pages = {2262--2269}, -title = {{The segregation of baryons and dark matter during halo assembly}}, -url = {http://arxiv.org/abs/1610.07592}, -volume = {470}, -year = {2017} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and disks are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disk components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to CALIFA integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component, and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -keywords = {elliptical and lenticular,galaxies,kinematics and dynamics}, -number = {December}, -pages = {1--11}, -title = {{Untangling galaxy components: full spectral bulge-disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {11}, -year = {2016} -} -@article{Hall2014, -abstract = {The science goals of space missions from the Hubble Space Telescope through to Gaia and Euclid require ultraprecise positional, photometric, and shape measurement information. However, in the radiation environment of the space telescopes, damage to the focal plane detectors through high-energy protons leads to the creation of traps, a loss of charge transfer efficiency, and a consequent deterioration in measurement accuracy. An understanding of the traps produced and their properties in the CCD during operation is essential to allow optimization of the devices and suitable modeling to correct the effect of the damage through the postprocessing of images. The technique of 'pumping single traps' has allowed the study of individual traps in high detail that cannot be achieved with other techniques, such as deep level transient spectroscopy, whilst also locating each trap to the subpixel level in the device. Outlining the principles used, we have demonstrated the technique for the A-center, the most influential trap in serial readout, giving results consistent with the more general theoretical values, but here showing new results indicating the spread in the emission times achieved and the variation in capture probability of individual traps with increasing signal levels. This technique can now be applied to other time and temperature regimes in the CCD to characterize individual traps in situ under standard operating conditions such that dramatic improvements can be made to optimization processes and modeling techniques. {\textcopyright} 2013 IEEE.}, -author = {Hall, David J. and Murray, Neil J. and Holland, Andrew D. and Gow, Jason and Clarke, Andrew and Burt, David}, -doi = {10.1109/TNS.2013.2295941}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hall et al. - 2014 - Determination of in situ trap properties in CCDs using a single-trap pumping technique.pdf:pdf}, -isbn = {9781467350570}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {A-centre,CCD image sensors,Euclid,Si-A,defect,pocket pumping,radiation damage,trap pumping}, -number = {4}, -pages = {1826--1833}, -title = {{Determination of in situ trap properties in CCDs using a "single-trap pumping" technique}}, -volume = {61}, -year = {2014} -} -@article{Goulding2016a, -abstract = {Studies of the physical properties of local elliptical galaxies (e.g., gas temperatures, halo masses, stellar kinematics) are shedding new light on galaxy formation. Here we present the hot X-ray gas properties of 33 early-type systems within the MASSIVE galaxy survey sample that have archival Chandra X-ray observations. Through careful X-ray spectral modeling, we derive X-ray luminosities (L{\_}X) and plasma temperatures (T{\_}gas) for the diffuse gas components in these galaxies. We combine the MASSIVE sample with 41 galaxies from the ATLAS{\^{}}3D survey to investigate the X-ray and optical properties of a statistically significant sample of nearby early-type galaxies across a wide-range of environments. We deduce that all early-type galaxies (independent of galaxy mass and rotational support) follow a universal scaling law such that L{\_}X{\$\sim${}}T{\_}gas{\^{}}4.5. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, the wide-scale environment does not contribute to the intrinsic scatter ({\$\sim${}}0.5dex) within the scaling relation. We further demonstrate that the scatter in L{\_}X around both K-band luminosity (L{\_}K) and the galaxy stellar velocity dispersion is primarily driven by T{\_}gas, with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the origin of the gas directly to either the stellar mass or the galaxy potential. Indeed, our data require a steeper relation between L{\_}X, L{\_}K, and sigma{\_}e than predicted by standard mass-loss models. Finally, we find a statistically significant correlation between sigma{\_}e and T{\_}gas, suggesting that T{\_}gas is set by the galaxy potential inside the optical effective radius. We conclude that within the inner-most 10-30kpc region, early-types maintain pressure-supported hot gas, with a minimum T{\_}gas set by the virial temperature, but the majority show evidence for some additional heating.}, -archivePrefix = {arXiv}, -arxivId = {1604.01764}, -author = {Goulding, Andy D and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Bogdan, Akos and Nyland, Kristina and Blakeslee, John P and McConnell, Nicholas J and Thomas, Jens}, -doi = {10.3847/0004-637x/826/2/167}, -eprint = {1604.01764}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {167}, -title = {{the Massive Survey. Iv. the X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe}}, -url = {http://arxiv.org/abs/1604.01764%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/826/2/167}, -volume = {826}, -year = {2016} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S.}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Guo et al. - 2016 - Deep learning for visual understanding A review(2).pdf:pdf}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, $\sigma$(R), for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude MK {\textless} -25.3mag, or stellar mass M* ≳ 4 × 1011M⊙, within 108 Mpc. Our wide-field 107 arcsec × 107 arcsec IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes $\gamma$ inner and $\gamma$ outer of s(R). While $\gamma$ inner is mostly negative, of the 56 galaxies with sufficient radial coverage to determine $\gamma$ outer we find 36 per cent to have rising outer dispersion profiles, 30 per cent to be flat within the uncertainties and 34 per cent to be falling. The fraction of galaxies with rising outer profiles increases with M* and in denser galaxy environment, with 10 of the 11 most massive galaxies in our sample having flat or rising dispersion profiles. The strongest environmental correlations are with local density and halo mass, but a weaker correlation with large-scale density also exists. The average $\gamma$ outer is similar for brightest group galaxies, satellites and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis h4. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{Sahu2019, -abstract = {Analyzing a sample of 84 early-type galaxies with directly-measured super-massive black hole masses---nearly doubling the sample size of such galaxies with multi-component decompositions---a symmetric linear regression on the reduced (merger-free) sample of 76 galaxies reveals {\$}M{\_}{\{}BH{\}}\backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.27\backslashpm 0.07{\}}{\$} with a total scatter of {\$}\backslashDelta{\_}{\{}rms{\}}={\$} 0.52 dex in the {\$}\backslashlog(M{\_}{\{}BH{\}}){\$} direction. However, and importantly, we discover that the ES/S0-type galaxies with disks are offset from the E-type galaxies by more than a factor of ten in their {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio, with ramifications for formation theories, simulations, and some virial factor measurements used to convert AGN virial masses into {\$}M{\_}{\{}BH{\}}{\$}. Separately, each population follows a steeper relation with slopes of {\$}1.86\backslashpm0.20{\$} and {\$}1.90\backslashpm0.20{\$}, respectively. The offset mass ratio is mainly due to the exclusion of the disk mass, with the two populations offset by only a factor of two in their {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,gal{\}}{\$} ratio in the {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,gal{\}}{\$} diagram where {\$}M{\_}{\{}BH{\}}\backslashpropto M{\_}{\{}*,gal{\}}{\^{}}{\{}1.8\backslashpm 0.2{\}}{\$} and {\$}\backslashDelta{\_}{\{}rms{\}}=0.6\backslashpm 0.1{\$} dex depending on the sample. For {\$}M{\_}{\{}BH{\}} \backslashgtrsim 10{\^{}}7 M{\_}{\{}\backslashodot{\}}{\$}, we detect no significant bend nor offset in either the {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,sph{\}}{\$} or {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,gal{\}}{\$} relations due to barred versus non-barred, or core-S$\backslash$'ersic versus S$\backslash$'ersic, early-type galaxies. For reference, the ensemble of late-type galaxies (which invariably are S$\backslash$'ersic galaxies) follow {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,gal{\}}{\$} relations with slopes equal to {\$}2.16\backslashpm 0.32{\$} and {\$}3.05\backslashpm 0.70{\$}, respectively. Finally, we provide some useful conversion coefficients, {\$}\backslashupsilon{\$}, accounting for the different stellar mass-to-light ratios used in the literature, and we report the discovery of a local, compact massive spheroid in NGC 5252.}, -archivePrefix = {arXiv}, -arxivId = {1903.04738}, -author = {Sahu, Nandini and Graham, Alister W and Davis, Benjamin L}, -doi = {10.3847/1538-4357/ab0f32}, -eprint = {1903.04738}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {black hole physics,bulges,cd,elliptical and lenticular,evolution,galaxies,photometry,structure}, -number = {2}, -pages = {155}, -title = {{ Black Hole Mass Scaling Relations for Early-type Galaxies. I. M BH – M *, sph and M BH – M *,gal }}, -volume = {876}, -year = {2019} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series that re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science data base, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies. This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution that limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ('encounter-driven') rings (such as ring and polar ring galaxies) are recognized in less than 1 per cent of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{Huang2018, -abstract = {We use {\$\sim${}}100 deg2 of deep ({\textgreater} 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach {\$\sim${}}4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) {\textgreater} 11.6 in more massive haloes at 0.3 {\textless} z {\textless} 0.5 have shallower inner stellar mass density profiles (within {\$\sim${}}10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) {\textgreater} 14.0 are {\$\sim${}}20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{Du2020, -abstract = {We recently developed an automated method, auto-GMM, to kinematically decompose simulated galaxies. It extracts the kinematic structures in an accurate, efficient, and unsupervised way. Here we use auto-GMM to study the stellar kinematic structures of disk galaxies from the TNG100 run of the cosmological suite IllustrisTNG. We identify four to five kinematic structures that are commonly present among the diverse galaxy population. Structures having strong to moderate rotation are defined as cold and warm disks, respectively. Spheroidal structures dominated by random motions are classified as bulges or stellar halos, depending on how tightly bound they are. Disky bulges are defined as structures that have moderate rotation but compact morphology. TNG100 returns multiple structures that have reasonable properties, qualitatively consistent with our general expectations. Across all disky galaxies and accounting for the stellar mass within 3 half-mass radii, the kinematic spheroidal structures, obtained by summing up stars of bulges and halos, contribute {\$}\backslashsim 45\backslash{\%}{\$} of the total stellar mass, while the disky structures constitute {\$}\backslashsim 55\backslash{\%}{\$}. This study also provides important insights about the relationship between kinematically and morphologically derived galactic structures. Comparing the morphology of kinematic structures with that of traditional bulge+disk decomposition, we conclude: (1) the morphologically decomposed bulges are composite structures comprised of a slowly rotating bulge, an inner halo, and a disky bulge; (2) kinematically disky bulges, akin to what are commonly called pseudo bulges in observations, are compact disk-like components that have rotation similar to warm disks; (3) halos contribute almost {\$}30\backslash{\%}{\$} of the surface density of the outer part of morphological disks when viewed face-on; and (4) both cold and warm disks are often truncated in central regions.}, -archivePrefix = {arXiv}, -arxivId = {2002.04182}, -author = {Du, Min and Ho, Luis C and Debattista, Victor P and Pillepich, Annalisa and Nelson, Dylan and Zhao, Dongyao and Hernquist, Lars}, -doi = {10.3847/1538-4357/ab8fa8}, -eprint = {2002.04182}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {391,591,602,622,767,corresponding author,disk galaxies,galaxy dynamics,galaxy kinematics,galaxy structure,hydrodynamical simulations,min du}, -number = {2}, -pages = {139}, -title = {{Kinematic Decomposition of IllustrisTNG Disk Galaxies: Morphology and Relation with Morphological Structures}}, -url = {http://arxiv.org/abs/2002.04182}, -volume = {895}, -year = {2020} -} -@article{Algorry2016, -abstract = {We examine the properties of barred disc galaxies in a $\Lambda$CDM cosmological hydrodynamical simulation from the EAGLE project. Our study follows the formation of 269 discs identified at z = 0 in the stellar mass range 10.6 {\textless} logM∗/M⊙ {\textless} 11. These discs show a wide range of bar strengths, from unbarred discs (≈60 per cent) to weak bars (≈20 per cent) and to strongly barred systems (≈20 per cent). Bars in these systems develop after redshift ≈1.3, on timescales that depend sensitively on the strength of the pattern. Strong bars develop relatively quickly (in a few Gyr, or roughly∼10 disc rotation periods) in systems that are disc dominated, gas poor, and have declining rotation curves.Weak bars develop more slowly in systems where the disc is less gravitationally important, and are still growing at z = 0. Unbarred galaxies are comparatively gas-rich discs whose rotation speeds do not exceed the maximum circular velocity of the haloes they inhabit. Bar lengths compare favourably with observations, ranging from 0.2 to 0.8 times the radius containing 90 per cent of the stars. Bars slow down remarkably quickly as they grow, causing the inner regions of the surrounding dark halo to expand. At z = 0 strong bars in simulated galaxies have corotation radii roughly 10 times the bar length. Such slow bars are inconsistent with the few cases where pattern speeds have been measured or inferred observationally, a discrepancy that, if confirmed, might prove a challenge for disc galaxy formation in $\Lambda$CDM.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1609.05909}, -author = {Algorry, David G and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Vecchia, Claudio Dalla and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx1008}, -eprint = {1609.05909}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Kinematics and dynamics,Galaxy: Disc,Galaxy: Formation,Galaxy: Structure}, -number = {1}, -pages = {1054--1064}, -title = {{Barred galaxies in the EAGLE cosmological hydrodynamical simulation}}, -url = {http://arxiv.org/abs/1609.05909%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1008}, -volume = {469}, -year = {2017} -} -@article{Enia2018, -abstract = {We perform lens modelling and source reconstruction of Sub-millimetre Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500$\mu$m in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). A previous analysis of the same data set used a single S{\'{e}}rsic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from theH-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission.We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5s. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value reff {\$\sim${}} 1.77 kpc and a median Gaussian full width at half-maximum {\$\sim${}}1.47 kpc. After correction for magnification, our sources have intrinsic star formation rates (SFR) {\$\sim${}} 900-3500M⊙ yr-1, resulting in a median SFR surface density $\Sigma$SFR {\$\sim${}} 132M⊙ yr-1 kpc-2 (or {\$\sim${}}218M⊙ yr-1 kpc-2 for the Gaussian fit). This is consistent with that observed for other star-forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst.}, -archivePrefix = {arXiv}, -arxivId = {1801.01831}, -author = {Enia, A and Negrello, M and Gurwell, M and Dye, S and Rodighiero, G and Massardi, M and {De Zotti}, G and Franceschini, A and Cooray, A and van der Werf, P and Birkinshaw, M and Michalowski, M J and Oteo, I}, -doi = {10.1093/mnras/sty021}, -eprint = {1801.01831}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong,Instrumentation: interferometers}, -number = {3}, -pages = {3467--3484}, -title = {{The Herschel-ATLAS: Magnifications and physical sizes of 500-$\mu$m-selected strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1801.01831}, -volume = {475}, -year = {2018} -} -@article{Morganti2013, -abstract = {NGC 4494 is one of several intermediate-luminosity elliptical galaxies inferred to have an unusually diffuse dark matter halo. We use the chi{\^{}}2-made-to-measure particle code NMAGIC to construct axisymmetric models of NGC 4494 from photometric and various kinematic data. The extended kinematics include light spectra in multiple slitlets out to 3.5 R{\_}e, and hundreds of planetary nebulae velocities out to {\$\sim${}}7 R{\_}e, thus allowing us to probe the dark matter content and orbital structure in the halo. We use Monte Carlo simulations to estimate confidence boundaries for the halo parameters, given our data and modelling set-up. We find that the true potential of the dark matter halo is recovered within Delta G (merit function){\textless}26 (Delta chi{\^{}}2{\textless}59) at 70{\%} confidence level (C.L.), and within Delta G{\textless}32 (Delta chi{\^{}}2{\textless}70) at 90{\%} C.L.. These numbers are much larger than the usually assumed Delta chi{\^{}}2=2.3 (4.6) for 70{\%} (90{\%}) C.L. for two free parameters, perhaps case-dependent, but calling into question the general validity of the standard assumptions used for halo and black hole mass determinations. The best-fitting models for NGC 4494 have a dark matter fraction of about 0.6{\$}\backslash{\$}pm0.1 at 5R{\_}e (70{\%} C.L.), and are embedded in a dark matter halo with circular velocity {\$\sim${}}200 km/s. The total circular velocity curve (CVC) is approximately flat at v{\_}c=220 km/s outside {\$\sim${}}0.5R{\_}e. The orbital anisotropy of the stars is moderately radial. These results are independent of the assumed inclination of the galaxy, and edge-on models are preferred. Comparing with the halos of NGC 3379 and NGC 4697, whose velocity dispersion profiles also decrease rapidly from the center outwards, the outer CVCs and dark matter halos are quite similar. NGC 4494 shows a particularly high dark matter fraction inside {\$\sim${}}3R{\_}e, and a strong concentration of baryons in the center.}, -archivePrefix = {arXiv}, -arxivId = {1303.2688}, -author = {Morganti, Lucia and Gerhard, Ortwin and Coccato, Lodovico and Martinez-valpuesta, Inma and Arnaboldi, Magda}, -doi = {10.1093/mnras/stt442}, -eprint = {1303.2688}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: individual: NGC 4494,Galaxies: kinematics and dynamics,Methods: numerical,cD}, -number = {4}, -pages = {3570--3588}, -title = {{Elliptical galaxies with rapidly decreasing velocity dispersion profiles: Nmagic models and dark halo parameter estimates for NGC 4494}}, -volume = {431}, -year = {2013} -} -@article{Massey2007, -abstract = {We present a three dimensional cosmic shear analysis of the Hubble Space Telescope COSMOS survey, the largest ever optical imaging program performed in space. We have measured the shapes of galaxies for the tell-tale distortions caused by weak gravitational lensing, and traced the growth of that signal as a function of redshift. Using both 2D and 3D analyses, we measure cosmological parameters Omega_m, the density of matter in the universe, and sigma_8, the normalization of the matter power spectrum. The introduction of redshift information tightens the constraints by a factor of three, and also reduces the relative sampling (or "cosmic") variance compared to recent surveys that may be larger but are only two dimensional. From the 3D analysis, we find sigma_8*(Omega_m/0.3)^0.44=0.866+^0.085_-0.068 at 68% confidence limits, including both statistical and potential systematic sources of error in the total budget. Indeed, the absolute calibration of shear measurement methods is now the dominant source of uncertainty. Assuming instead a baseline cosmology to fix the geometry of the universe, we have measured the growth of structure on both linear and non-linear physical scales. Our results thus demonstrate a proof of concept for tomographic analysis techniques that have been proposed for future weak lensing surveys by a dedicated wide-field telescope in space.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701480}, -author = {Massey, Richard and Rhodes, Jason and Leauthaud, Alexie and Capak, Peter and Ellis, Richard and Koekemoer, Anton and Refregier, Alexandre and Scoville, Nick and Taylor, James E. and Albert, Justin and Berge, Joel and Heymans, Catherine and Johnston, David and Kneib, Jean‐Paul and Mellier, Yannick and Mobasher, Bahram and Semboloni, Elisabetta and Shopbell, Patrick and Tasca, Lidia and {Van Waerbeke}, Ludovic}, -doi = {10.1086/516599}, -eprint = {0701480}, -issn = {0067-0049}, -journal = {ApJS}, -keywords = {Cosmology: Gravitational Lensing,Cosmology: Large-Scale Structure of Universe,Cosmology: Observations}, -month = {sep}, -number = {1}, -pages = {239--253}, -primaryClass = {astro-ph}, -title = {{COSMOS: Three‐dimensional Weak Lensing and the Growth of Structure}}, -url = {http://arxiv.org/abs/astro-ph/0701480%0Ahttp://dx.doi.org/10.1086/516599}, -volume = {172}, -year = {2007} -} -@article{Melo2023, -abstract = {General Relativity (GR) has been successfully tested mainly at Solar system scales; however, galaxy-scale tests have become popular in the last few decades. In this work, we investigate the $\eta$PPN parameter, which is commonly defined by the ratio of two scalar potentials that appears in the cosmological linearly perturbed metric. Under the assumption of GR and a vanish anisotropic stress tensor, $\eta$PPN = 1. Using ALMA, HST, and VLT/MUSE data, we combine mass measurements, using gravitational lensing and galactic dynamics, for the SDP.81 lens galaxy (z = 0.299) to constrain $\eta$PPN. By using a flexible and self-consistent mass profile, our fiducial model takes into account the contribution of the stellar mass and a dark matter halo to reconstruct the lensed galaxy and the spatially resolved stellar kinematics. We infer, after accounting for systematic uncertainties related to the mass model, cosmology, and kinematics, $\eta$PPN = 1.13+0.03−0.03 ± 0.20 (sys), which is in accordance with GR predictions. Better spectroscopy data are needed to push the systematics down and bring the uncertainty to the percentage level since our analysis shows that the main source of the systematics is related to kinematics, which heavily depends on the signal-to-noise ratio of the spectra.}, -archivePrefix = {arXiv}, -arxivId = {2212.08463}, -author = {Melo-Carneiro, Carlos R. and Furlanetto, Cristina and Chies-Santos, Ana L.}, -doi = {10.1093/mnras/stad162}, -eprint = {2212.08463}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Melo2023ProbeGR.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cosmology: cosmological parameters,galaxies: kinematics and dynamics,gravitation,gravitational lensing: strong}, -number = {2}, -pages = {1613--1629}, -title = {{Probing general relativity in galactic scales at z ∼ 0.3}}, -volume = {520}, -year = {2023} -} -@article{Dutton2007, -abstract = {We use observed rotation velocity-luminosity (VL) and size-luminosity (RL) relations to single out a specific scenario for disk galaxy formation in the $\Lambda$CDM cosmology. Our model involves four independent lognormal random variables: dark halo concentration c, disk spin $\lambda$gal, disk mass fraction mgal, and stellar mass-to-light ratio $\Upsilon$I. A simultaneous match of the VL and RL zero points with adiabatic contraction requires low-c halos, but this model has V2.2$\sim$1.8Vvir (where V2.2 and Vvir are the circular velocity at 2.2 disk scale lengths and the virial radius, respectively), which will be unable to match the luminosity function (LF). Similarly models without adiabatic contraction but standard c also predict high values of V2.2/Vvir. Models in which disk formation induces an expansion rather than the commonly assumed contraction of the dark matter halos have V2.2$\sim$1.2Vvir, which allows a simultaneous fit of the LF. This may result from nonspherical, clumpy gas accretion, where dynamical friction transfers energy from the gas to the dark matter. This model requires low $\lambda$gal and mgal values, contrary to naive expectations. However, the low $\lambda$gal is consistent with the notion that disk galaxies predominantly survive in halos with a quiet merger history, while a low mgal is also indicated by galaxy-galaxy lensing. The smaller than expected scatter in the RL relation and the lack of correlation between the residuals of the VL and RL relations, respectively, imply that the scatter in $\lambda$gal and in c needs to be smaller than predicted for $\Lambda$CDM halos, again consistent with the idea that disk galaxies preferentially reside in halos with a quiet merger history.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0604553}, -author = {Dutton, Aaron A. and van den Bosch, Frank C. and Dekel, Avishai and Courteau, Stephane}, -doi = {10.1086/509314}, -eprint = {0604553}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Formation,Galaxies: Fundamental Parameters,Galaxies: Spiral,Galaxies: Structure}, -month = {jan}, -number = {1}, -pages = {27--52}, -primaryClass = {astro-ph}, -title = {{A Revised Model for the Formation of Disk Galaxies: Low Spin and Dark Halo Expansion}}, -url = {http://adsabs.harvard.edu/abs/2007ApJ...654...27D}, -volume = {654}, -year = {2007} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M* = 10{\^{}}{\{}10.2{\}} to 10{\^{}}{\{}12.0{\}} solar mass. We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority ({\textgreater}75{\%}) of elliptical galaxies is not well described by a single Sersic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (R{\_}e {\textless} 1 kpc) inner component with luminosity fraction f {\$\sim${}} 0.1-0.15; an intermediate-scale (R{\_}e {\$\sim${}} 2.5 kpc) middle component with f {\$\sim${}} 0.2-0.25; and a dominant (f = 0.6), extended (R{\_}e {\$\sim${}} 10 kpc) outer envelope. All subcomponents have average Sersic indices n {\$\sim${}} 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C and Peng, Chien Y and Li, Zhao Yu and Barth, Aaron J}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{Wang2018c, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of $10^{10.7}\mathrm{M}_{\odot} \leqslant M_{\ast} \leqslant 10^{11.9}\mathrm{M}_{\odot}$ at $z = 0$, the total power-law slope has a mean of $\langle\gamma^{\prime}\rangle = 2.003 \pm 0.008$ and a standard deviation of $\sigma_{\gamma^{\prime}} = 0.175$ over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between $\gamma^{\prime}$ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and $\gamma^{\prime}$ is almost constant with redshift below $z = 2$. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter $c_{200}$ in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, $\gamma_{\mathrm{mw}}^{\prime}-f_{\mathrm{DM}}$, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2018 - Early-type galaxy density profiles from IllustrisTNG I. Galaxy correlations and the impact of baryons(5).pdf:pdf}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {1}, -year = {2018} -} -@article{Vogelsberger2013, -abstract = {We present a multi-epoch analysis of the galaxy populations formed within the cosmological hydrodynamical simulations presented in Vogelsberger et al. These simulations explore the performance of a recently implemented feedback model which includes primordial and metal line radiative cooling with self-shielding corrections; stellar evolution with associated mass-loss and chemical enrichment; feedback by stellar winds; black hole seeding, growth and merging; and active galactic nuclei (AGN) quasar-and radio-mode heating with a phenomenological prescription for AGN electro-magnetic feedback.We illustrate the impact of the model parameter choices on the resulting simulated galaxy population properties at high and intermediate redshifts.We demonstrate that our scheme is capable of producing galaxy populations that broadly reproduce the shape of the observed galaxy stellar mass function extending from redshift z = 0 to z = 3. We also characterize the evolving galactic B-band luminosity function, stellar mass to halo mass ratio, star formation main sequence, Tully-Fisher relation and gas-phase mass-metallicity relation and confront them against recent observational estimates. This detailed comparison allows us to validate elements of our feedback model, while also identifying areas of tension (e.g., the shape and normalization of the mass-metallicity relation and normalization of the star formation main sequence) that will be addressed in future work. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1305.4931}, -author = {Torrey, Paul and Vogelsberger, Mark and Genel, Shy and Sijacki, Debora and Springel, Volker and Hernquist, Lars}, -doi = {10.1093/mnras/stt2295}, -eprint = {1305.4931}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {dec}, -number = {3}, -pages = {1985--2004}, -title = {{A model for cosmological simulations of galaxy formation physics: Multi-epoch validation}}, -url = {http://arxiv.org/abs/1305.2913}, -volume = {438}, -year = {2014} -} -@article{Bolton2008a, -abstract = {We present the definitive data for the full sample of 131 strong gravitational lens candidates observed with the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope by the Sloan Lens ACS (SLACS) Survey. All targets were selected for higher-redshift emission lines and lower-redshift continuum in a single Sloan Digital Sky Survey (SDSS) spectrum. The foreground galaxies are primarily of early-type morphology, with redshifts from approximately 0.05 to 0.5 and velocity dispersions from 160 km/s to 400 km/s; the faint background emission-line galaxies have redshifts ranging from about 0.2 to 1.2. We confirm 70 systems showing clear evidence of multiple imaging of the background galaxy by the foreground galaxy, as well as an additional 19 systems with probable multiple imaging. For 63 clear lensing systems, we present singular isothermal ellipsoid and light-traces-mass gravitational lens models fitted to the ACS imaging data. These strong-lensing mass measurements are supplemented by magnitudes and effective radii measured from ACS surface-brightness photometry and redshifts and velocity dispersions measured from SDSS spectroscopy. These data constitute a unique resource for the quantitative study of the inter-relations between mass, light, and kinematics in massive early-type galaxies. We show that the SLACS lens sample is statistically consistent with being drawn at random from a parent sample of SDSS galaxies with comparable spectroscopic parameters and effective radii, suggesting that the results of SLACS analyses can be generalized to the massive early-type population.}, -archivePrefix = {arXiv}, -arxivId = {0805.1931}, -author = {Bolton, Adam S. and Burles, Scott and Koopmans, L{\'{e}}on V. E. and Treu, Tommaso and Gavazzi, Rapha{\"{e}}l and Moustakas, Leonidas A. and Wayth, Randall and Schlegel, David J.}, -doi = {10.1086/589327}, -eprint = {0805.1931}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Cosmology: Gravitational Lensing,Galaxies: Elliptical and Lenticular,Surveys,cD}, -number = {2}, -pages = {964--984}, -title = {{The Sloan Lens ACS Survey. V. The Full ACS Strong‐Lens Sample}}, -url = {http://arxiv.org/abs/0805.1931%0Ahttp://dx.doi.org/10.1086/589327}, -volume = {682}, -year = {2008} -} -@article{Ma2014, -abstract = {Massive early-type galaxies represent the modern day remnants of the earliest major star formation episodes in the history of the universe. These galaxies are central to our understanding of the evolution of cosmic structure, stellar populations, and supermassive black holes, but the details of their complex formation histories remain uncertain. To address this situation, we have initiated the MASSIVE Survey, a volume-limited, multi-wavelength, integral-field spectroscopic (IFS) and photometric survey of the structure and dynamics of the ∼100 most massive early-type galaxies within a distance of 108 Mpc. This survey probes a stellar mass range M∗ ≳ 1011.5 M⊙ and diverse galaxy environments that have not been systematically studied to date. Our wide-field IFS data cover about two effective radii of individual galaxies, and for a subset of them, we are acquiring additional IFS observations on sub-arcsecond scales with adaptive optics. We are also acquiring deep K-band imaging to trace the extended halos of the galaxies and measure accurate total magnitudes. Dynamical orbit modeling of the combined data will allow us to simultaneously determine the stellar, black hole, and dark matter halo masses. The primary goals of the project are to constrain the black hole scaling relations at high masses, investigate systematically the stellar initial mass function and dark matter distribution in massive galaxies, and probe the late-time assembly of ellipticals through stellar population and kinematical gradients. In this paper, we describe the MASSIVE sample selection, discuss the distinct demographics and structural and environmental properties of the selected galaxies, and provide an overview of our basic observational program, science goals and early survey results.}, -archivePrefix = {arXiv}, -arxivId = {1407.1054}, -author = {Ma, Chung Pei and Greene, Jenny E. and McConnell, Nicholas and Janish, Ryan and Blakeslee, John P. and Thomas, Jens and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/795/2/158}, -eprint = {1407.1054}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ma et al. - 2014 - The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies wi.pdf:pdf}, -isbn = {0000000000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: elliptical and lenticular, cD,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content,galaxies: structure}, -number = {2}, -pages = {158}, -pmid = {28562576}, -title = {{The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...795..158M}, -volume = {795}, -year = {2014} -} -@article{Arcetri2018, -abstract = {We quantify the importance of mass accretion during active galactic nuclei (AGN) phases in the growth of supermassive black holes (BHs) by comparing the mass function of black holes in the Local Universe with that expected from AGN relics, which are black holes grown entirely with mass accretion during AGN phases. The local BH mass function (BHMF) is estimated by applying the well-known correlations between BH mass, bulge luminosity and stellar velocity dispersion to galaxy luminosity and velocity functions. We find that different correlations provide the same BHMF only if they have the same intrinsic dispersion. The density of supermassive black holes in the Local Universe that we estimate is $\rho$BH = 4.6-1.4+1.9h0.72 × 105 M⊙ Mpc-3. The relic BHMF is derived from the continuity equation with the only assumption that AGN activity is due to accretion on to massive BHs and that merging is not important. We find that the relic BHMF at z = 0 is generated mainly at z {\textless} 3 where the major part of the growth of a BH takes place. Moreover, BH growth is antihierarchical in the sense that smaller BHs (MBH {\textless} 10 7 M⊙) grow at lower redshifts (z {\textless} 1) with respect to more massive ones (z ∼ 1-3). Unlike previous work, we find that the BHMF of AGN relics is perfectly consistent with the local BHMF, indicating that local BHs were mainly grown during AGN activity. This agreement is obtained while satisfying, at the same time, the constraints imposed from the X-ray background (XRB). The comparison between the local and relic BHMFs also suggests that the merging process is not important in shaping the relic BHMF, at least at low redshifts (z {\textless} 3), and allows us to estimate the average radiative efficiency (e), the ratio between emitted and Eddington luminosity (A.) and the average lifetime of active BHs. Our analysis thus suggests the following scenario: local BHs grew during AGN phases in which accreting matter was converted into radiation with efficiencies $\epsilon$ = 0.04-0.16 and emitted at a fraction $\Lambda$ = 0.1-1.7 of the Eddington luminosity. The average total lifetime of these active phases ranges from ≃ 4.5 × 108 yr for MBH {\textless} 108 M⊙ to ≃ 1.5 × 108 yr for MBH {\textgreater} 109 M⊙, but can become as large as ∼109 yr for the lowest acceptable $\epsilon$ and $\lambda$values.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0311619}, -author = {Marconi, A and Risaliti, G and Gilli, R and Hunt, L K and Maiolino, R and Salvati, M}, -doi = {10.1111/j.1365-2966.2004.07765.x}, -eprint = {0311619}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cosmology: miscellaneous,Galaxies: active,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -pages = {169--185}, -primaryClass = {astro-ph}, -title = {{Local supermassive black holes, relics of active galactic nuclei and the X-ray background}}, -volume = {351}, -year = {2004} -} -@article{Yang2019a, -abstract = {We use the Illustris simulation to study the distributions of ellipticities and kinematic misalignments of galactic projections, as well as the intrinsic shapes and rotation of the simulated galaxies. Our results for the projections of galaxies display clear trends of an overall increase of kinematic misalignment and a slight decrease of ellipticity for fast rotators with increasing masses, while revealing no clear distinction between slow rotators of different mass. It is also found that the number of very slow rotators with large ellipticities is much larger than found in observations. The intrinsic properties of the galaxies are then analysed. The results for the intrinsic shapes of the galaxies are mostly consistent with previous results inferred from observational data. The distributions of intrinsic misalignment of the galaxies suggest that some of the galaxies produced by Illustris have significant rotation around their medium axes. Further analysis reveals that most of these galaxies display signs of non-equilibrium. We then study the evolution of the intrinsic misalignments and shapes of three specific Illustris galaxies, which we consider as typical ones, along the main progenitor line of their merger trees, revealing how mergers influence the intrinsic shapes and kinematics: the spin axis in general stays close to the shortest axis, and tends to quickly relax to such an equilibrium state within a few dynamical times of the galaxy after major perturbations; triaxiality and intrinsic flatness in general decrease with time, however, sometimes increases occur that are clearly seen to correlate with major merger events.}, -archivePrefix = {arXiv}, -arxivId = {1908.01102}, -author = {Yang, Lisiyuan and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hongyu}, -doi = {10.1093/mnras/stz2156}, -eprint = {1908.01102}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yang et al. - 2019 - Photometric and kinematic misalignments and their evolution among fast and slow rotators in the illustris simulatio.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: kinematics and dynamics,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -number = {1}, -pages = {534--547}, -title = {{Photometric and kinematic misalignments and their evolution among fast and slow rotators in the illustris simulation}}, -volume = {489}, -year = {2019} -} -@article{Tinker2013, -abstract = {We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z = [0.2, 1.0]. For massive galaxies, M ≳ 1010.6 M , our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z = 1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M ∼ 1010 M , the fraction of central galaxies on the red sequence increases by a factor of 10 over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z = 1 to z = 0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency. {\textcopyright}2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1308.2974}, -author = {Tinker, Jeremy L and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H}, -doi = {10.1088/0004-637X/778/2/93}, -eprint = {1308.2974}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: halos}, -number = {2}, -title = {{Evolution of the stellar-to-dark matter relation: Separating star-forming and passive galaxies from z = 1 to 0}}, -volume = {778}, -year = {2013} -} -@article{Gnedin2004, -abstract = {The cooling of gas in the centers of dark matter halos is expected to lead to a more concentrated dark matter distribution. The response of dark matter to the condensation of baryons is usually calculated using the model of adiabatic contraction, which assumes spherical symmetry and circular orbits. In contrast, halos in the hierarchical structure formation scenarios grow via multiple violent mergers and accretion along filaments, and particle orbits in the halos are highly eccentric. We study the effects of the cooling of gas in the inner regions of halos using high-resolution cosmological simulations which include gas dynamics, radiative cooling, and star formation. We find that the dissipation of gas indeed increases the density of dark matter and steepens its radial profile in the inner regions of halos compared to the case without cooling. For the first time, we test the adiabatic contraction model in cosmological simulations and find that the standard model systematically overpredicts the increase of dark matter density in the inner 5% of the virial radius. We show that the model can be improved by a simple modification of the assumed invariant from M(r)r to M(rav)r, where r and rav are the current and orbit-averaged particle positions. This modification approximately accounts for orbital eccentricities of particles and reproduces simulation profiles to within 10-20%. We present analytical fitting functions that accurately describe the transformation of the dark matter profile in the modified model and can be used for interpretation of observations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0406247}, -author = {Gnedin, Oleg Y and Kravtsov, Andrey V and Klypin, Anatoly A and Nagai, Daisuke}, -doi = {10.1086/424914}, -eprint = {0406247}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Theory,Galaxies: Formation,Galaxies: Halos,Methods: Numerical}, -number = {1}, -pages = {12}, -primaryClass = {astro-ph}, -title = {{Response of dark matter halos to condensation of baryons: cosmological simulations and improved adiabatic contraction model}}, -url = {http://arxiv.org/abs/astro-ph/0406247}, -volume = {616}, -year = {2004} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright} 2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel, Sari, Ceverino - 2009 - Formation of massive galaxies at high redshift Cold streams, clumpy disks, and compact spheroids(2).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of consistent stellar parameters and abundances ('stellar labels') for hundreds of thousands of stars in the Milky Way: this poses a formidable spectral modeling challenge. In many cases, there is a sub-set of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the 'known' labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with Teff, log g and [Fe/H] as the labels, and then applying it to the spectra of 56,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ness, M and Hogg, David W and Rix, H W and Ho, Anna Y Q and Zasowski, G}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{THE CANNON: A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION}}, -volume = {808}, -year = {2015} -} -@article{Cole2011, -abstract = {We consider the infall of a massive clump into a dark matter halo as a simple and extreme model for the effect of baryonic physics (neglected in gravity-only simulations of large-scale structure formation) on the dark matter. We find that such an infalling clump is extremely efficient in altering the structure of the halo and reducing its central density: a clump of 1 per cent the mass of the halo can remove about twice its own mass from the inner halo and transform a cusp into a core or weaker cusp. If the clump is subsequently removed, mimicking a galactic wind, the central halo density is further reduced and the mass removed from the inner halo doubled. Lighter clumps are even more efficient: the ratio of removed mass to clump mass increases slightly towards smaller clump masses. This process becomes more efficient the more radially anisotropic the initial dark matter velocities are. While such a clumpy infall may be somewhat unrealistic, it demonstrates that the baryons need to transfer only a small fraction of their initial energy to the dark matter via dynamical friction to explain the discrepancy between predicted dark matter density profiles and those inferred from observations of dark-matter-dominated galaxies. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1105.4050}, -author = {Cole, David R. and Dehnen, Walter and Wilkinson, Mark I.}, -doi = {10.1111/j.1365-2966.2011.19110.x}, -eprint = {1105.4050}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxies: haloes,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {1118--1134}, -title = {{Weakening dark matter cusps by clumpy baryonic infall}}, -volume = {416}, -year = {2011} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as 'notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude (<50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 < G < 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G. M. and Prod'homme, T. and Murray, N. J. and Crowley, C. and Hopkinson, G. and Brown, A. G.A. and Kohley, R. and Holland, A.}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Seabroke et al. - 2013 - Digging supplementary buried channels Investigating the notch architecture within the CCD pixels on ESA's Gaia.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Rusin2005, -abstract = {The supermassive black hole at the center of a distant galaxy can be weighed, in rare but realistic cases, when the galaxy acts as a strong gravitational lens. The central image that should be produced by the lens is either destroyed or accompanied by a second central image, depending on the mass of the black hole. We demonstrate that when a central image pair is detected, the mass of the black hole can be determined with an accuracy of < 0.1 dex, if the form of the smooth mass distribution near the galaxy core is known. Uncertainty in the central mass distribution introduces a systematic error in the black hole mass measurement. However, even with nearly complete ignorance of the inner mass distribution, the black hole mass can still be determined to within a factor of 10. Central image pairs should be readily observable with future radio interferometers, allowing this technique to be used for a census of supermassive black holes in inactive galaxies at significant redshift (0.2 < z < 1.0).}, -author = {Rusin, David and Keeton, Charles R. and Winn, Joshua N.}, -doi = {10.1086/432439}, -issn = {0004-637X}, -journal = {ApJ}, -number = {2}, -pages = {L93--L96}, -title = {{Measuring Supermassive Black Holes in Distant Galaxies with Central Lensed Images}}, -volume = {627}, -year = {2005} -} -@article{Naab2009, -abstract = {Using a high-resolution hydrodynamical cosmological simulation of the formation of a massive spheroidal galaxy we show that elliptical galaxies can be very compact and massive at high redshift in agreement with recent observations. Accretion of stripped infalling stellar material increases the size of the system with time and the central concentration is reduced by dynamical friction of the surviving stellar cores. In a specific case of a spheroidal galaxy with a final stellar mass of 1.5 × 1011 M ⊙ we find that the effective radius re increases from 0.7 ± 0.2 kpc at z = 3 to re = 2.4 ± 0.4 kpc at z = 0 with a concomitant decrease in the effective density of an order of magnitude and a decrease of the central velocity dispersion by approximately 20% over this time interval. A simple argument based on the virial theorem shows that during the accretion of weakly bound material (minor mergers) the radius can increase as the square of the mass in contrast to the usual linear rate of increase for major mergers. By undergoing minor mergers compact high-redshift spheroids can evolve into present-day systems with sizes and concentrations similar to observed local ellipticals. This indicates that minor mergers may be the main driver for the late evolution of sizes and densities of early-type galaxies. {\textcopyright} 2009 The American Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {0903.1636}, -author = {Naab, Thorsten and Johansson, Peter H. and Ostriker, Jeremiah P.}, -doi = {10.1088/0004-637X/699/2/L178}, -eprint = {0903.1636}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Naab, Johansson, Ostriker - 2010 - Minor mergers and the size evolution of elliptical galaxies.pdf:pdf}, -issn = {2041-821}, -journal = {Astrophysical Journal Letters}, -keywords = {Galaxies: elliptical and lenticular, cd,Galaxies: evolution,Galaxies: interactions,Galaxies: structure,Methods: numerical}, -month = {jul}, -number = {2 PART 2}, -pages = {L178----L182}, -title = {{Minor mergers and the size evolution of elliptical galaxies}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L178?key=crossref.405faa44137f4be9a7e3800a4c3e7dea}, -volume = {699}, -year = {2010} -} -@article{Li2017, -abstract = {We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier {\$}\backslashrm ATLAS{\^{}}{\{}3D{\}}{\$} results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients.}, -archivePrefix = {arXiv}, -arxivId = {1703.04894}, -author = {Li, Hongyu and Ge, Junqiang and Mao, Shude and Cappellari, Michele and Long, R J and Li, Ran and Emsellem, Eric and Dutton, Aaron A and Li, Cheng and Bundy, Kevin and Thomas, Daniel and Drory, Niv and Lopes, Alexandre Roman}, -doi = {10.3847/1538-4357/aa662a}, -eprint = {1703.04894}, -isbn = {0004-637X}, -issn = {1538-4357}, -pages = {1--9}, -title = {{SDSS-IV MaNGA: variation of the stellar initial mass function in spiral and early-type galaxies}}, -url = {http://arxiv.org/abs/1703.04894%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa662a}, -year = {2017} -} -@article{Nightingale2019, -abstract = {We investigate how strong gravitational lensing can test contemporary models of massive elliptical (ME) galaxy formation, by combining a traditional decomposition of their visible stellar distribution with a lensing analysis of their mass distribution. As a proof of concept, we study a sample of three ME lenses, observing that all are composed of two distinct baryonic structures, a 'red' central bulge surrounded by an extended envelope of stellar material. Whilst these two components look photometrically similar, their distinct lensing effects permit a clean decomposition of their mass structure. This allows us to infer two key pieces of information about each lens galaxy: (i) the stellar mass distribution (without invoking stellar populations models) and (ii) the inner dark matter halo mass. We argue that these two measurements are crucial to testing models of ME formation, as the stellar mass profile provides a diagnostic of baryonic accretion and feedback whilst the dark matter mass places each galaxy in the context of LCDM large-scale structure formation. We also detect large rotational offsets between the two stellar components and a lopsidedness in their outer mass distributions, which hold further information on the evolution of each ME. Finally, we discuss how this approach can be extended to galaxies of all Hubble types and what implication our results have for studies of strong gravitational lensing.}, -archivePrefix = {arXiv}, -arxivId = {1901.07801}, -author = {Nightingale, James W. and Massey, Richard J. and Harvey, David R. and Cooper, Andrew P. and Etherington, Amy and Tam, Sut Ieng and Hayes, Richard G.}, -doi = {10.1093/mnras/stz2220}, -eprint = {1901.07801}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Nightingale et al. - 2019 - Galaxy structure with strong gravitational lensing Decomposing the internal mass distribution of massive (5).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: Evolution,Galaxies: Formation,Gravitational lensing: Strong}, -number = {2}, -pages = {2049--2068}, -title = {{Galaxy structure with strong gravitational lensing: Decomposing the internal mass distribution of massive elliptical galaxies}}, -url = {http://arxiv.org/abs/1901.07801}, -volume = {489}, -year = {2019} -} -@article{Viel2013, -abstract = {We present updated constraints on the free-streaming of warm dark matter (WDM) particles derived from an analysis of the Lyman-$\alpha$ flux power spectrum measured from high-resolution spectra of 25 z{\textgreater}4 quasars obtained with the Keck High Resolution Echelle Spectrometer and the Magellan Inamori Kyocera Echelle spectrograph. We utilize a new suite of high-resolution hydrodynamical simulations that explore WDM masses of 1, 2 and 4 keV (assuming the WDM consists of thermal relics), along with different physically motivated thermal histories. We carefully address different sources of systematic error that may affect our final results and perform an analysis of the Lyman-$\alpha$ flux power with conservative error estimates. By using a method that samples the multidimensional astrophysical and cosmological parameter space, we obtain a lower limit mWDM{\^{a}}‰3.3 keV (2$\sigma$) for warm dark matter particles in the form of early decoupled thermal relics. Adding the Sloan Digital Sky Survey Lyman-$\alpha$ flux power spectrum does not improve this limit. Thermal relics of masses 1, 2 and 2.5 keV are disfavored by the data at about the 9$\sigma$, 4$\sigma$ and 3$\sigma$ C.L., respectively. Our analysis disfavors WDM models where there is a suppression in the linear matter power spectrum at (nonlinear) scales corresponding to k=10h/Mpc which deviates more than 10{\%} from a Lambda cold dark matter model. Given this limit, the corresponding "free-streaming mass" below which the mass function may be suppressed is ∼2×108h-1M {\^{a}}{\v{S}}™. There is thus very little room for a contribution of the free-streaming of WDM to the solution of what has been termed the small scale crisis of cold dark matter. {\textcopyright}2013 American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {1306.2314}, -author = {Viel, Matteo and Becker, George D and Bolton, James S and Haehnelt, Martin G}, -doi = {10.1103/PhysRevD.88.043502}, -eprint = {1306.2314}, -issn = {15507998}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -number = {4}, -pages = {1--20}, -title = {{Warm dark matter as a solution to the small scale crisis: New constraints from high redshift Lyman-$\alpha$ forest data}}, -volume = {88}, -year = {2013} -} -@article{Tinker2016, -abstract = {We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen etal (2012) clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of Mgal for galaxies with logMgal{\textgreater}=11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma{\_}logM. Using this approach, we find sigma{\_}logM=0.18{\^{}}{\{}+0.01{\}}{\_}{\{}-0.02{\}}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L and Brownstein, Joel R and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -issn = {1538-4357}, -title = {{The Correlation Between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -year = {2016} -} -@article{DiCintio2014, -abstract = {We use a suite of 31 simulated galaxies drawn from the MaGICC project to investigate the effects of baryonic feedback on the density profiles of dark matter haloes. The sample covers a wide mass range: 9.4×109 =11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma_logM. Using this approach, we find sigma_logM=0.18^{+0.01}_{-0.02}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L. and Brownstein, Joel R. and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D. and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D.}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tinker et al. - 2017 - The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {121}, -title = {{The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -volume = {839}, -year = {2017} -} -@article{LeFloch2005, -abstract = {We analyze a sample of $\sim$2600 MIPS/Spitzer 24mic sources brighter than $\sim$80muJy and located in the Chandra Deep Field South to characterize the evolution of the comoving infrared (IR) energy density of the Universe up to z$\sim$1. Using published ancillary optical data we first obtain a nearly complete redshift determination for the 24mic objects associated with R<24 counterparts at z<1. We find that the 24mic population at 0.5 10^11 L_IR) are responsible for 70+/-15% of this energy density at z$\sim$1. Taking into account the contribution of the UV luminosity evolving as (1+z)^$\sim$2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z$\sim$0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24mic fluxes into luminosities.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506462}, -author = {{Le Floc'h}, Emeric and Papovich, Casey and Dole, Herve and Bell, Eric F. and Lagache, Guilaine and Rieke, George H. and Egami, Eiichi and Perez‐Gonzalez, Pablo G. and Alonso‐Herrero, Almudena and Rieke, Marcia J. and Blaylock, Myra and Engelbracht, Charles W. and Gordon, Karl D. and Hines, Dean C. and Misselt, Karl A. and Morrison, Jane E. and Mould, Jeremy}, -doi = {10.1086/432789}, -eprint = {0506462}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Observations,Galaxies: Evolution,Galaxies: High-Redshift,Infrared: Galaxies}, -month = {oct}, -number = {1}, -pages = {169--190}, -primaryClass = {astro-ph}, -title = {{ Infrared Luminosity Functions from the Chandra Deep Field–South: The Spitzer View on the History of Dusty Star Formation at 0 ≲ z ≲ 1 }}, -url = {http://arxiv.org/abs/astro-ph/0506462%0Ahttp://dx.doi.org/10.1086/432789}, -volume = {632}, -year = {2005} -} -@article{Geometryef, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(8).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Costantin2017, -abstract = {Context. The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. Aims. We aim to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. Methods. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the i-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new (B=A, C=A) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. Results. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations of 25° ≤ $\theta$ ≤ 65° we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66{\%}), with a smaller fraction of prolate spheroids (19{\%}), and triaxial ellipsoids (15{\%}). The majority of triaxial bulges are in barred galaxies (75{\%}). Moreover, we found that bulges with low S{\'{e}}rsic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, bulges in late-type galaxies or in less massive galaxies have no preference for being oblate, prolate, or triaxial. On the contrary, bulges with high S{\'{e}}rsic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. Conclusions. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L and M{\'{e}}ndez-Abreu, J and Corsini, E M and Eliche-Moral, M C and Tapia, T and Morelli, L and Elena, Dalla Bont{\`{a}} and Pizzella, A}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -volume = {609}, -year = {2018} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centres of typical $\sim$ L* and lower mass spheroids exhibit power-law 'cusps' with $\Sigma$ $\alpha$ R-$\eta$, where 0.5 ≲ $\eta$ ≲ 1 for radii $\sim$ 1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for, or strongly modify, the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m = 1 lopsided/eccentric disc instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*(< R) « MBH. When the stellar surface density profile is comparatively shallow with $\eta$ < 1/2, the modes cannot efficiently propagate to R = 0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than $\eta$ = 1, the inward propagation of eccentricity is strongly damped, suppressing inflow and bringing $\eta$ down again. Together these results produce an equilibrium slope of 1/2 ≲ $\eta$ ≲ 1 in the potential of the central black hole. These physical arguments are supported by non-linear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies. {\textcopyright} 2010 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F. and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins, Quataert - 2011 - An explanation for the slopes of stellar cusps in galaxy spheroids.pdf:pdf}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter (CDM) galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes possess a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a $\Lambda$CDM universe. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R and Eke, Vincent R and Frenk, Carlos S and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{Yan2016, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R{\$\sim${}}2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is {\$\sim${}}73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R and Bershady, Matthew A and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R and Thomas, Daniel and Wake, David A and Weijmans, Anne-Marie and Westfall, Kyle B and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A and Blanton, Michael R and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T and Goddard, Daniel and Gunn, James E and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R and Oravetz, Daniel and Pan, Kaike and Parejko, John K and Sanchez, Sebastian F and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -title = {{SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality}}, -url = {http://arxiv.org/abs/1607.08613%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {197}, -year = {2016} -} -@article{Hopkins2011b, -abstract = {Feedback from massive stars is believed to play a critical role in shaping the galaxy mass function, the structure of the interstellar medium (ISM), and the low efficiency of star formation, but the exact form of the feedback is uncertain. In this paper, the first in a series, we present and test a novel numerical implementation of stellar feedback resulting from momentum imparted to the ISM by radiation, supernovae, and stellar winds. We employ a realistic cooling function, and find that a large fraction of the gas cools to {\textless}100K, so that the ISM becomes highly inhomogeneous. Despite this, our simulated galaxies reach an approximate steady state, in which gas gravitationally collapses to form giant molecular clouds (GMCs), dense clumps, and stars; subsequently, stellar feedback disperses the GMCs, repopulating the diffuse ISM. This collapse and dispersal cycle is seen in models of SMC-like dwarfs, the Milky-Way, and z{\$\sim${}}2 clumpy disk analogues. The simulated global star formation efficiencies are consistent with the observed Kennicutt-Schmidt relation. Moreover, the star formation rates are nearly independent of the numerically imposed high-density star formation efficiency, density threshold, and density scaling. This is a consequence of the fact that, in our simulations, star formation is regulated by stellar feedback limiting the amount of very dense gas available for forming stars. In contrast, in simulations without stellar feedback, i.e. under the action of only gravity and gravitationally-induced turbulence, the ISM experiences runaway collapse to very high densities. In these simulations without feedback, the global star formation rates exceed observed galactic star formation rates by 1-2 orders of magnitude, demonstrating that stellar feedback is crucial to the regulation of star formation in galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1101.4940}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2011.19306.x}, -eprint = {1101.4940}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation}, -number = {2}, -pages = {950--973}, -title = {{Self-regulated star formation in galaxies via momentum input from massive stars}}, -volume = {417}, -year = {2011} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Birrer2015b, -abstract = {We present a strong lensing modeling technique based on versatile basis sets for the lens and source planes. Our method uses high performance Monte Carlo algorithms, allows for an adaptive build up of complexity and bridges the gap between parametric and pixel based reconstruction methods. We apply our method to a HST image of the strong lens system RXJ1131-1231 and show that our method finds a reliable solution and is able to detect substructure in the lens and source planes simultaneously. Using mock data we show that our method is sensitive to sub-clumps with masses four orders of magnitude smaller than the main lens, which corresponds to about $10^8 M_{\odot}$, without prior knowledge on the position and mass of the sub-clump. The modelling approach is flexible and maximises automation to facilitate the analysis of the large number of strong lensing systems expected in upcoming wide field surveys. The resulting search for dark sub-clumps in these systems, without mass-to-light priors, offers promise for probing physics beyond the standard model in the dark matter sector.}, -archivePrefix = {arXiv}, -arxivId = {1504.07629}, -author = {Birrer, Simon and Amara, Adam and Refregier, Alexandre}, -doi = {10.1088/0004-637X/813/2/102}, -eprint = {1504.07629}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmological parameters,distance scale,gravitational lensing: strong,methods: numerical}, -number = {2}, -pages = {102}, -title = {{GRAVITATIONAL LENS MODELING with BASIS SETS}}, -url = {http://stacks.iop.org/0004-637X/813/i=2/a=102?key=crossref.b6824f4280340fdc0fa018ab63d85879}, -volume = {813}, -year = {2015} -} -@article{LaBarbera2010, -abstract = {We present an analysis of stellar population gradients in 4546 early-type galaxies (ETGs) with photometry in grizYHJK along with optical spectroscopy. ETGs were selected as bulge-dominated systems, displaying passive spectra within the SDSS fibers. A new approach is described which utilizes color information to constrain age and metallicity gradients. Defining an effective color gradient, ∇*, which incorporates all of the available color indices, we investigate how ∇* varies with galaxy mass proxies, i.e., velocity dispersion, stellar (M*) and dynamical (Mdyn) masses, as well as age, metallicity, and [$\alpha$/Fe]. ETGs with Mdyn larger than 8.5 × 1010 M⊙ have increasing age gradients and decreasing metallicity gradients with respect to mass, metallicity, and enhancement. We find that velocity dispersion and [$\alpha$/Fe] are the main drivers of these correlations. ETGs with 2.5 × 10 10 Ṁ ≤ Mdyn ≤ 8.5 × 10 10 M⊙ show no correlation of age, metallicity, and color gradients with respect to mass, although color gradients still correlate with stellar population parameters, and these correlations are independent of each other. In both mass regimes, the striking anti-correlation between color gradient and $\alpha$-enhancement is significant at ∼5$\sigma$ and results from the fact that metallicity gradient decreases with [$\alpha$/Fe]. This anti-correlation may reflect the fact that star formation and metallicity enrichment are regulated by the interplay between the energy input from supernovae, and the temperature and pressure of the hot X-ray gas in ETGs. For all mass ranges, positive age gradients are associated with old galaxies (>5-7 Gyr). For galaxies younger than ∼5 Gyr, mostly at low mass, the age gradient tends to be anti-correlated with the Age parameter, with more positive gradients at younger ages.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1006.4056}, -author = {Barbera, F. La and {De Carvalho}, R. R. and {De La Rosa}, I. G. and Gal, R. R. and Swindle, R. and Lopes, P. A.A.}, -doi = {10.1088/0004-6256/140/5/1528}, -eprint = {1006.4056}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Evolution - Galaxies,Formation - Galaxies,Fundamental parameters,Galaxies}, -month = {nov}, -number = {5}, -pages = {1528--1556}, -primaryClass = {astro-ph.CO}, -title = {{Spider. IV. Optical and near-infrared color gradients in early-type galaxies: New insight into correlations with galaxy properties}}, -url = {http://stacks.iop.org/1538-3881/140/i=5/a=1528?key=crossref.aeafeae7d16ab184d33f1707803b9e32}, -volume = {140}, -year = {2010} -} -@article{Griffiths2025, -abstract = {Machine learning (ML) and artificial intelligence (AI) methods are increasingly used in personalized medicine, including precision oncology. Ma et al. (Nature Cancer 2021) developed a new method c alled "Transfer of Cell Line Response Prediction" (TCRP) to train predictors of drug response in cancer cell lines and optimize their performance in higher complex cancer model systems via few-shot learning. TCRP was presented as a successful modeling approach in multiple case studies. Given the importance of this approach to assist clinicians in their treatment decision process, we sought to reproduce independently the authors' findings and improve the reusability of TCRP in new case studies, including validation in clinical trial datasets, a high bar for drug response prediction. Our results support the superiority of TCRP over established statistical and machine learning approaches in preclinical and clinical settings. We developed new resources to increase the reusability of the TCRP model for future improvements and validation studies.}, -author = {Griffiths, M and Kubeyev, A and Laurie, J and MedRxiv, A Giorni - and 2024, Undefined}, -file = {:C\:/Users/Jammy/Documents/Papers/Medical/Concr2024.pdf:pdf}, -journal = {medarxiv}, -pages = {1--29}, -title = {{Computational prediction of therapeutic response and cancer outcomes}}, -url = {https://www.medrxiv.org/content/10.1101/2024.01.17.24301444.abstract}, -year = {2025} -} -@article{Governato2015, -abstract = {We use high resolution Hydro{\$}+{\$}N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass {\$\sim${}} 10{\$}{\^{}}{\{}6-7{\}}{\$} M{\$}\backslashodot{\$}, total mass 10{\$}{\^{}}{\{}10{\}}{\$} M{\$}\backslashodot{\$} in {\$}\backslashLambda{\$} dominated CDM and 2keV WDM cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the DM model, but proportionally to the SF efficiency, gas outflows lower the central mass density through `dynamical heating', such that all realizations have circular velocities {\$}{\textless}{\$} 20kms at 500{\$}{\\sim{}}{\$}pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial color-magnitude diagrams and star formation histories in order to directly compare to available observations. The simulated galaxies formed most of their stars in many {\$}\backslashsim{\$}10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including `baryon physics' in simulations when 1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and 2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F and Weisz, D and Pontzen, A and Loebman, S and Reed, D and Brooks, A M and Behroozi, P and Christensen, C and Madau, P and Mayer, L and Shen, S and Walker, M and Quinn, T and Keller, B W and Wadsley, J}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum {\$}j{\_}\backslashstar{\$} and the stellar mass {\$}M{\_}\backslashstar{\$} in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction {\$}f{\_}{\{}\backslashrm inf{\}}{\$} of baryons that infall toward the central regions of galaxies where star formation can occur. We find {\$}f{\_}{\{}\backslashrm inf{\}}\backslashapprox 1{\$} for LTGs and {\$}\backslashapprox 0.4{\$} for ETGs with an uncertainty of about {\$}0.25{\$} dex, consistent with a biased collapse. By comparing with the locally observed {\$}j{\_}\backslashstar{\$} vs. {\$}M{\_}\backslashstar{\$} relations for LTGs and ETGs we estimate the fraction {\$}f{\_}j{\$} of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find {\$}f{\_}j\backslashapprox 1.11{\^{}}{\{}+0.75{\}}{\_}{\{}-0.44{\}}{\$}, in line with the classic disc formation picture; for ETGs we infer {\$}f{\_}j\backslashapprox 0.64{\^{}}{\{}+0.20{\}}{\_}{\{}-0.16{\}}{\$}, that can be traced back to a {\$}z{\textless}1{\$} evolution via dry mergers. We also show that the observed scatter in the {\$}j{\_}{\{}\backslashstar{\}}{\$} vs. {\$}M{\_}{\{}\backslashstar{\}}{\$} relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at {\$}z\backslashsim 2{\$} is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, J and Lapi, A and Mancuso, C and Wang, H and Danese, L}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {2}, -pages = {105}, -title = {{Angular Momentum of Early- and Late-type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -volume = {843}, -year = {2017} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the Tiger principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper reports on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R and Copin, Y and Monnet, G and Miller, Bryan W and Allington-Smith, J R and Bureau, M and Carollo, C Marcella and Davies, Roger L and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F and Verolme, E K and {De Zeeuw}, P Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs,cD}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{Baugh:1996aa, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an Omega=1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0{\textless}=z{\textless}=0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z=0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z=0 rich clusters become E/S0 dominated, and we find a `Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z{\$\sim${}}=1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -author = {{Baugh, C. M.} and {Cole, S.} and {Frenk, C. S.}}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {GALAXIES: EVOLUTION,GALAXIES: FORMATION,GALAXIES: LUMINOSITY FUNCTION,MASS FUNCTION}, -month = {dec}, -number = {4}, -pages = {1361--1378}, -title = {{Evolution of the Hubble sequence in hierarchical models for galaxy formation}}, -url = {http://adsabs.harvard.edu/abs/1996MNRAS.283.1361B}, -volume = {283}, -year = {1996} -} -@article{Rauch1998, -abstract = {Observations of redshifted Lyman $\alpha$ (Ly$\alpha$) forest absorption in the spectra of quasistellar objects (QSOs) provide a highly sensitive probe of the distribution of gaseous matter in the universe. Over the past two decades, optical spectroscopy with large ground-based telescopes, and more recently ultraviolet (UV) spectroscopy from space, have yielded a wealth of information on what appears to be a gaseous, photoionized intergalactic medium (IGM), partly enriched by the products of stellar nucleosynthesis, residing in coherent structures over many hundreds of kiloparsecs. Recent progress with cosmological hydro-simulations based on hierarchical structure formation models has led to important insights into the physical structures giving rise to the forest. If these ideas are correct, a truly inter-and protogalactic medium [at high redshift (z ∼ 3), the main repository of baryons] collapses under the influence of dark matter gravity into flattened or filamentary structures, which are seen in absorption against background QSOs. With decreasing redshift, galaxies forming in the denser regions may contribute an increasing part of the Ly$\alpha$ absorption cross section. Comparisons between large data samples from the new generation of telescopes and artificial Ly$\alpha$ forest spectra from cosmological simulations promise to become a useful cosmological tool.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9806286}, -author = {Rauch, Michael}, -doi = {10.1146/annurev.astro.36.1.267}, -eprint = {9806286}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {Cosmology,Galaxy formation,Intergalactic medium (IGM),Quasistellar object (QSO) absorption lines,Ultraviolet background radiation}, -number = {1}, -pages = {267--316}, -primaryClass = {astro-ph}, -title = {{The Lyman alpha forest in the spectra of quasistellar objects}}, -url = {http://arxiv.org/abs/astro-ph/9806286%0Ahttp://dx.doi.org/10.1146/annurev.astro.36.1.267}, -volume = {36}, -year = {1998} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-$\alpha$ emission from the host galaxy of SDSS$\sim$J2222+2745, a strongly lensed quasar at $z = 2.8$. Spectroscopic follow-up clearly reveals extended Lyman-$\alpha$ in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as $\sim$200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-$\alpha$ emission to its physical origin on one side of the host galaxy at radii $\sim$0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-$\alpha$ and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-$\alpha$, host galaxy Lyman-$\alpha$, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B. and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D. and Rigby, Jane R. and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bayliss et al. - 2017 - Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy(2).pdf:pdf}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M{\textgreater}10{\^{}}11 M{\_}sun) galaxies at 1.7{\textless}z{\textless}3 utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our sample is almost an order of magnitude larger than previous studies at these redshifts, providing the first statistical study of massive galaxy sizes at z{\textgreater}2, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n{\textless}2) and spheroid-like (n{\textgreater}2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z{\$\sim${}}2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z{\textgreater}2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ({\$\sim${}}2x10{\^{}}10 M{\_}sun kpc{\^{}}-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J and Bouwens, Rychard J and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -isbn = {1005-0302}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61----L64}, -title = {{ Size Evolution of the Most Massive Galaxies at 1.7 {\textless} z {\textless} 3 from GOODS NICMOS Survey Imaging }}, -url = {http://arxiv.org/abs/0807.4141%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as 'notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude ({\textless}50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 {\textless} G {\textless} 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G M and Prod'homme, T and Murray, N J and Crowley, C and Hopkinson, G and Brown, A G A and Kohley, R and Holland, A}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Bullock:2005aa, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {dec}, -number = {2}, -pages = {931--949}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Smith2017a, -abstract = {Abell 1201 is a massive galaxy cluster at z = 0.169 with a brightest cluster galaxy (BCG) that acts as a gravitational lens to a background source at z = 0.451. The lensing configuration is unusual, with a single bright arc formed at small radius (∼2 arcsec), where stars and dark matter are both expected to contribute substantially to the total lensing mass. Here, we present deep spectroscopic observations of the Abell 1201 BCG with MUSE (Multi-Unit Spectroscopic Explorer), which reveal emission lines from a faint counterimage, opposite to the main arc, at a radius of 0.6 arcsec. We explore models in which the lensing mass is described by a combination of stellar mass and a standard dark matter halo. The counterimage is not predicted in such models, unless the dark matter component is negligible, which would imply an extremely heavy stellar initial mass function (IMF) in this galaxy. We consider two modifications to the model, which can produce the observed configuration without resorting to extreme IMFs. Imposing a radial gradient in the stellar mass-to-light ratio, ϒ, can generate a counterimage close to the observed position if ϒ increases by ≳60 per cent within the inner ∼1 arcsec (e.g. variation from a Milky Way-like to a Salpeter-like IMF). Alternatively, the counterimage can be produced by introducing a central supermassive black hole. The required mass is MBH = (1.3 ± 0.6) × 1010 M☉, which is comparable to the largest black holes known to date, several of which are also hosted by BCGs. We comment on future observations that promise to distinguish between these alternatives.}, -archivePrefix = {arXiv}, -arxivId = {1701.02745}, -author = {Smith, Russell J. and Lucey, John R. and Edge, Alastair C.}, -doi = {10.1093/mnras/stx059}, -eprint = {1701.02745}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Smith2017CounterImageAbell1201.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cd,Galaxies: clusters: individual: Abell 1201,Galaxies: elliptical,Gravitational lensing: strong,Lenticular}, -number = {1}, -pages = {836--848}, -title = {{A counterimage to the gravitational arc in Abell 1201: Evidence for IMF variations, or a 1010 M☉ black hole?★†}}, -volume = {467}, -year = {2017} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ({\$}z = 1.489{\$}), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5{\$}+{\$}2223 ({\$}z = 0.542{\$}), published by Grillo et al. (2016), and explore different {\$}\backslashLambda{\$}CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of {\$}H{\_}{\{}0{\}}{\$} and {\$}\backslashOmega{\_}{\{}\backslashrm m{\}}{\$} with relative (1{\$}\backslashsigma{\$}) statistical errors of, respectively, 6{\%} (7{\%}) and 31{\%} (26{\%}) in flat (general) cosmological models, assuming a conservative 3{\%} uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of {\$}H{\_}{\{}0{\}}{\$}, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C and Rosati, P and Suyu, S H and Balestra, I and Caminha, G B and Halkola, A and Kelly, P L and Lombardi, M and Mercurio, A and Rodney, S A and Treu, T}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -number = {2}, -pages = {94}, -title = {{Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”}}, -url = {http://arxiv.org/abs/1802.01584}, -volume = {860}, -year = {2018} -} -@article{Dye2017, -abstract = {We have modelled $\sim$0.1 arcsec resolution Atacama Large Millimetre/submillimeter Array imaging of six strong gravitationally lensed galaxies detected by the Herschel Space Observatory. Our modelling recovers mass properties of the lensing galaxies and, by determining magnification factors, intrinsic properties of the lensed submillimetre sources. We find that the lensed galaxies all have high ratios of star formation rate to dust mass, consistent with or higher than the mean ratio for high-redshift submillimetre galaxies and low-redshift ultraluminous infrared galaxies. Source reconstruction reveals that most galaxies exhibit disturbed morphologies. Both the cleaned image plane data and the directly observed interferometric visibilities have been modelled, enabling comparison of both approaches. In the majority of cases, the recovered lens models are consistent between methods, all six having mass density profiles that are close to isothermal. However, one system with poor signal to noise shows mildly significant differences.}, -archivePrefix = {arXiv}, -arxivId = {1705.05413}, -author = {Dye, S. and Furlanetto, C. and Dunne, L. and Eales, S. A. and Negrello, M. and Nayyeri, H. and van der Werf, P. P. and Serjeant, S. and Farrah, D. and Micha{\l}owski, M. J. and Baes, M. and Marchetti, L. and Cooray, A. and Riechers, D. A. and Amvrosiadis, A.}, -doi = {10.1093/mnras/sty513}, -eprint = {1705.05413}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dye et al. - 2018 - Modelling high-resolution ALMA observations of strongly lensed highly star-forming galaxies detected by Herschel(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {4}, -pages = {4383--4394}, -title = {{Modelling high-resolution ALMA observations of strongly lensed highly star-forming galaxies detected by Herschel}}, -volume = {476}, -year = {2018} -} -@article{Lam2015, -abstract = {Dynamic, interpreted languages, like Python, are attractive for domain-experts and scientists experimenting with new ideas. However, the performance of the interpreter is of-ten a barrier when scaling to larger data sets. This paper presents a just-in-time compiler for Python that focuses in scientific and array-oriented computing. Starting with the simple syntax of Python, Numba compiles a subset of the language into efficient machine code that is comparable in performance to a traditional compiled language. In addi-tion, we share our experience in building a JIT compiler using LLVM[1].}, -author = {Lam, Siu Kwan and Pitrou, Antoine and Seibert, Stanley}, -doi = {10.1145/2833157.2833162}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lam, Pitrou, Seibert - 2015 - Numba.pdf:pdf}, -isbn = {9781450340052}, -journal = {Proceedings of the Second Workshop on the LLVM Compiler Infrastructure in HPC - LLVM '15}, -keywords = {2,a jit for numeric,com-,compiler,jit,just-in-time,llvm,numba is a function-at-a-time,python}, -pages = {1--6}, -title = {{Numba}}, -url = {http://dl.acm.org/citation.cfm?doid=2833157.2833162}, -year = {2015} -} -@article{Gadotti2008a, -abstract = {We have performed 2D bulge/bar/disc decompositions using g, r and i-band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for bulge-to-total ratio than the global Sersic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour-magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between bulge Sersic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass-size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass-size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs.}, -archivePrefix = {arXiv}, -arxivId = {0810.1953}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2008.14257.x}, -eprint = {0810.1953}, -isbn = {0372-9311 (Print)$\backslash$r0372-9311 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {1531--1552}, -pmid = {20063786}, -title = {{Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: A Sloan Digital Sky Survey perspective}}, -url = {http://arxiv.org/abs/0810.1953%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2008.14257.x}, -volume = {393}, -year = {2009} -} -@article{Fea, -author = {By, Llustrated}, -keywords = {pee r}, -number = {1987}, -pages = {3--6}, -title = {{P 2 P 2 P 2}}, -volume = {93}, -year = {2009} -} -@article{Keres2009, -abstract = {We study the formation of galaxies in a large volume (50 h-1 Mpc, 2 × 2883 particles) cosmological simulation, evolved using the entropy and energy-conserving smoothed particle hydrodynamics (SPH) code gadget-2. Most of the baryonic mass in galaxies of all masses is originally acquired through filamentary 'cold mode' accretion of gas that was never shock heated to its halo virial temperature, confirming the key feature of our earlier results obtained with a different SPH code. Atmospheres of hot, virialized gas develop in haloes above 2-3 × 1011 M⊙, a transition mass that is nearly constant from z = 3 to 0. Cold accretion persists in haloes above the transition mass, especially at z ≥ 2. It dominates the growth of galaxies in low-mass haloes at all times, and it is the main driver of the cosmic star formation history. Our results suggest that the cooling of shock-heated virialized gas, which has been the focus of many analytic models of galaxy growth spanning more than three decades, might be a relatively minor element of galaxy formation. At high redshifts, satellite galaxies have gas accretion rates similar to central galaxies of the same baryonic mass, but at z < 1 the accretion rates of low-mass satellites are well below those of comparable central galaxies. Relative to our earlier simulations, the gadget-2 simulations predict much lower rates of 'hot mode' accretion from the virialized gas component. Hot accretion rates compete with cold accretion rates near the transition mass, but only at z ≤ 1. Hot accretion is inefficient in haloes above ∼5 × 1012 M⊙, with typical rates lower than 1 M⊙ yr-1 at z ≤ 1, even though our simulation does not include active galactic nuclei (AGN) heating or other forms of 'preventive' feedback. Instead, the accretion rates are low because the inner density profiles of hot gas in these haloes are shallow, with long associated cooling times. The cooling recipes typically used in semi-analytic models can overestimate the accretion rates in these haloes by orders of magnitude, so these models may overemphasize the role of preventive feedback in producing observed galaxy masses and colours. A fraction of the massive haloes develop cuspy profiles and significant cooling rates between z = 1 and 0, a redshift trend similar to the observed trend in the frequency of cooling flow clusters. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0809.1430}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Fardal, Mark and Dav{\'{e}}, Romeel and Weinberg, David H.}, -doi = {10.1111/j.1365-2966.2009.14541.x}, -eprint = {0809.1430}, -isbn = {doi:10.1111/j.1365-2966.2009.14541.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Galaxies: haloes,Intergalactic medium}, -month = {may}, -number = {1}, -pages = {160--179}, -title = {{Galaxies in a simulated $\Lambda$cDM universe - I. Cold mode and hot cores}}, -volume = {395}, -year = {2009} -} -@article{Mao2000, -abstract = {Recent observations indicate that many if not all galaxies host massive central black holes. In this paper we explore the influence of black holes on the lensing properties. We model the lens as an isothermal ellipsoid with a finite core radius plus a central black hole. We show that the presence of the black hole substantially changes the critical curves and caustics. If the black hole mass is above a critical value, then it will completely suppress the central images for all source positions. Realistic central black holes are likely to have masses below this critical value. Even in such subcritical cases, the black hole can suppress the central image when the source is inside a zone of influence, which depends on the core radius and black hole mass. In the subcritical cases, an additional image may be created by the black hole in some regions, which for some radio lenses may be detectable with high-resolution and large dynamic range VLBI maps. The presence of central black holes should also be taken into account when one constrains the core radius from the lack of central images in gravitational lenses.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0007011}, -author = {Mao, Shude and Witt, Hans J. and Koopmans, Leon V.E.}, -doi = {10.1046/j.1365-8711.2001.04143.x}, -eprint = {0007011}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Cosmology: theory,Dark matter,Galaxies: nuclei,Galaxies: structure,Gravitational lensing}, -number = {2}, -pages = {301--307}, -primaryClass = {astro-ph}, -title = {{The influence of central black holes on gravitational lenses}}, -volume = {323}, -year = {2001} -} -@article{Bullock:2005aa, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -journal = {$\backslash$apj}, -month = {dec}, -pages = {931--949}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos I: Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR $\eta$(z) using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of 102 SGL with the measurement of corresponding velocity dispersion $\sigma$0 and Einstein radius $\theta$E. In addition, we also use a dataset of 12 two image lensing systems containing the measure of time delay $\Delta$ t between source images. Jointly these two datasets give us the angular diameter distance DAol of the lens. Further, for luminosity distance, we use the 740 observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ($\eta$=1) within 2$\sigma$ confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R F L}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Li2018a, -abstract = {We investigate the discrepancy between the two-dimensional projected lensing mass and the dynam- ical mass for an ensemble of 97 strong gravitational lensing systems discovered by the Sloan Lens ACS (SLACS) Survey, the BOSS Emission-Line Lens Survey (BELLS), and the BELLS for GALaxy-Ly{\{}$\backslash$alpha{\}} EmitteR sYs- tems (BELLS GALLERY) Survey. We fit the lensing data to obtain the Einstein mass, and use the velocity dispersion of the lensing galaxies provided by the Sloan Digital Sky Survey (SDSS) to get the projected dynamical mass within the Einstein radius by assuming the power-law mass approximation. The discrepancy is found to be obvious and quantified by Bayesian analysis. For the singular isothermal sphere (SIS) mass model, we obtain that the Einstein mass is 20.7{\%} more than the dynamical mass, and the discrepancy increases with the redshift of the lensing galaxies. For more general power-law mass model, the discrepancy still exists within 1{\{}$\backslash$sigma{\}} credible region. The main reason of the the discrepancy could be mass contamination, including all invisible masses along the line of sight. In addition, the measurement errors and the approximation of the mass models could lead to part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1803.00819}, -author = {Li, Rui and Wang, Jiancheng and Shu, Yiping and Xu, Zhaoyi}, -doi = {10.3847/1538-4357/aaab50}, -eprint = {1803.00819}, -issn = {15384357}, -number = {2010}, -title = {{The discrepancy between Einstein mass and dynamical mass for SIS and power-law mass models}}, -url = {http://arxiv.org/abs/1803.00819%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaab50}, -year = {2018} -} -@article{Fassnacht1999, -abstract = {We have discovered a new gravitational lens in the Cosmic Lens All-Sky Survey (CLASS). B2045+265 is a four-image system with a maximum separation of 1.9 arcsec. A fifth radio component is detected, but its radio spectrum and its positional coincidence with infrared emission from the lensing galaxy strongly suggests that it is the radio core of the lensing galaxy. This implies that the B2045+265 system consists of a flat-spectrum radio source being lensed by another flat-spectrum radio source. Infrared images detect the lensed images of the background source and the lensing galaxy. The lensed images have relative positions and flux densities that are consistent with those seen at radio wavelengths. Spectra of the system reveal a lens redshift of z_l=0.8673 and a source redshift of z_s=1.28. The image splitting and system redshifts imply that the projected mass inside the Einstein radius of the lensing galaxy is M_E=4.7x10^{11} h^{-1} M_sun. An estimate of the light emitted inside the Einstein radius gives a mass-to-light ratio in the rest frame B band of (M/L_B)_E = 20 h (M/L_B)_sun. Both the mass and mass-to-light ratio are higher than what is seen in nearby Sa galaxies. In fact, the implied rotation velocity for the lensing galaxy is two to three times higher than what is seen in nearby spirals. The large projected mass inside the Einstein ring radius may be the result of a significant amount of dark matter in the system, perhaps from a compact group of galaxies; however, it may also arise from a misidentification of the source redshift. A simple model of the gravitational potential of the lens reproduces the image positions well, but further modeling is required to satisfy the constraints from the image flux density ratios. With further observations and modeling, this lens may yield an estimate of H_0.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9811167}, -author = {Fassnacht, C. D. and Blandford, R. D. and Cohen, J. G. and Matthews, K. and Pearson, T. J. and Readhead, A. C. S. and Womble, D. S. and Myers, S. T. and Browne, I. W. A. and Jackson, N. J. and Marlow, D. R. and Wilkinson, P. N. and Koopmans, L. V. E. and de Bruyn, A. G. and Schilizzi, R. T. and Bremer, M. and Miley, G.}, -doi = {10.1086/300724}, -eprint = {9811167}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {COSMOLOGY: DISTANCE SCALE,COSMOLOGY: GRAVITATIONAL LENSING,GALAXIES: DISTANCES AND REDSHIFTS,GALAXIES: QUASARS: INDIVIDUAL: ALPHANUMERIC: B204}, -month = {feb}, -number = {2}, -pages = {658--670}, -pmid = {740917}, -primaryClass = {astro-ph}, -title = {{B2045+265: A New Four-Image Gravitational Lens from CLASS}}, -url = {http://arxiv.org/abs/astro-ph/9811167%0Ahttp://dx.doi.org/10.1086/300724}, -volume = {117}, -year = {1999} -} -@article{Hsu2018, -abstract = {We present a new framework to characterize the occurrence rates of planet candidates identified by Kepler based on hierarchical Bayesian modeling, Approximate Bayesian Computing (ABC), and sequential importance sampling. For this study we adopt a simple 2-D grid in planet radius and orbital period as our model and apply our algorithm to estimate occurrence rates for Q1-Q16 planet candidates orbiting around solar-type stars. We arrive at significantly increased planet occurrence rates for small planet candidates ({\$}R{\_}p{\textless}1.25 R{\_}{\{}\backslashoplus{\}}{\$}) at larger orbital periods ({\$}P{\textgreater}80{\$}d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is {\$}1.6{\^{}}{\{}+1.2{\}}{\_}{\{}-0.5{\}}{\$} per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2{\$}R{\_}{\{}\backslashoplus{\}}{\$} that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C and Ford, Eric B and Ragozzine, Darin and Morehead, Robert C}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -number = {5}, -pages = {205}, -title = {{ Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation }}, -url = {http://arxiv.org/abs/1803.10787%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -volume = {155}, -year = {2018} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S{\`{e}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as Mh(M*) ∝ reff$\eta$ (M*). We find that, on average, our lens galaxies have an $\eta$ = 0.42 ± 0.12, i.e. larger galaxies live in more massive dark matter haloes. The $\eta$ is strongest for high-mass luminous red galaxies. Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed M*, satellite galaxies have a larger $\eta$ and greater scatter in the Mh and reff relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J.L. and Hudson, Michael J. and Balogh, Michael L. and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Charlton et al. - 2017 - The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Gow2016, -abstract = {{\textcopyright}2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P D and Murray, Neil J}, -doi = {10.1117/12.2232706}, -isbn = {9781510602090}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{VandeSande2016, -abstract = {Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h3 ({\$\sim${}}skewness) and h4 ({\$\sim${}}kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using 2D integral field data from the SAMI Galaxy Survey. A proxy for the spin parameter ({\$}\backslashlambda{\_}{\{}R{\_}e{\}}{\$}) and ellipticity ({\$}\backslashepsilon{\_}e{\$}) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h3 versus {\$}V/\backslashsigma{\$} anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h3 and {\$}V/\backslashsigma{\$}. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h3 versus {\$}V/\backslashsigma{\$} signatures. We identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar {\$}\backslashlambda{\_}{\{}R{\_}e{\}}-\backslashepsilon{\_}e{\$} values can show distinctly different h3-{\$}V/\backslashsigma{\$} signatures. Class 5 objects are previously unidentified fast rotators that show a weak h3 versus {\$}V/\backslashsigma{\$} anti-correlation. These objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h3 versus {\$}V/\backslashsigma{\$} as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.}, -archivePrefix = {arXiv}, -arxivId = {1611.07039}, -author = {van de Sande, Jesse and Bland-Hawthorn, Joss and Fogarty, Lisa M R and Cortese, Luca and D'Eugenio, Francesco and Croom, Scott M and Scott, Nicholas and Allen, James T and Brough, Sarah and Bryant, Julia J and Cecil, Gerald and Colless, Matthew and Couch, Warrick J and Davies, Roger and Elahi, Pascal J and Foster, Caroline and Goldstein, Gregory and Goodwin, Michael and Groves, Brent and Ho, I-Ting and Jeong, Hyunjin and Jones, D Heath and Konstantopoulos, Iraklis S and Lawrence, Jon S and Leslie, Sarah K and L{\'{o}}pez-S{\'{a}}nchez, {\'{A}}ngel R and McDermid, Richard M and McElroy, Rebecca and Medling, Anne M and Oh, Sree and Owers, Matt S and Richards, Samuel N and Schaefer, Adam L and Sharp, Rob and Sweet, Sarah M and Taranu, Dan and Tonini, Chiara and Walcher, C Jakob and Yi, Sukyoung K}, -doi = {10.3847/1538-4357/835/1/104}, -eprint = {1611.07039}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cosmology,dynamics,evolution,formation,galaxies,kinematics and,observations,stellar content,structure}, -number = {1}, -pages = {104}, -title = {{the Sami Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics}}, -url = {http://arxiv.org/abs/1611.07039%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/835/1/104}, -volume = {835}, -year = {2017} -} -@article{Erwin2015, -abstract = {I describe a new, open-source astronomical image-fitting program called imfit, specialized for galaxies but potentially useful for other sources, which is fast, flexible, and highly extensible. A key characteristic of the program is an object-oriented design that allows new types of image components (two-dimensional surfacebrightness functions) to be easily written and added to the program. Image functions provided with imfit include the usual suspects for galaxy decompositions (S{\'{e}}rsic, exponential, Gaussian), along with Core-S{\'{e}}rsic and brokenexponential profiles, elliptical rings, and three components that perform line-of-sight integration through threedimensional luminosity-density models of disks and rings seen at arbitrary inclinations. Available minimization algorithms include Levenberg-Marquardt, Nelder-Mead simplex, and Differential Evolution, allowing trade-offs between speed and decreased sensitivity to local minima in the fit landscape. Minimization can be done using the standard $\chi$2 statistic (using either data or model values to estimate per-pixel Gaussian errors, or else user-supplied error images) or Poisson-based maximum-likelihood statistics; the latter approach is particularly appropriate for cases of Poisson data in the low-count regime. I show that fitting low-signal-to-noise ratio galaxy images using $\chi$2 minimization and individual-pixel Gaussian uncertainties can lead to significant biases in fitted parameter values, which are avoided if a Poisson-based statistic is used; this is true even when Gaussian read noise is present.}, -archivePrefix = {arXiv}, -arxivId = {1408.1097}, -author = {Erwin, Peter}, -doi = {10.1088/0004-637X/799/2/226}, -eprint = {1408.1097}, -file = {:C\:/Users/Jammy/Documents/Papers/imfit.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: bulges,Galaxies: photometry,Galaxies: structure,Methods: data analysis,Techniques: image processing,Techniques: photometric}, -number = {2}, -title = {{Imfit: A fast, flexible new program for astronomical image fitting}}, -volume = {799}, -year = {2015} -} -@article{Hermans2019, -abstract = {Posterior inference with an intractable likelihood is becoming an increasingly common task in scientific domains which rely on sophisticated computer simulations. Typically, these forward models do not admit tractable densities forcing practitioners to make use of approximations. This work introduces a novel approach to address the intractability of the likelihood and the marginal model. We achieve this by learning a flexible amortized estimator which approximates the likelihood-to-evidence ratio. We demonstrate that the learned ratio estimator can be embedded in MCMC samplers to approximate likelihood-ratios between consecutive states in the Markov chain, allowing us to draw samples from the intractable posterior. Techniques are presented to improve the numerical stability and to measure the quality of an approximation. The accuracy of our approach is demonstrated on a variety of benchmarks against well-established techniques. Scientific applications in physics show its applicability.}, -archivePrefix = {arXiv}, -arxivId = {1903.04057}, -author = {Hermans, Joeri and Begy, Volodimir and Louppe, Gilles}, -eprint = {1903.04057}, -number = {i}, -title = {{Likelihood-free MCMC with Amortized Approximate Ratio Estimators}}, -url = {http://arxiv.org/abs/1903.04057}, -year = {2019} -} -@article{Li2017, -abstract = {We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier {\$}\backslashrm ATLAS{\^{}}{\{}3D{\}}{\$} results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients.}, -archivePrefix = {arXiv}, -arxivId = {1703.04894}, -author = {Li, Hongyu and Ge, Junqiang and Mao, Shude and Cappellari, Michele and Long, R J and Li, Ran and Emsellem, Eric and Dutton, Aaron A and Li, Cheng and Bundy, Kevin and Thomas, Daniel and Drory, Niv and Lopes, Alexandre Roman}, -doi = {10.3847/1538-4357/aa662a}, -eprint = {1703.04894}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {77}, -title = {{SDSS-IV MaNGA: Variation of the Stellar Initial Mass Function in Spiral and Early-type Galaxies}}, -url = {http://arxiv.org/abs/1703.04894%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa662a}, -volume = {838}, -year = {2017} -} -@article{Amorisco2022, -abstract = {A defining prediction of the cold dark matter cosmological model is the existence of a very large population of low-mass haloes. This population is absent in models in which the dark matter particle is warm (WDM). These alternatives can, in principle, be distinguished observationally because haloes along the line of sight can perturb galaxy–galaxy strong gravitational lenses. Furthermore, the WDM particle mass could be deduced because the cut-off in their halo mass function depends on the mass of the particle. We systematically explore the detectability of low-mass haloes in WDM models by simulating and fitting mock lensed images. Contrary to previous studies, we find that haloes are harder to detect when they are either behind or in front of the lens. Furthermore, we find that the perturbing effect of haloes increases with their concentration: Detectable haloes are systematically high-concentration haloes, and accounting for the scatter in the mass–concentration relation boosts the expected number of detections by as much as an order of magnitude. Haloes have lower concentration for lower particle masses and this further suppresses the number of detectable haloes beyond the reduction arising from the lower halo abundances alone. Taking these effects into account can make lensing constraints on the value of the mass function cut-off at least an order of magnitude more stringent than previously appreciated.}, -archivePrefix = {arXiv}, -arxivId = {2109.00018}, -author = {Amorisco, Nicola C and Nightingale, James and He, Qiuhan and Amvrosiadis, Aristeidis and Cao, Xiaoyue and Cole, Shaun and Etherington, Amy and Frenk, Carlos S and Li, Ran and Massey, Richard and Robertson, Andrew}, -doi = {10.1093/mnras/stab3527}, -eprint = {2109.00018}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Amorscio2022Sensiti.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {dark matter,gravitational lensing,strong}, -number = {2}, -pages = {2464--2479}, -title = {{Halo concentration strengthens dark matter constraints in galaxy–galaxy strong lensing analyses}}, -volume = {510}, -year = {2022} -} -@article{Li2024, -abstract = {We present a forecast analysis on the feasibility of measuring the cosmological parameters with a large number of galaxy-galaxy scale strong gravitational lensing systems. Future wide-area surveys like Euclid and 4MOST are expected to discover and measure the properties of more than 10 000 strong lensing systems. We develop a hierarchical model that can simultaneously constrain the lens population and cosmological parameters by combining Einstein radius measurements with stellar dynamical mass estimates for every lens. Marginalizing over the lens density profiles and stellar orbital anisotropies, we find that w can be constrained, at 68 per cent confidence, to a precision of 0.11 with 10 000 galaxy-galaxy lens systems, which would be better than any existing single-probe constraint. We test our method on 161 existing lenses from various surveys (LSD, SL2S, SLACS, and S4TM), finding w = -0.96 ± 0.46. We also show how to mitigate against the potential systematic of redshift evolution in the mean lens density profile of the population.}, -archivePrefix = {arXiv}, -arxivId = {2307.09271}, -author = {Li, Tian and Collett, Thomas E. and Krawczyk, Coleman M. and Enzi, Wolfgang}, -doi = {10.1093/mnras/stad3514}, -eprint = {2307.09271}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Li2023StrongLensPopulations.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cosmological parameters,cosmology: observations,dark energy,galaxies: structure,gravitational lensing: strong}, -number = {3}, -pages = {5311--5323}, -title = {{Cosmology from large populations of galaxy-galaxy strong gravitational lenses}}, -volume = {527}, -year = {2024} -} -@article{Swinbank2015, -abstract = {We exploit long baseline ALMA submillimeter observations of the lensed star-forming galaxy SDP 81 at z = 3.042 to investigate the properties of the interstellar medium (ISM) on scales of 50-100 pc. The kinematics of the 12CO gas within this system are well described by a rotationally supported disk with an inclination-corrected rotation speed, vrot = 320 ± 20 km s-1, and a dynamical mass of Mdyn= (3.5 ± 1.0)× 1010 within a radius of 1.5 kpc. The disk is gas-rich and unstable, with a Toomre parameter, Q = 0.30 ± 0.10, and so into star-forming regions with Jeans length LJ∼130 pc. We identify five star-forming regions within the ISM on these scales and show that their scaling relations between luminosity, line widths, and sizes are significantly offset from those typical of molecular clouds in local galaxies (Larson's relations). These offsets are likely to be caused by the high external hydrostatic pressure for the ISM, Ptot/KB∼ 40-20+30 × 107 K cm-3, which is ∼104× higher than the typical ISM pressure in the Milky Way. The physical conditions of the star-forming ISM and giant molecular clouds appear to be similar to those found in the densest environments in the local universe, such as those in the Galactic center.}, -archivePrefix = {arXiv}, -arxivId = {1505.05148}, -author = {Swinbank, A. M. and Dye, S. and Nightingale, J. W. and Furlanetto, C. and Smail, Ian and Cooray, A. and Dannerbauer, H. and Dunne, L. and Eales, S. and Gavazzi, R. and Hunter, T. and Ivison, R. J. and Negrello, M. and Oteo-Gomez, I. and Smit, R. and Werf, P. Van Der and Vlahakis, C.}, -doi = {10.1088/2041-8205/806/1/L17}, -eprint = {1505.05148}, -issn = {20418213}, -journal = {Astrophysical Journal Letters}, -keywords = {evolution,galaxies: high-redshift,galaxies: starburst}, -number = {1}, -pages = {L17}, -title = {{ALMA resolves the properties of star-forming regions in a dense gas disk at z ∼ 3}}, -url = {http://stacks.iop.org/2041-8205/806/i=1/a=L17?key=crossref.1b0d809c74a12e05028991e4a510e0b6%5Cnhttp://adsabs.harvard.edu/abs/2015ApJ...806L..17S}, -volume = {806}, -year = {2015} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work conducted to interpret this phenomenon has found that it is due to the non-spherical nature of dark matter halos. However, most studies overpredict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shapes of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations where satellite galaxies without associated subhalos ("orphan galaxies") are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region. {\textcopyright}2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W P and Kang, X and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%7B%5C%25%7D5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem%7B%5C&%7Dsid=IOPP%7B%5C%25%7D3Ajnl%7B%5C_%7Dref%7B%5C&%7Dspage=305%7B%5C&%7Dtitle=ArA%7B%5C&%7Dvolume=5%7B%5C&%7Ddate=1969%7B%5C&%7Dv%7B%5C}, -volume = {786}, -year = {2014} -} -@article{Yang2019b, -abstract = {Using the Atacama Large Millimeter/submillimeter Array (ALMA), we report high angular-resolution observations of the redshift z = 3.63 galaxy H-ATLAS J083051.0+013224 (G09v1.97), one of the most luminous strongly lensed galaxies discovered by the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). We present 0.″2-0.″4 resolution images of the rest-frame 188 and 419 $\mu$m dust continuum and the CO(6-5), H2O(211-202), and Jup = 2 H2O+ line emission. We also report the detection of H2O(211-202) in this source. The dust continuum and molecular gas emission are resolved into a nearly complete ∼1.″5 diameter Einstein ring plus a weaker image in the center, which is caused by a special dual deflector lensing configuration. The observed line profiles of the CO(6-5), H2O(211-202), and Jup = 2 H2O+ lines are strikingly similar. In the source plane, we reconstruct the dust continuum images and the spectral cubes of the CO, H2O, and H2O+ line emission at sub-kiloparsec scales. The reconstructed dust emission in the source plane is dominated by a compact disk with an effective radius of 0.7 ± 0.1 kpc plus an overlapping extended disk with a radius twice as large. While the average magnification for the dust continuum is $\mu$ ∼ 10-11, the magnification of the line emission varies from 5 to 22 across different velocity components. The line emission of CO(6-5), H2O(211-202), and H2O+ have similar spatial and kinematic distributions. The molecular gas and dust content reveal that G09v1.97 is a gas-rich major merger in its pre-coalescence phase, with a total molecular gas mass of ∼1011 M. Both of the merging companions are intrinsically ultra-luminous infrared galaxies (ULIRGs) with infrared luminosities LIR reaching 4 × 1012 L, and the total LIR of G09v1.97 is (1.4 ± 0.7)×1013 L. The approaching southern galaxy (dominating from V = -400 to -150 km s-1 relative to the systemic velocity) shows no obvious kinematic structure with a semi-major half-light radius of as = 0.4 kpc, while the receding galaxy (0 to 350 km s-1) resembles an as = 1.2 kpc rotating disk. The two galaxies are separated by a projected distance of 1.3 kpc, bridged by weak line emission (-150 to 0 km s-1) that is co-spatially located with the cold dust emission peak, suggesting a large amount of cold interstellar medium (ISM) in the interacting region. As one of the most luminous star-forming dusty high-redshift galaxies, G09v1.97 is an exceptional source for understanding the ISM in gas-rich starbursting major merging systems at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {1903.00273}, -author = {Yang, C and Gavazzi, R and Beelen, A and Cox, P and Omont, A and Lehnert, M D and Gao, Y and Ivison, R J and Swinbank, A M and Barcos-Mu{\~{n}}oz, L and Neri, R and Cooray, A and Dye, S and Eales, S and Fu, H and Gonz{\'{a}}lez-Alfonso, E and Ibar, E and Micha{\l}owski, M J and Nayyeri, H and Negrello, M and Nightingale, J and P{\'{e}}rez-Fournon, I and Riechers, D A and Smail, I and {Van Der Werf}, P}, -doi = {10.1051/0004-6361/201833876}, -eprint = {1903.00273}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: ISM,Galaxies: high-redshift,Gravitational lensing: strong,ISM: molecules,Radio lines: ISM,Submillimeter: galaxies}, -title = {{CO, H2O, H2O+ line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales}}, -volume = {624}, -year = {2019} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely, the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since {\$}z=1.0{\$}. We find that lower-mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher-mass or lower-redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys, we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology,gravitational lensing,haloes - galaxies,strong - galaxies,structure -,theory - dark matter}, -number = {2}, -pages = {1824--1848}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {469}, -year = {2017} -} -@article{Brainerd2005, -abstract = {The distribution of satellite galaxies relative to isolated host galaxies in the Sloan Digital Sky Survey (SDSS) is investigated. Host-satellite systems are selected using three different methods, yielding samples of $\sim$3300, $\sim$1600, and $\sim$950 satellites. In the plane of the sky, the distributions of all three samples show highly significant deviations from circular symmetry (>99.99%, >99.99%, and 99.79% confidence levels, respectively), and the degree of anisotropy is a strong function of the projected radius, r p , at which the satellites are found. For r p ##IMG## [http://ej.iop.org/icons/Entities/lesssim.gif] {lesssim} 100 kpc, the SDSS satellites are aligned preferentially with the major axes of the hosts. This is in stark contrast to the Holmberg effect, in which satellites are aligned with the minor axes of host galaxies. The degree of anisotropy in the distribution of the SDSS satellites decreases with r p and is consistent with an isotropic distribution at of order the 1 $\sigma$ level for 250 kpc ##IMG## [http://ej.iop.org/icons/Entities/lesssim.gif] {lesssim} r p ##IMG## [http://ej.iop.org/icons/Entities/lesssim.gif] {lesssim} 500 kpc.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408559}, -author = {Brainerd, Tereasa G.}, -doi = {10.1086/432713}, -eprint = {0408559}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brainerd - 2005 - Anisotropic Distribution of SDSS Satellite Galaxies Planar (Not Polar) Alignment(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L101--L104}, -primaryClass = {astro-ph}, -title = {{Anisotropic Distribution of SDSS Satellite Galaxies: Planar (Not Polar) Alignment}}, -url = {http://stacks.iop.org/1538-4357/628/i=2/a=L101}, -volume = {628}, -year = {2005} -} -@article{Springel2006a, -abstract = {Galaxies are not uniformly distributed in space. On large scales, the Universe displays coherent structure, with galaxies residing in groups and clusters on scales of ∼ 1–3 h− 1 Mpc, which lie at the intersections of long filaments of galaxies that are < 10 h− 1 Mpc�in length. Vast regions of relatively empty space, known as voids, contain very few galaxies and span the volume in between these structures. This observed large-scale structure depends both on cosmological parameters and on the formation and evolution of galaxies. Using the two-point correlation function, one can trace the dependence of large-scale structure on galaxy properties, such as luminosity, color, stellar mass, and track its evolution with redshift. Comparison of the observed galaxy clustering signatures with dark matter simulations allows one to model and understand the clustering of galaxies and their formation and evolution within their parent dark matter halos. Clustering measurements can determine the parent dark matter halo mass of a given galaxy population, connect observed galaxy populations at different epochs, and constrain cosmological parameters and galaxy evolution models. This chapter describes the methods used to measure the two-point correlation function in both redshift and real space, presents the current results of how the clustering amplitude depends on various galaxy properties, and discusses quantitative measurements of the structures of voids and filaments. The interpretation of these results with current theoretical models is also presented.}, -archivePrefix = {arXiv}, -arxivId = {1202.6633}, -author = {Coil, Alison L.}, -doi = {10.1007/978-94-007-5609-0_8}, -eprint = {1202.6633}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Coil - 2013 - The large-scale structure of the universe(2).pdf:pdf}, -isbn = {9789400756090}, -issn = {0038-6308}, -journal = {Planets, Stars and Stellar Systems: Volume 6: Extragalactic Astronomy and Cosmology}, -number = {7088}, -pages = {387--421}, -pmid = {16641985}, -title = {{The large-scale structure of the universe}}, -url = {http://arxiv.org/abs/astro-ph/0604561%0Ahttp://dx.doi.org/10.1038/nature04805}, -volume = {440}, -year = {2013} -} -@article{Dye2015a, -abstract = {We have modelled Atacama Large Millimetre/sub-millimetre Array (ALMA) long baseline imaging of the strong gravitational lens system H-ATLAS J090311.6+003906 (SDP.81). We have reconstructed the distribution of band 6 and 7 continuum emission in the z = 3.042 source and determined its kinematic properties by reconstructing CO(5-4) and CO(8-7) line emission in bands 4 and 6. The continuum imaging reveals a highly non-uniform distribution of dust with clumps on scales of $\sim$200 pc. In contrast, the CO line emission shows a relatively smooth, disc-like velocity field which is well fitted by a rotating disc model with an inclination angle of (40 ± 5)° and an asymptotic rotation velocity of 320 km s-1. The inferred dynamical mass within 1.5 kpc is (3.5±0.5)×1010 M⊙ which is comparable to the total molecular gas masses of (2.7 ± 0.5) × 1010 M⊙ and (3.5 ± 0.6) × 1010 M⊙ from the dust continuum emission and CO emission, respectively. Our new reconstruction of the lensed Hubble Space Telescope near-infrared emission shows two objects which appear to be interacting, with the rotating disc of gas and dust revealed by ALMA distinctly offset from the near-infrared emission. The clumpy nature of the dust and a low value of the Toomre parameter of Q $\sim$ 0.3 suggest that the disc is in a state of collapse.We estimate a star formation rate in the disc of 470 ± 80M⊙ yr-1 with an efficiency $\sim$65 times greater than typical low-redshift galaxies. Our findings add to the growing body of evidence that the most infrared luminous, dust obscured galaxies in the high-redshift Universe represent a population of merger-induced starbursts.}, -archivePrefix = {arXiv}, -arxivId = {1503.08720}, -author = {Dye, S. and Furlanetto, C. and Swinbank, A. M. and Vlahakis, C. and Nightingale, J. W. and Dunne, L. and Eales, S. A. and Smail, Ian and Oteo, I. and Hunter, T. and Negrello, M. and Dannerbauer, H. and Ivison, R. J. and Gavazzi, R. and Cooray, A. and van der Werf, P.}, -doi = {10.1093/mnras/stv1442}, -eprint = {1503.08720}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: str,Gravitational lensing: strong}, -number = {3}, -pages = {2258--2268}, -title = {{Revealing the complex nature of the strong gravitationally lensed system H-ATLAS J090311.6+003906 using ALMA}}, -volume = {452}, -year = {2015} -} -@article{Lange2024, -abstract = {We analyze two galaxy-scale strong gravitational lenses, SPT0418-47 and SPT2147-50, using JWST NIRCam imaging across multiple filters. To account for angular complexity in the lens mass distribution, we introduce multipole perturbations with orders $m=1, 3, 4$. Our results show strong evidence for angular mass complexity in SPT2147, with multipole strengths of 0.3-1.7 $\%$ for $m=3, 4$ and 2.4-9.5 $\%$ for $m=1$, while SPT0418 shows no such preference. We also test lens models that include a dark matter substructure, finding a strong preference for a substructure in SPT2147-50 with a Bayes factor (log-evidence change) of $\sim 60$ when multipoles are not included. Including multipoles reduces the Bayes factor to $\sim 11$, still corresponding to a $5\sigma$ detection of a subhalo with an NFW mass of $\log_{10}(M_{200}/M_{\odot}) = 10.87\substack{+0.53\\ -0.71}$. While SPT2147-50 may represent the fourth detection of a dark matter substructure in a strong lens, further analysis is needed to confirm that the signal is not due to systematics associated with the lens mass model.}, -archivePrefix = {arXiv}, -arxivId = {2410.12987}, -author = {Lange, Samuel C. and Amvrosiadis, Aristeidis and Nightingale, James W. and He, Qiuhan and Frenk, Carlos S. and Robertson, Andrew and Cole, Shaun and Massey, Richard and Cao, Xiaoyue and Li, Ran and Wang, Kaihao}, -eprint = {2410.12987}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Lange2024DMAngulr.pdf:pdf}, -journal = {MNRAS, submitted}, -keywords = {cosmology,dark matter,galaxies,gravitational lensing,observations,strong,structure}, -number = {October}, -pages = {1--18}, -title = {{Galaxy Mass Modelling from Multi-Wavelength JWST Strong Lens Analysis: Dark Matter Substructure, Angular Mass Complexity, or Both?}}, -url = {http://arxiv.org/abs/2410.12987}, -volume = {18}, -year = {2024} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in SPH simulations. About half the gas shock heats to roughly the virial temperature of the galaxy potential well before cooling, condensing, and forming stars, but the other half radiates its acquired gravitational energy at much lower temperatures, typically T{\textless}10{\^{}}5 K, and the histogram of maximum gas temperatures is clearly bimodal. The "cold mode" of gas accretion dominates for low mass galaxies (M{\_}baryon {\textless} 10{\^{}}{\{}10.3{\}}Msun or M{\_}halo {\textless} 10{\^{}}{\{}11.4{\}}Msun), while the conventional "hot mode" dominates the growth of high mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasi-spherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with cold mode dominating at high redshift and in low density regions today, and hot mode dominating in group and cluster environments at low redshift. Star formation rates closely track accretion rates, and we discuss the physics behind the observed environment and redshift dependence of galactic scale star formation. If we allowed hot accretion to be suppressed by conduction or AGN feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colors of ellipticals and the cutoff of the galaxy luminosity function. The transition between cold and hot accretion at M{\_}h {\$\sim${}} 10{\^{}}{\{}11.4{\}}Msun is similar to that found by Birnboim {\&} Dekel (2003) using 1-d simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. (2003) find a marked shift in galaxy properties. We speculate on connections between these theoretical and observational transitions.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ({\$}\backslashbackslashrho\backslashbackslashsim r{\^{}}{\{}-\backslashbackslashgamma{\{}\backslash{\}}{\}}{\$}), we find that, although the zero cosmic curvature is still included within {\$}2 \backslashbackslashsigma{\{}\backslash{\$}{\}} confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile {\$}\backslashbackslashrho\backslashbackslashsim r{\^{}}{\{}-\backslashbackslashalpha{\{}\backslash{\}}{\}}{\$} to be different from that of the total-mass density profile {\$}\backslashbackslashnu\backslashbackslashsim r{\^{}}{\{}-\backslashbackslashdelta{\{}\backslash{\}}{\}}{\$}, a weaker constraint on the curvature ({\$}\backslashbackslashOmega{\{}\backslash{\_}{\}}k{\textless}0.197{\$} at 68{\$}\backslash{\$}{\%} confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of {\$}\backslashbackslashDelta \backslashbackslashOmega{\{}\backslash{\_}{\}}k\backslashbackslashsimeq 10{\^{}}{\{}-3{\}}{\$}, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{Weinberg2002, -abstract = {Simulations predict that the dark matter halos of galaxies should have central cusps, while those inferred from observed galaxies do not have cusps. We demonstrate, using both linear perturbation theory and n-body simulations, that a disk bar, which should be ubiquitous in forming galaxies, can produce cores in cuspy CDM dark matter profiles within five bar orbital times. Simulations of forming galaxies suggest that one of Milky Way size could have a 10 kpc primordial bar; this bar will remove the cusp out to approximately 5 kpc in approximately 1.5 gigayears, while the disk only loses approximately 8% of its original angular momentum. An inner Lindblad-like resonance couples the rotating bar to orbits at all radii through the cusp, transferring the bar pattern angular momentum to the dark matter cusp, rapidly flattening it. This resonance disappears for profiles with cores and is responsible for a qualitative difference in bar driven halo evolution with and without a cusp. This bar induced evolution will have a profound effect on the structure and evolution of almost all galaxies. Hence, both to understand galaxy formation and evolution and to make predictions from theory it is necessary to resolve these dynamical processes. Unfortunately, correctly resolving these important dynamical processes in ab initio calculations of galaxy formation is a daunting task, requiring at least 4,000,000 halo particles using our SCF code, and probably requiring many times more particles when using noisier tree, direct summation, or grid based techniques, the usual methods employed in such calculations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0110632}, -author = {Weinberg, Martin D. and Katz, Neal}, -doi = {10.1086/343847}, -eprint = {0110632}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Theory,Galaxies: Evolution,Galaxies: Halos,Galaxies: Kinematics and Dynamics}, -month = {dec}, -number = {2}, -pages = {627--633}, -primaryClass = {astro-ph}, -title = {{Bar‐driven Dark Halo Evolution: A Resolution of the Cusp‐Core Controversy}}, -url = {http://stacks.iop.org/0004-637X/580/i=2/a=627}, -volume = {580}, -year = {2002} -} -@article{Libeskind2014, -abstract = {We examine the angular infall pattern of subhaloes onto host haloes in the context of the large-scale structure. We find that this infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are found to be preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that its always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range ({\$\sim${}}10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group}, -archivePrefix = {arXiv}, -arxivId = {1407.0394}, -author = {Libeskind, Noam I and Knebe, Alexander and Hoffman, Yehuda and Gottl{\"{o}}ber, Stefan}, -doi = {10.1093/mnras/stu1216}, -eprint = {1407.0394}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Large-scale structure of universe}, -number = {2}, -pages = {1274--1280}, -title = {{The universal nature of subhalo accretion}}, -volume = {443}, -year = {2014} -} -@article{Diemand2008, -abstract = {In cold dark matter cosmological models, structures form and grow through the merging of smaller units. Numerical simulations have shown that such merging is incomplete; the inner cores of haloes survive and orbit as 'subhaloes' within their hosts. Here we report a simulation that resolves such substructure even in the very inner regions of the Galactic halo. We find hundreds of very concentrated dark matter clumps surviving near the solar circle, as well as numerous cold streams. The simulation also reveals the fractal nature of dark matter clustering: isolated haloes and subhaloes contain the same relative amount of substructure and both have cusped inner density profiles. The inner mass and phase-space densities of subhaloes match those of recently discovered faint, dark-matter-dominated dwarf satellite galaxies, and the overall amount of substructure can explain the anomalous flux ratios seen in strong gravitational lenses. Subhaloes boost $\gamma$-ray production from dark matter annihilation by factors of 4 to 15 relative to smooth galactic models. Local cosmic ray production is also enhanced, typically by a factor of 1.4 but by a factor of more than 10 in one per cent of locations lying sufficiently close to a large subhalo. (These estimates assume that the gravitational effects of baryons on dark matter substructure are small.) {\textcopyright}2008 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0805.1244}, -author = {Diemand, J. and Kuhlen, M. and Madau, P. and Zemp, M. and Moore, B. and Potter, D. and Stadel, J.}, -doi = {10.1038/nature07153}, -eprint = {0805.1244}, -isbn = {0008-5472 (Print)\r0008-5472 (Linking)}, -issn = {14764687}, -journal = {Nature}, -month = {aug}, -number = {7205}, -pages = {735--738}, -pmid = {18685701}, -title = {{Clumps and streams in the local dark matter distribution}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/18685701}, -volume = {454}, -year = {2008} -} -@article{Griffiths2019, -abstract = {We report an embarrassingly parallel method for the evaluation of thermodynamic properties over an energy landscape exhibiting broken ergodicity, nested is the likelihood of the observed data D givenbasin-sampling (NBS). We also introduce the No Galilean U-Turn Sampler (NoGUTS), a new sampling scheme based on the No U-Turn Sampler (NUTS) introduced by Hoffman and Gelman (2014) that works with the Galilean Monte Carlo scheme introduced by Betancourt (2012) to aid the efficient generation of new live points. NoGUTS can be thought of as a form of reflective slice sampling with an automatic stopping criterion. We apply this approach to a benchmark atomic cluster of 31 Lennard-Jones atoms, which exhibits a low temperature solid-solid heat capacity peak. The calculated heat capacity is compared with results generated by parallel tempering (PT), basin-sampling parallel tempering (BSPT), and standard nested sampling (NS) simulations. NBS reproduces the full heat capacity curve predicted by PT and BSPT, while the NS calculation with similar computational cost fails to resolve the low-temperature solid-solid phase transition.}, -author = {Griffiths, Matthew and Wales, David J}, -doi = {10.1021/acs.jctc.9b00567}, -issn = {15499626}, -journal = {Journal of Chemical Theory and Computation}, -number = {12}, -pages = {6865--6881}, -pmid = {31557432}, -title = {{Nested Basin-Sampling}}, -volume = {15}, -year = {2019} -} -@article{Zibetti2020, -abstract = {We perform spatially resolved stellar population analysis for a sample of 69 early-type galaxies (ETGs) from the CALIFA integral field spectroscopic survey, including 48 ellipticals and 21 S0's. We generate and quantitatively characterize profiles of light-weighted mean stellar age and metallicity within ≲2Re, as a function of radius and stellar-mass surface density $\mu$*. We study in detail the dependence of profiles on galaxies' global properties, including velocity dispersion $\sigma$e, stellar mass, morphology. ETGs are universally characterized by strong, negative metallicity gradients ({\$}\backslashsim \backslash!-0.3\backslash, \backslashtext{\{}dex{\}}{\$} per Re) within 1Re, which flatten out moving towards larger radii. A quasi-universal local $\mu$*–metallicity relation emerges, which displays a residual systematic dependence on $\sigma$e, whereby higher $\sigma$e implies higher metallicity at fixed $\mu$*. Age profiles are typically U-shaped, with minimum around 0.4 Re, asymptotic increase to maximum ages beyond {\$}\backslashsim 1.5\backslash, {\$}Re, and an increase towards the centre. The depth of the minimum and the central increase anticorrelate with $\sigma$e. A possible qualitative interpretation of these observations is a two-phase scenario. In the first phase, dissipative collapse occurs in the inner 1Re, establishing a negative metallicity gradient. The competition between the outside-in quenching due to feedback-driven winds and some form of inside-out quenching, possibly caused by central AGN feedback or dynamical heating, determines the U-shaped age profiles. In the second phase, the accretion of ex-situ stars from quenched and low-metallicity satellites shapes the flatter stellar population profiles in the outer regions.}, -archivePrefix = {arXiv}, -arxivId = {1906.02209}, -author = {Zibetti, Stefano and Gallazzi, Anna R and Hirschmann, Michaela and Consolandi, Guido and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and van de Ven, Glenn and Lyubenova, Mariya}, -doi = {10.1093/mnras/stz3205}, -eprint = {1906.02209}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {abundances,cd,elliptical and lenticular,evolution,formation,galax-,galaxies,ies,imaging,stellar content,techniques}, -number = {3}, -pages = {3562--3585}, -title = {{Insights into formation scenarios of massive early-type galaxies from spatially resolved stellar population analysis in CALIFA}}, -volume = {491}, -year = {2020} -} -@article{Gomer2018, -abstract = {The positions of multiple images in galaxy lenses are related to the galaxy mass distribution. Smooth elliptical mass profiles were previously shown to be inadequate in reproducing the quad population. In this paper, we explore the deviations from such smooth elliptical mass distributions. Unlike most other work, we use a model-free approach based on the relative polar image angles of quads, and their position in 3D space with respect to the fundamental surface of quads (FSQ). The FSQ is defined by quads produced by elliptical lenses. We have generated thousands of quads from synthetic populations of lenses with substructure consistent with Lambda cold dark matter ($\Lambda$CDM) simulations, and found that such perturbations are not sufficient to match the observed distribution of quads relative to the FSQ. The result is unchanged even when subhalo masses are increased by a factor of 10, and the most optimistic lensing selection bias is applied. We then produce quads from galaxies created using two components, representing baryons and dark matter. The transition from the mass being dominated by baryons in inner radii to being dominated by dark matter in outer radii can carry with it asymmetries, which would affect relative image angles. We run preliminary experiments using lenses with two elliptical mass components with non-identical axial ratios and position angles, perturbations from ellipticity in the form of non-zero Fourier coefficients a4 and a6, and artificially offset ellipse centres as a proxy for asymmetry at image radii. We show that combination of these effects is a promising way of accounting for quad population properties. We conclude that the quad population provides a unique and sensitive tool for constraining detailed mass distribution in the centres of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1712.07665}, -author = {Gomer, Matthew R and Williams, Liliya L R}, -doi = {10.1093/mnras/stx3294}, -eprint = {1712.07665}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1987--2002}, -title = {{The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses}}, -volume = {475}, -year = {2018} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and S{\'{e}}rsic index distributions obtained from two-dimensional structural fits to 40, 000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of S{\'{e}}rsic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. {\textcopyright}2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Casey2014, -abstract = {Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 1013L⊙ with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both space-based and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the best-understood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al., 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies. {\textcopyright} 2014 Elsevier B.V.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9806317}, -author = {Casey, Caitlin M. and Narayanan, Desika and Cooray, Asantha}, -doi = {10.1016/j.physrep.2014.02.009}, -eprint = {9806317}, -file = {:C\:/Users/Jammy/Documents/Papers/High_Redshift_galaxies/Casey2014DustyHighRedshiftSummary.pdf:pdf}, -issn = {03701573}, -journal = {Physics Reports}, -keywords = {Cosmology,Galaxies,Galaxy evolution,Galaxy formation,Infrared galaxies}, -number = {2}, -pages = {45--161}, -primaryClass = {astro-ph}, -title = {{Dusty star-forming galaxies at high redshift}}, -volume = {541}, -year = {2014} -} -@article{Lacerna2020, -abstract = {We study the spatially resolved properties of 333 elliptical galaxies with the MaNGA/SDSS-IV survey. The aim is to understand the fundamental processes of formation and quenching of elliptical galaxies. We used the DESI Legacy Imaging Surveys for accurate morphological classification. Based on integrated spectroscopic properties and colors, we classified galaxies into classical "red and dead", recently quenched, and blue star-forming ellipticals (CLEs, RQEs, and BSFs corresponding to 75%, 10%, and 4% of the sample, respectively). We inferred their stellar age and stellar metallicity gradients out to 1.5 effective radius, and reconstructed their global and radial histories of mass growth and star formation. We find the mass- and light-weighted age gradients of CLEs are nearly flat or mildly negative, with small differences between both ages. The respective metallicity gradients are negative, being flatter as less massive are the CLEs. The more massive CLEs assembled earlier and quenched faster than the less massive ones. The CLEs show a weak inside-out growth and a clear inside-out quenching. At masses < $10^{11}$ $M_{\bigodot}$, the age and $Z$ gradients of the RQEs and BSFs are flatter than those of the CLEs but with larger scatters. They show very weak inside-out growth and quenching, being the quenching slow and even not completed at $z\sim$ 0 for the BSFs. Instead, the massive RQEs show an outside-in quenching, and positive gradients in the light-weighted age and stellar metallicities. Our results are consistent with a scenario where the inner parts of CLEs formed by an early and coeval dissipative collapse with a consequent burst of star formation and further quenching, whereas the outer parts continued their assembly likely by dry mergers. We also discuss some evolutionary scenarios for the RQE and BSF galaxies that would agree with their generic results presented here.}, -archivePrefix = {arXiv}, -arxivId = {2001.05506}, -author = {Lacerna, I. and Ibarra-Medel, H. and Avila-Reese, V. and Hern{\'{a}}ndez-Toledo, H. M. and V{\'{a}}zquez-Mata, J. A. and S{\'{a}}nchez, S. F.}, -eprint = {2001.05506}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lacerna et al. - 2020 - SDSS-IV MaNGA global and local stellar population properties of elliptical galaxies and their assembly histories.pdf:pdf}, -keywords = {cd - galaxies,elliptical and lenticular,evolution - galaxies,formation - galaxies,galaxies,star formation,stellar content - galaxies,structure - galaxies}, -title = {{SDSS-IV MaNGA: global and local stellar population properties of elliptical galaxies and their assembly histories}}, -url = {http://arxiv.org/abs/2001.05506}, -year = {2020} -} -@article{Gilman2017, -abstract = {The free streaming length of dark matter particles determines the abundance of structure on sub-galactic scales. We present a statistical technique, amendable to any parametrization of subhalo density profile and mass function, to probe darkmatter on these scales with quadrupole image lenses. We consider a warm dark matter particle with a mass function characterized by a normalization and free streaming scale mhm. We forecast bounds on dark matter warmth for 120-180 lenses, attainable with future surveys, at typical lens (source) redshifts of 0.5 (1.5) in early-type galaxies with velocity dispersions of 220-270 km s-1.We demonstrate that limits on mhm deteriorate rapidly with increasing uncertainty in image fluxes, underscoring the importance of precise measurements and accurate lens models. For our forecasts, we assume the deflectors in the lens sample do not exhibit complex morphologies, so we neglect systematic errors in their modelling. Omitting the additional signal from line-of-sight haloes, our constraints underestimate the true power of the method. Assuming cold dark matter, for a low normalization, corresponding to the destruction of all subhaloes within the host scale radius, we forecast 2$\sigma$ bounds on mhm (thermal relic mass) of 107.5 (5.0), 108 (3.6), and 108.5 (2.7) M⊙ (keV) for flux errors of 2 per cent, 4 per cent, and 8 per cent. With a higher normalization, these constraints improve to 107.2 (6.6), 107.5 (5.3), and 107.8 (4.3) M⊙ (keV) with 120 systems. We are also able to measure the normalization of the mass function, which has implications for baryonic feedback models and tidal stripping.}, -archivePrefix = {arXiv}, -arxivId = {1712.04945}, -author = {Gilman, Daniel and Birrer, Simon and Treu, Tommaso and Keeton, Charles R. and Nierenberg, Anna}, -doi = {10.1093/mnras/sty2261}, -eprint = {1712.04945}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gilman et al. - 2018 - Probing the nature of dark matter by forward modelling flux ratios in strong gravitational lenses.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: structure,Gravitational lensing: strong,Methods: statistical}, -number = {1}, -pages = {819--834}, -title = {{Probing the nature of dark matter by forward modelling flux ratios in strong gravitational lenses}}, -url = {http://arxiv.org/abs/1712.04945}, -volume = {481}, -year = {2018} -} -@article{Xie2015, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P. and Frenk, Carlos S. and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xie et al. - 2015 - The size evolution of elliptical galaxies(3).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Lilly2016, -abstract = {There are very strong observed correlations between the specific star-formation rates (sSFR) of galaxies and their mean surface mass densities, {\{}$\backslash$Sigma{\}}, as well as other aspects of their internal structure. These strong correlations have often been taken to indicate that the internal structure of a galaxy must play a major physical role, directly or indirectly, in the control of star-formation. In this paper we show by means of a very simple toy model that these correlations can arise naturally without any such physical role once the observed evolution of the size-mass relation for star-forming galaxies is taken into account. In particular, the model reproduces the sharp threshold in {\{}$\backslash$Sigma{\}} between galaxies that are star-forming and those that are quenched, and the evolution of this threshold with redshift. Similarly, it produces iso-quenched-fraction contours in the {\$}{\{}f{\_}Q(m,R{\_}e){\}}{\$} plane that are almost exactly parallel to lines of constant {\{}$\backslash$Sigma{\}} for centrals and shallower for satellites. It does so without any dependence on quenching on size or {\{}$\backslash$Sigma{\}}, and without invoking any differences between centrals and satellites, beyond the different mass-dependences of their quenching laws. The toy-model also reproduces several other observations, including the sSFR gradients within galaxies and the appearance of inside-out build-up of passive galaxies. Finally, it is shown that curvature in the Main Sequence sSFR-mass relation can produce curvature in the apparent B/T ratios with mass. Our analysis therefore suggests that many of the strong correlations that are observed between galaxy structure and sSFR may well be a consequence of things unrelated to quenching and should not be taken as evidence of the physical processes that drive quenching.}, -archivePrefix = {arXiv}, -arxivId = {1604.06459}, -author = {Lilly, Simon J and Carollo, C Marcella}, -doi = {10.3847/0004-637x/833/1/1}, -eprint = {1604.06459}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {1}, -pmid = {15540530}, -title = {{Surface Density Effects in Quenching: Cause or Effect?}}, -url = {http://arxiv.org/abs/1604.06459%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/833/1/1}, -volume = {833}, -year = {2016} -} -@article{Hopkins2010c, -abstract = {We present a simple estimate of the mass 'deficits' in cored spheroids, as a function of galaxy mass and radius within the galaxy. Previous attempts to measure such deficits depended on fitting some functional form to the profile at large radii extrapolating inwards; this is sensitive to the assumed functional form and does not allow for variation in nuclear profile shapes. For example, we show that literally interpreting the residuals from a single/cored Sersic function fit as implied 'deficit' can be misleading. Instead, we take advantage of larger data sets to directly construct stellar mass profiles of observed systems and measure the stellar mass enclosed in a series of physical radii (M*(< R)), for samples of cusp and core spheroids at the same stellar mass. We show that there is a significant (model-independent) bimodality in this distribution of central structure for this sample at small radii. We non-parametrically measure the median offset between core and cusp populations (the 'deficit'$\Delta$M*(< R)). We can then construct the scoured mass profile as a function of radius, without reference to any assumed functional form. The mass deficit rises in power-law fashion ($\Delta$M*(< R) ∝R1.3-1.8) from a significant but small mass at R≲ 10 pc, to asymptote to a maximum ∼ 0.5-2 MBH at ∼ 100 pc, where MBH is the mass of the central, supermassive black hole (BH) hosted by the spheroid. At larger radii there is no statistically significant separation between populations; the upper limit to the cumulative scoured mass at ∼kpc is ∼ 2-4 MBH. This does not depend strongly on stellar mass. The dispersion in M*(< R) appears larger in the core population, possibly reflecting the fact that core scouring increases the scatter in central profile shapes. We measure this broadening effect as a function of radius. The relatively low mass deficits inferred, and characteristic radii, are in good agreement with models of 'scouring' from BH binary systems. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1006.0488}, -author = {Hopkins, Philip F. and Hernquist, Lars}, -doi = {10.1111/j.1365-2966.2010.16915.x}, -eprint = {1006.0488}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins, Hernquist - 2010 - A non-parametric estimate of mass 'scoured' in galaxy cores.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {447--457}, -title = {{A non-parametric estimate of mass 'scoured' in galaxy cores}}, -url = {http://arxiv.org/abs/1006.0488%0Ahttp://dx.doi.org/10.1111/j.1365-2966.2010.16915.x}, -volume = {407}, -year = {2010} -} -@article{Jaroszynski2012, -abstract = {We investigate strong lensing by non-singular finite isothermal ellipsoids taking into account the influence of the matter along the line of sight and in the close lens vicinity. We compare three descriptions of light propagation: the full approach taking into account all matter inhomogeneities along the rays; the single plane approach, where we take into account the influence of the strong lens neighbours but neglect the foreground and background objects; and the single lens approach. In each case, we simulate many strong lensing configurations placing a point source at the same redshift but in different locations inside the region surrounded by caustics. We further analyse configurations of four or five images. For every simulated strong lensing configuration, we attempt to fit a simplified lens model using a single isothermal ellipsoid or a single isothermal ellipsoid with external shear. The single lens fits to configurations obtained in the full approach are rejected in majority of cases with 95per cent significance. For configurations obtained in the single plane approach, the rejection rate is substantially lower. Also the inclusion of external shear in simplified modelling improves the chances of obtaining acceptable fits, but the problem is not solved completely. The quantitative estimates of the rates of rejection of simplified models depend on the required accuracy of the models, and we present few illustrative examples, which show that both matter close to the lens and matter along the rays do have important influence on lens modelling. We also estimate the typical value of the external shear and compare the fitted parameters of the simplified models with the parameters of the lenses used in the simulations. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1204.6223}, -author = {Jaroszynski, M. and Kostrzewa-Rutkowska, Z.}, -doi = {10.1111/j.1365-2966.2012.21197.x}, -eprint = {1204.6223}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Jaroszynski, Kostrzewa-Rutkowska - 2012 - Background, foreground and nearby matter influence on strong gravitational lenses(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: strong,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {1}, -pages = {325--332}, -title = {{Background, foreground and nearby matter influence on strong gravitational lenses}}, -volume = {424}, -year = {2012} -} -@article{Cautun2015, -abstract = {The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model ($\Lambda$ cold dark matter - $\Lambda$CDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of theMWand M31 planes in $\Lambda$CDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high-resolution cosmological simulations. We find that planar structures are very common, and that {\$\sim${}}10 per cent of $\Lambda$CDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small-scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and $\Lambda$CDM predictions. In fact, {\$\sim${}}10 per cent of $\Lambda$CDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1506.04151}, -author = {Cautun, Marius and Bose, Sownak and Frenk, Carlos S and Guo, Qi and Han, Jiaxin and Hellwing, Wojciech A and Sawala, Till and Wang, Wenting}, -doi = {10.1093/mnras/stv1557}, -eprint = {1506.04151}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {4}, -pages = {3838--3852}, -title = {{Planes of satellite galaxies: When exceptions are the rule}}, -volume = {452}, -year = {2015} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) 'CMASS' sample at z $\sim$ 0.5. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogues which include selection effects, reproduce the overall SMF, the projected two-point correlation function wp, the CMASS dn/dz, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of 'age matching' and show that these effects are markedly different compared to the ones explored by Hearin et al. at lower stellar masses. We construct two models, one in which galaxy colour is stochastic ('AbM' model) as well as a model which contains assembly bias effects ('AgM' model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colours are not a stochastic process in high-mass haloes. Our results suggest that the colours of galaxies in high-mass haloes are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P. and Bundy, Kevin and Zentner, Andrew R. and Behroozi, Peter S. and Reid, Beth A. and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L. and White, Martin and Schneider, Donald P.}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Saito et al. - 2016 - Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass.pdf:pdf}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Milosavljevic2001, -abstract = {We investigate a model in which galactic nuclei form via the coalescence of pre-existing stellar systems containing supermassive black holes. Merger simulations are carried out using N-body algorithms that can follow the formation and decay of a black-hole binary and its effect on the surrounding stars down to sub-parsec scales. Our initial stellar systems have steep central density cusps similar to those in low-luminosity elliptical galaxies. Formation of a black-hole binary transfers energy to the stars and lowers the central density; continued decay of the binary creates a {\$\sim${}}1/r density cusp similar to those observed in bright elliptical galaxies, with a break radius that extends well beyond the sphere of gravitational influence of the black holes. The decay of the black hole binary is followed over a factor of {\$\sim${}}20 in separation after formation of a hard binary, considerably farther than in previous simulations. We see almost no dependence of the binary's decay rate on number of particles in the simulation, contrary to earlier studies in which a lower initial density of stars led to a more rapid depletion of the binary's loss cone. We nevertheless argue that the decay of a black hole binary in a real galaxy would be expected to stall at separations of 0.01-1 pc unless some additional mechanism is able to extract energy from the binary. Our results support a picture in which the observed dependence of nuclear cusp slope on galaxy luminosity is a consequence of galaxy interactions. We also discuss the implications of our results for the survivability of dark-matter cusps.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103350}, -author = {Milosavljevic, Milos and Merritt, David}, -doi = {10.1086/323830}, -eprint = {0103350}, -isbn = {1476-4687 (Electronic)$\backslash$n0028-0836 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Black Hole Physics,Galaxies: Nuclei,Stellar Dynamics}, -month = {dec}, -number = {1}, -pages = {34--62}, -pmid = {20123743}, -primaryClass = {astro-ph}, -title = {{Formation of Galactic Nuclei}}, -url = {http://arxiv.org/abs/astro-ph/0103350%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/323830}, -volume = {563}, -year = {2001} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of {\$\sim${}}3692 galaxies, with -18.5 {\textless}= M{\_}g {\textless} -22.0 mag and redshift 0.01 {\textless}= z {\textless} 0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of {\$\sim${}}2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined ({\textgreater}60 degrees) systems, we find the following results. (1) The optical r-band fraction (f{\_}opt-r) of barred galaxies is {\$\sim${}}48{\%}-52{\%}. (2) When galaxies are separated according to normalized half light radius (r{\_}e/R{\_}24), a remarkable result is seen: f{\_}opt-r rises sharply, from {\$\sim${}}40{\%} in galaxies that have small r{\_}e/R{\_}24 and visually appear to host prominent bulges, to {\$\sim${}}70{\%} for galaxies that have large r{\_}e/R{\_}24 and appear disk-dominated. (3) f{\_}opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that {\$\sim${}}20{\%} of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity {\textgreater}=0.4) and large enough (semi-major axis {\textgreater}=1.5 kpc) to be reliably characterized via ellipse-fitting out to z{\$\sim${}}0.8, we get an optical r-band fraction for strong bars f{\_}opt-s of {\$\sim${}}34{\%}. This value is higher only by a modest factor of 1.4, compared to the value of {\$\sim${}}24{\%}+-4{\%} reported at z{\$\sim${}}0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z{\$\sim${}}0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Johnson, Crockett}, -doi = {10.2307/3616804}, -eprint = {0802.3961}, -issn = {00255572}, -journal = {The Mathematical Gazette}, -keywords = {Astrophysics}, -number = {407}, -pages = {17}, -title = {{A Construction for a Regular Heptagon}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {59}, -year = {1975} -} -@article{Veale2017a, -abstract = {We analyse the environmental properties of 370 local early-type galaxies (ETGs) in the MASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute {\$}K{\$}-band magnitude {\$}-21.5 {\textgreater}M{\_}K {\textgreater}-26.6{\$}, or stellar mass {\$}8 \backslashbackslashtimes 10{\^{}}{\{}9{\}} {\textless}M{\_}* {\textless}2 \backslashbackslashtimes 10{\^{}}{\{}12{\}} M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}}. We find these galaxies to reside in a diverse range of environments measured by four methods: group membership (whether a galaxy is a brightest group/cluster galaxy, satellite, or isolated), halo mass, large-scale mass density (measured over a few Mpc), and local mass density (measured within the {\$}N{\$}th neighbour). The spatially resolved IFS stellar kinematics provide robust measurements of the spin parameter {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}e{\$} and enable us to examine the relationship among {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}e{\$}, {\$}M{\_}*{\$}, and galaxy environment. We find a strong correlation between {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}e{\$} and {\$}M{\_}*{\$}, where the average {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}e{\$} decreases from {\$}\backslashbackslashsim 0.4{\$} to below 0.1 with increasing mass, and the fraction of slow rotators {\$}f{\_}{\{}\backslashbackslashrm slow{\}}{\$} increases from {\$}\backslashbackslashsim 10{\$}{\%} to 90{\%}. We show for the first time that at fixed {\$}M{\_}*{\$}, there are almost no trends between galaxy spin and environment; the apparent kinematic morphology-density relation for ETGs is therefore primarily driven by {\$}M{\_}*{\$} and is accounted for by the joint correlations between {\$}M{\_}*{\$} and spin, and between {\$}M{\_}*{\$} and environment. A possible exception is that the increased {\$}f{\_}{\{}\backslashbackslashrm slow{\}}{\$} at high local density is slightly more than expected based only on these joint correlations. Our results suggest that the physical processes responsible for building up the present-day stellar masses of massive galaxies are also very efficient at reducing their spin, in any environment.}, -archivePrefix = {arXiv}, -arxivId = {1703.08573}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and McConnell, Nicholas and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/mnras/stx1639}, -eprint = {1703.08573}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {1428--1445}, -title = {{The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxies}}, -url = {http://arxiv.org/abs/1703.08573%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1639}, -volume = {471}, -year = {2017} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {https://ui.adsabs.harvard.edu/%7B%5C#%7Dabs/2009Natur.457..451D/abstract}, -volume = {457}, -year = {2009} -} -@article{Devour2017, -abstract = {Accurate measurement of galaxy structures is a prerequisite for quantitative investigation of galaxy properties or evolution. Yet, the impact of galaxy inclination and dust on commonly used metrics of galaxy structure is poorly quantified. We use infrared data sets to select inclination-independent samples of disc and flattened elliptical galaxies. These samples show strong variation in S$\backslash$'{\{}e{\}}rsic index, concentration, and half-light radii with inclination. We develop novel inclination-independent galaxy structures by collapsing the light distribution in the near-infrared on to the major axis, yielding inclination-independent `linear' measures of size and concentration. With these new metrics we select a sample of Milky Way analogue galaxies with similar stellar masses, star formation rates, sizes and concentrations. Optical luminosities, light distributions, and spectral properties are all found to vary strongly with inclination: When inclining to edge-on, {\$}r{\$}-band luminosities dim by {\$}{\textgreater}{\$}1 magnitude, sizes decrease by a factor of 2, `dust-corrected' estimates of star formation rate drop threefold, metallicities decrease by 0.1 dex, and edge-on galaxies are half as likely to be classified as star forming. These systematic effects should be accounted for in analyses of galaxy properties.}, -archivePrefix = {arXiv}, -arxivId = {1702.06528}, -author = {Devour, Brian M and Bell, Eric F}, -doi = {10.1093/mnrasl/slx021}, -eprint = {1702.06528}, -issn = {1745-3925}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {dust,extinction,galaxies,general,photometric,techniques}, -number = {1}, -pages = {L31----L35}, -pmid = {18462818}, -title = {{Revealing strong bias in common measures of galaxy properties using new inclination-independent structures}}, -url = {http://arxiv.org/abs/1702.06528%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnrasl/slx021}, -volume = {468}, -year = {2017} -} -@article{Li2018a, -abstract = {We investigate the discrepancy between the two-dimensional projected lensing mass and the dynam- ical mass for an ensemble of 97 strong gravitational lensing systems discovered by the Sloan Lens ACS (SLACS) Survey, the BOSS Emission-Line Lens Survey (BELLS), and the BELLS for GALaxy-Ly{\{}$\backslash$alpha{\}} EmitteR sYs- tems (BELLS GALLERY) Survey. We fit the lensing data to obtain the Einstein mass, and use the velocity dispersion of the lensing galaxies provided by the Sloan Digital Sky Survey (SDSS) to get the projected dynamical mass within the Einstein radius by assuming the power-law mass approximation. The discrepancy is found to be obvious and quantified by Bayesian analysis. For the singular isothermal sphere (SIS) mass model, we obtain that the Einstein mass is 20.7{\%} more than the dynamical mass, and the discrepancy increases with the redshift of the lensing galaxies. For more general power-law mass model, the discrepancy still exists within 1{\{}$\backslash$sigma{\}} credible region. The main reason of the the discrepancy could be mass contamination, including all invisible masses along the line of sight. In addition, the measurement errors and the approximation of the mass models could lead to part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1803.00819}, -author = {Li, Rui and Wang, Jiancheng and Shu, Yiping and Xu, Zhaoyi}, -doi = {10.3847/1538-4357/aaab50}, -eprint = {1803.00819}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {64}, -title = {{The Discrepancy between Einstein Mass and Dynamical Mass for SIS and Power-law Mass Models}}, -url = {http://arxiv.org/abs/1803.00819%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaab50}, -volume = {855}, -year = {2018} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}1011 to {\textgreater} 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyze sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in {\$}255{\$} square degrees of the Kilo Degree Survey (KiDS), one of the current-generation optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii {\$}\backslashbackslashgtrsim 1.4{\$} arcsec, about twice the {\$}r{\$}-band seeing in KiDS. In a sample of {\$}21789{\$} colour-magnitude selected Luminous Red Galaxies (LRG), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find {\$}\backslashbackslashsim100{\$} massive LRG-galaxy lenses at {\$}z\backslashbackslashlsim 0.4{\$} in KiDS when completed. In the most optimistic scenario this number can grow considerably (to maximally {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C E and Tortora, C and Chatterjee, S and Vernardos, G and Koopmans, L V E and Kleijn, G Verdoes and Napolitano, N R and Covone, G and Schneider, P and Grado, A and McFarland, J}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys,cD}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright}2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{Grogin2011, -abstract = {This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at z ≈ 1.5-8, and to study Type Ia supernovae at z > 1.5. Five premier multi-wavelength sky regions are selected, each with extensive multi-wavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 infrared channel (WFC3/IR) and the WFC3 ultraviolet/optical channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers ∼ 125 arcmin 2 within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of ∼ 800 arcmin2 across GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-Deep Survey). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up-to-date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including charge transfer efficiency degradation for ACS, removal of electronic bias-striping present in ACS data after Servicing Mission 4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper. {\textcopyright} 2011. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1105.3754}, -author = {Koekemoer, Anton M. and Faber, S. M. and Ferguson, Henry C. and Grogin, Norman A. and Kocevski, Dale D. and Koo, David C. and Lai, Kamson and Lotz, Jennifer M. and Lucas, Ray A. and McGrath, Elizabeth J. and Ogaz, Sara and Rajan, Abhijith and Riess, Adam G. and Rodney, Steve A. and Strolger, Louis and Casertano, Stefano and Castellano, Marco and Dahlen, Tomas and Dickinson, Mark and Dolch, Timothy and Fontana, Adriano and Giavalisco, Mauro and Grazian, Andrea and Guo, Yicheng and Hathi, Nimish P. and Huang, Kuang Han and {Van Der Wel}, Arjen and Yan, Hao Jing and Acquaviva, Viviana and Alexander, David M. and Almaini, Omar and Ashby, Matthew L.N. and Barden, Marco and Bell, Eric F. and Bournaud, Fr{\'{e}}d{\'{e}}ric and Brown, Thomas M. and Caputi, Karina I. and Cassata, Paolo and Challis, Peter J. and Chary, Ranga Ram and Cheung, Edmond and Cirasuolo, Michele and Conselice, Christopher J. and Cooray, Asantha Roshan and Croton, Darren J. and Daddi, Emanuele and Dav{\'{e}}, Romeel and {De Mello}, Duilia F. and {De Ravel}, Loic and Dekel, Avishai and Donley, Jennifer L. and Dunlop, James S. and Dutton, Aaron A. and Elbaz, David and Fazio, Giovanni G. and Filippenko, Alexei V. and Finkelstein, Steven L. and Frazer, Chris and Gardner, Jonathan P. and Garnavich, Peter M. and Gawiser, Eric and Gruetzbauch, Ruth and Hartley, Will G. and H{\"{a}}ussler, Boris and Herrington, Jessica and Hopkins, Philip F. and Huang, Jia Sheng and Jha, Saurabh W. and Johnson, Andrew and Kartaltepe, Jeyhan S. and Khostovan, Ali A. and Kirshner, Robert P. and Lani, Caterina and Lee, Kyoung Soo and Li, Weidong and Madau, Piero and McCarthy, Patrick J. and McIntosh, Daniel H. and McLure, Ross J. and McPartland, Conor and Mobasher, Bahram and Moreira, Heidi and Mortlock, Alice and Moustakas, Leonidas A. and Mozena, Mark and Nandra, Kirpal and Newman, Jeffrey A. and Nielsen, Jennifer L. and Niemi, Sami and Noeske, Kai G. and Papovich, Casey J. and Pentericci, Laura and Pope, Alexandra and Primack, Joel R. and Ravindranath, Swara and Reddy, Naveen A. and Renzini, Alvio and Rix, Hans Walter and Robaina, Aday R. and Rosario, David J. and Rosati, Piero and Salimbeni, Sara and Scarlata, Claudia and Siana, Brian and Simard, Luc and Smidt, Joseph and Snyder, Diana and Somerville, Rachel S. and Spinrad, Hyron and Straughn, Amber N. and Telford, Olivia and Teplitz, Harry I. and Trump, Jonathan R. and Vargas, Carlos and Villforth, Carolin and Wagner, Cory R. and Wandro, Pat and Wechsler, Risa H. and Weiner, Benjamin J. and Wiklind, Tommy and Wild, Vivienne and Wilson, Grant and Wuyts, Stijn and Yun, Min S.}, -doi = {10.1088/0067-0049/197/2/36}, -eprint = {1105.3754}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Koekemoer2011CANDELs.pdf:pdf}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {ApJSS}, -keywords = {cosmology: observations,galaxies: high-redshift}, -month = {dec}, -number = {2}, -pages = {3535--39}, -title = {{Candels: The cosmic assembly near-infrared deep extragalactic legacy survey - The hubble space telescope observations, imaging data products, and mosaics}}, -volume = {197}, -year = {2011} -} -@article{Eisenstein2001, -abstract = {We describe the target selection and resulting properties of a spectroscopic sample of luminous, red galaxies (LRG) from the imaging data of the Sloan Digital Sky Survey (SDSS). These galaxies are selected on the basis of color and magnitude to yield a sample of luminous, intrinsically red galaxies that extends fainter and further than the main flux-limited portion of the SDSS galaxy spectroscopic sample. The sample is designed to impose a passively-evolving luminosity and rest-frame color cut to a redshift of 0.38. Additional, yet more luminous, red galaxies are included to a redshift of 0.5. Approximately 12 of these galaxies per square degree are targeted for spectroscopy, so the sample will number over 100,000 with the full survey. SDSS commissioning data indicate that the algorithm efficiently selects luminous (M{\_}g=-21.4), red galaxies, that the spectroscopic success rate is very high, and that the resulting set of galaxies is approximately volume-limited out to z=0.38. When the SDSS is complete, the LRG spectroscopic sample will fill over 1h{\^{}}-3 Gpc{\^{}}3 with an approximately homogeneous population of galaxies and will therefore be well suited to studies of large-scale structure and clusters out to z=0.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108153}, -author = {Eisenstein, Daniel J and Annis, James and Gunn, James E and Szalay, Alexander S and Connolly, Andrew J and Nichol, R C and Bahcall, Neta A and Bernardi, Mariangela and Burles, Scott and Castander, Francisco J and Fukugita, Masataka and Hogg, David W and Ivezi{\'{c}}, {\v{Z}}eljko and Knapp, G R and Lupton, Robert H and Narayanan, Vijay and Postman, Marc and Reichart, Daniel E and Richmond, Michael and Schneider, Donald P and Schlegel, David J and Strauss, Michael A and SubbaRao, Mark and Tucker, Douglas L and {Vanden Berk}, Daniel and Vogeley, Michael S and Weinberg, David H and Yanny, Brian}, -doi = {10.1086/323717}, -eprint = {0108153}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2267--2280}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample}}, -url = {http://arxiv.org/abs/astro-ph/0108153%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/323717}, -volume = {122}, -year = {2001} -} -@article{Gnedin2004, -abstract = {The cooling of gas in the centers of dark matter halos is expected to lead to a more concentrated dark matter distribution. The response of dark matter to the condensation of baryons is usually calculated using the model of adiabatic contraction, which assumes spherical symmetry and circular orbits. In contrast, halos in the hierarchical structure formation scenarios grow via multiple violent mergers and accretion along filaments, and particle orbits in the halos are highly eccentric. We study the effects of the cooling of gas in the inner regions of halos using high-resolution cosmological simulations which include gas dynamics, radiative cooling, and star formation. We find that the dissipation of gas indeed increases the density of dark matter and steepens its radial profile in the inner regions of halos compared to the case without cooling. For the first time, we test the adiabatic contraction model in cosmological simulations and find that the standard model systematically overpredicts the increase of dark matter density in the inner 5% of the virial radius. We show that the model can be improved by a simple modification of the assumed invariant from M(r)r to M(r_av)r, where r and r_av are the current and orbit-averaged particle positions. This modification approximately accounts for orbital eccentricities of particles and reproduces simulation profiles to within 10-20%. We present analytical fitting functions that accurately describe the transformation of the dark matter profile in the modified model and can be used for interpretation of observations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0406247}, -author = {Gnedin, Oleg Y. and Kravtsov, Andrey V. and Klypin, Anatoly A. and Nagai, Daisuke}, -doi = {10.1086/424914}, -eprint = {0406247}, -isbn = {0018-9200}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Theory,Galaxies: Formation,Galaxies: Halos,Methods: Numerical}, -month = {nov}, -number = {1}, -pages = {16--26}, -primaryClass = {astro-ph}, -title = {{Response of Dark Matter Halos to Condensation of Baryons: Cosmological Simulations and Improved Adiabatic Contraction Model}}, -url = {http://arxiv.org/abs/astro-ph/0406247%0Ahttp://dx.doi.org/10.1086/424914}, -volume = {616}, -year = {2004} -} -@article{Geng2025, -abstract = {Strong lensing systems, expected to be abundantly discovered by next-generation surveys, offer a powerful tool for studying cosmology and galaxy evolution. The connection between galaxy structure and cosmology through distance ratios highlights the need to examine the evolution of lensing galaxy mass density profiles. We propose a novel, dark energy-model-independent method to investigate the mass density slopes of lensing galaxies and their redshift evolution using an extended power-law (EPL) model. We employ a non-parametric approach based on Artificial Neural Networks (ANNs) trained on Type Ia Supernovae (SNIa) data to reconstruct distance ratios of strong lensing systems. These ratios are compared with theoretical predictions to estimate the evolution of EPL model parameters. Analyses conducted at three levels, including the combined sample, individual lenses, and binned groups, ensure robust and reliable estimates. A negative trend in the mass density slope with redshift is observed, quantified as $\partial\gamma/\partial z = -0.20 \pm 0.12$ under a triangular prior for anisotropy. This study demonstrates that the redshift evolution of density slopes in lensing galaxies can be determined independently of dark energy models. Simulations based on LSST Rubin Observatory forecasts, which anticipate 100,000 strong lenses, show that spectroscopic follow-up of just 10 percent of these systems can constrain the redshift evolution coefficient with uncertainty ($\Delta\partial\gamma/\partial z$) to 0.021. This precision distinguishes evolving and non-evolving density slopes, providing new insights into galaxy evolution and cosmology.}, -archivePrefix = {arXiv}, -arxivId = {2501.02577}, -author = {Geng, Shuaibo and Grespan, Margherita and Thuruthipilly, Hareesh and Harikumar, Sreekanth and Pollo, Agnieszka and Biesiada, Marek}, -eprint = {2501.02577}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Geng2025SLRelations.pdf:pdf}, -journal = {arXiv:2501.02577}, -keywords = {galaxy evolution,strong gravitational lensing}, -title = {{Investigating the Redshift Evolution of Lensing Galaxy Density Slopes via Model-Independent Distance Ratios}}, -url = {http://arxiv.org/abs/2501.02577}, -year = {2025} -} -@article{astropy:2013, -archivePrefix = {arXiv}, -arxivId = {astro-ph.IM/1307.6212}, -author = {{Astropy Collaboration} and Robitaille, T.$\sim$P. and Tollerud, E.$\sim$J. and Greenfield, P and Droettboom, M and Bray, E and Aldcroft, T and Davis, M and Ginsburg, A and Price-Whelan, A.$\sim$M. and Kerzendorf, W.$\sim$E. and Conley, A and Crighton, N and Barbary, K and Muna, D and Ferguson, H and Grollier, F and Parikh, M.$\sim$M. and Nair, P.$\sim$H. and Unther, H.$\sim$M. and Deil, C and Woillez, J and Conseil, S and Kramer, R and Turner, J.$\sim$E.$\sim$H. and Singer, L and Fox, R and Weaver, B.$\sim$A. and Zabalza, V and Edwards, Z.$\sim$I. and {Azalee Bostroem}, K and Burke, D.$\sim$J. and Casey, A.$\sim$R. and Crawford, S.$\sim$M. and Dencheva, N and Ely, J and Jenness, T and Labrie, K and Lim, P.$\sim$L. and Pierfederici, F and Pontzen, A and Ptak, A and Refsdal, B and Servillat, M and Streicher, O}, -doi = {10.1051/0004-6361/201322068}, -eprint = {1307.6212}, -journal = {A\&A}, -keywords = {methods: data analysis,methods: miscellaneous,virtual observatory tools}, -month = {oct}, -pages = {A33}, -primaryClass = {astro-ph.IM}, -title = {{Astropy: A community Python package for astronomy}}, -volume = {558}, -year = {2013} -} -@article{Bingham2019, -abstract = {Pyro is a probabilistic programming language built on Python as a platform for developing advanced probabilistic models in AI research. To scale to large data sets and high-dimensional models, Pyro uses stochastic variational inference algorithms and probability distributions built on top of PyTorch, a modern GPU-accelerated deep learning framework. To accommodate complex or model-specific algorithmic behavior, Pyro leverages Poutine, a library of composable building blocks for modifying the behavior of probabilistic programs.}, -archivePrefix = {arXiv}, -arxivId = {1810.09538}, -author = {Bingham, Eli and Chen, Jonathan P and Jankowiak, Martin and Obermeyer, F and Pradhan, Neeraj and Karaletsos, Theofanis and Singh, Rohit and Szerlip, Paul and Horsfall, Paul and Goodman, Noah D}, -eprint = {1810.09538}, -issn = {15337928}, -journal = {Journal of Machine Learning Research}, -keywords = {Approximate Bayesian inference,Deep learning,Generative models,Graphical models,Probabilistic programming}, -number = {Xxxx}, -pages = {0--5}, -title = {{Pyro: Deep universal probabilistic programming}}, -volume = {20}, -year = {2019} -} -@article{Kormendy2004, -abstract = {The robustness of stellar-dynamical black hole (BH) mass measurements is illustrated using 7 galaxies that have results from independent groups. Derived masses have remained constant to a factor of about 2 as spatial resolution has improved by factors of 2 - 330 and as the analysis has improved from spherical, isotropic models to axisymmetric, three-integral models. This gives us confidence that the masses are reliable and that the galaxies do not indulge in a wide variety of perverse orbital structures. Constraints on BH alternatives are also improving. In M31, Hubble Space Telescope (HST) spectroscopy shows that the central massive dark object (MDO) is in a tiny cluster of blue stars embedded in the P2 nucleus of the galaxy. The MDO must be less than about 0.06 arcsec in radius. M31 becomes the third galaxy in which dark clusters of brown dwarf stars or stellar remnants can be excluded. In our Galaxy, observations of almost-complete stellar orbits show that the MDO radius is less than about 0.0006 pc. Among BH alternatives, this excludes even neutrino balls. Therefore, measurements of central dark masses and the conclusion that these are BHs have both stood the test of time. Confidence in the BH paradigm for active galactic nuclei is correspondingly high. Compared to the radius of the BH sphere of influence, BHs are discovered at similar spatial resolution with HST as in ground-based work. The reason is that HST is used to observe more distant galaxies. Large, unbiased samples are accessible. As a result, HST has revolutionized the study of BH demographics.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306353}, -author = {Kormendy, John}, -doi = {10.1146/annurev.astro.33.1.581}, -eprint = {0306353}, -isbn = {0521824494}, -issn = {00664146}, -journal = {Coevolution of Black Holes and Galaxies}, -pages = {1}, -primaryClass = {astro-ph}, -title = {{The Stellar-Dynamical Search for Supermassive Black Holes in Galactic Nuclei}}, -url = {http://arxiv.org/abs/astro-ph/0306353}, -volume = {1}, -year = {2003} -} -@article{Dullo2013, -abstract = {We have used the full radial extent of images from the Hubble Space Telescope's Advanced Camera for Surveys and Wide Field Planetary Camera 2 to extract surface brightness profiles from a sample of six, local lenticular galaxy candidates. We have modeled these profiles using a core-S{\'{e}}rsic bulge plus an exponential disk model. Our fast rotating lenticular disk galaxies with bulge magnitudes MV ≲ -21.30 mag have central stellar deficits, suggesting that these bulges may have formed from "dry" merger events involving supermassive black holes (BHs) while their surrounding disk was subsequently built up, perhaps via cold gas accretion scenarios. The central stellar mass deficits M def are roughly 0.5-2 M BH (BH mass), rather than ∼10-20 M BH as claimed from some past studies, which is in accord with core-S{\'{e}}rsic model mass deficit measurements in elliptical galaxies. Furthermore, these bulges have S{\'{e}}rsic indices n ∼3, half-light radii Re < 2 kpc and masses >1011 M⊙, and therefore appear to be descendants of the compact galaxies reported at z ∼ 1.5-2. Past studies which have searched for these local counterparts by using single-component galaxy models to provide the z ∼ 0 size comparisons have overlooked these dense, compact, and massive bulges in today's early-type disk galaxies. This evolutionary scenario not only accounts for what are today generally old bulges - which must be present in z ∼ 1.5 images - residing in what are generally young disks, but it eliminates the uncomfortable suggestion of a factor of three to five growth in size for the compact, z ∼ 1.5 galaxies that are known to possess infant disks. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1303.1273}, -author = {Dullo, Bililign T. and Graham, Alister W.}, -doi = {10.1088/0004-637X/768/1/36}, -eprint = {1303.1273}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: fundamental parameter,galaxies: nuclei,galaxies: photometry,galaxies: structure}, -month = {may}, -number = {1}, -pages = {36}, -title = {{Central stellar mass deficits in the bulges of local lenticular galaxies, and the connection with compact z ∼ 1.5 galaxies}}, -url = {http://stacks.iop.org/0004-637X/768/i=1/a=36?key=crossref.f039d46909aa5a098182bec8768b821d}, -volume = {768}, -year = {2013} -} -@article{Golse2002, -abstract = {We introduce analytical expressions for a pseudo fully analytical elliptical projected Navarro, Frenk & White (NFW) mass profile to be used in lensing equations. We propose a formalism that incorporates the ellipticity into the expression for the lens potential, producing a pseudo-elliptical mass distribution. This approach can be implemented to any circular mass profile for which the projected mass profile $\Sigma$(r) and the deflection angle profile $\alpha$(r) both have analytical expressions; however the potential does not necessarily need to take an analytical form. We apply this new formalism to the NFW mass distribution and study how well this pseudo-elliptical NFW model describes an elliptical mass distribution. We conclude that the pseudo-elliptical NFW model is a good description of elliptical mass distributions provided that the ellipticity of the projected mass distribution is ≲0.4, although with a slightly boxy distribution.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0112138}, -author = {Golse, G. and Kneib, J. P.}, -doi = {10.1051/0004-6361:20020639}, -eprint = {0112138}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {Cosmology: miscellaneous,Dark matter,Galaxies: clusters: general,Galaxies: halos,Gravitational lensing}, -month = {aug}, -number = {3}, -pages = {821--827}, -primaryClass = {astro-ph}, -title = {{Pseudo elliptical lensing mass model: Application to the NFW mass distribution}}, -url = {http://www.aanda.org/10.1051/0004-6361:20020639}, -volume = {390}, -year = {2002} -} -@article{Gavazzi2008, -abstract = {We report the discovery of two concentric Einstein rings around the gravitational lens SDSS J0946+1006. The main lens is at redshift zl = 0.222, while the inner ring (1) is at redshift zs1 = 0.609 (E Ein1 = 1.43″ ± 0.01″). The wider image separation (REin2 = 2.07″ ± 0.02″) of the outer ring (2) implies a higher redshift than that of ring 1; the detection of ring 2 in the F814W ACS filter implies an upper limit of zs2 ≲ 6.9. The main lens can be described by a power-law total mass density profile $\rho$tot ∏ r-$\gamma$′ with $\gamma$′ = 2.00 ±0.03 and velocity dispersion $\sigma$SIE = 287 ± 5 km s-1 (the stellar velocity dispersion is $\sigma$v, * = 284 ± 24 km s_1). The strong lensing configuration is inconsistent with light traces mass. Adopting a prior on the stellar mass-to-light ratio from previous SLACS work, we infer a 73% ±9% dark matter fraction within the cylinder of radius equal to the effective radius of the lens. We find that, for the case of SDSS J0946+1006, the geometry of the two rings does not place interesting constraints on cosmography because of the suboptimal redshifts of lens and sources. We then consider the perturbing effect of the mass associated with ring 1 building a compound lens model. This introduces minor changes to the mass of the main lens and provides an estimate of zs2 = 3.1-1.0+2.0 and of the mass of the source responsible for ring 1 ($\sigma$SIE, sl = 94-47-27 km s-1). We conclude by examining the prospects of doing cosmography with a sample of 50 double rings, expected from future space-based surveys. Accounting for uncertainties in the mass profile of the lens and the effects of the perturber, we find that such a sample would constrain $\Omega$m and w within 10%, assuming flatness. {\textcopyright} 2008. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0801.1555}, -author = {Gavazzi, Rapha{\"{e}}l and Treu, Tommaso and Koopmans, L{\'{e}}on V. E. and Bolton, Adam S. and Moustakas, Leonidas A. and Burles, Scott and Marshall, Philip J.}, -doi = {10.1086/529541}, -eprint = {0801.1555}, -isbn = {0004-637x}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {1046--1059}, -title = {{The Sloan Lens ACS Survey. VI. Discovery and Analysis of a Double Einstein Ring1}}, -url = {http://stacks.iop.org/0004-637X/677/i=2/a=1046}, -volume = {677}, -year = {2008} -} -@article{Foreman-Mackey2016, -abstract = {This Python module uses matplotlib (Hunter 2007) to visualize multidimensional samples using a scatterplot matrix. In these visualizations, each one-and two-dimensional pro-jection of the sample is plotted to reveal covariances. corner was originally conceived to display the results of Markov Chain Monte Carlo simulations and the defaults are chosen with this application in mind but it can be used for displaying many qualitatively different samples.}, -author = {Foreman-Mackey, Daniel}, -doi = {10.21105/joss.00024}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Foreman-Mackey - 2016 - corner.py Scatterplot matrices in Python(2).pdf:pdf}, -issn = {2475-9066}, -journal = {J. Open Source Softw.}, -number = {2}, -pages = {24}, -title = {{corner.py: Scatterplot matrices in Python}}, -volume = {1}, -year = {2016} -} -@article{Abadi2010, -abstract = {We use N-body/gasdynamical cosmological simulations to examine the effect of the assembly of a central galaxy on the shape and mass profile of its surrounding dark matter halo. Two series of simulations are compared; one that follows only the evolution of the dark matter component of individual haloes in the proper $\Lambda$cold dark matter ($\Lambda$CDM) cosmological context, and a second series where a baryonic component is added and followed hydrodynamically. The simulations with baryons include radiative cooling but neglect the formation of stars and their feedback. The efficient, unimpeded cooling that results leads most baryons to collect at the halo centre in a centrifugally supported disc which, due to angular momentum losses, is too small and too massive when compared with typical spiral galaxies. This admittedly unrealistic model allows us, nevertheless, to gauge the maximum effect that galaxies may have in transforming their surrounding dark haloes. We find, in agreement with earlier work, that the shape of the halo becomes more axisymmetric: post galaxy assembly, haloes are transformed from triaxial into essentially oblate systems, with well-aligned isopotential contours of roughly constant flattening (〈/a〉∼ 0.85). Haloes always contract as a result of galaxy assembly, but the effect is substantially less pronounced than predicted by the traditional 'adiabatic-contraction' hypothesis. The reduced contraction helps to reconcile $\Lambda$CDM haloes with constraints on the dark matter content inside the solar circle and should alleviate the longstanding difficulty of matching simultaneously the scaling properties of galaxy discs and the galaxy luminosity function. The halo contraction we report is also less pronounced than found in earlier simulations, a disagreement which suggests that halo contraction is not solely a function of the initial and final distribution of baryons. Not only how much baryonic mass has been deposited at the centre of a halo matters, but also the mode of its deposition. Although simple formulae might work in particular cases where galaxies form nearly adiabatically, in general it might prove impossible to predict the halo response to galaxy formation without a detailed understanding of a galaxy's detailed assembly history. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0902.2477}, -author = {Abadi, Mario G. and Navarro, Julio F. and Fardal, Mark and Babul, Arif and Steinmetz, Matthias}, -doi = {10.1111/j.1365-2966.2010.16912.x}, -eprint = {0902.2477}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: disc,Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {sep}, -number = {1}, -pages = {435--446}, -title = {{Galaxy-induced transformation of dark matter haloes}}, -volume = {407}, -year = {2010} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales (∼500 kpc) in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the virial radius of the haloes while describing the infalling matter via fluxes through a spherical shell; and we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP described for the first time in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one- and two-point statistics. The peripheral and advected momenta are correlated with the spin of the embedded halo at levels of 30 and 50 per cent. The infall takes place preferentially in the plane perpendicular to the direction defined by the spin of the halo. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be ∼15 per cent. The substructures have their spin orthogonal to their velocity vector in the rest frame of the halo at a level of about 5 per cent, suggestive of an image of a flow along filamentary structures, which provides an explanation for the measured anisotropy. Using a 'synthetic' stacked halo, it is shown that the positions and orientations of satellites relative to the direction of spin of the halo are not random even in projection. The average ellipticity of stacked haloes is 10 per cent, while the alignment excess in projection reaches 2 per cent. All measured correlations are fitted by a simple three-parameter model. We conclude that a halo does not see its environment as an Isotropic perturbation, we investigate how the anisotropy is propagated inwards using perturbation theory, and we discuss briefly the implications for weak lensing, warps and the thickness of galactic discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D and Pichon, C and Colombi, S}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Bellstedt2018, -abstract = {We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 1010 {\textless} M*/M⊙ {\textless} 1011.6 that cover a large radial range of 0.1-4.0 effective radii.We combine SLUGGS and ATLAS3D data sets to model the total-mass profiles of a sample of 21 fast-rotator galaxies, utilizing a hyperparameter method to combine the two independent data sets. The total-mass density profile slope values derived for these galaxies are consistent with those measured in the inner regions of galaxies by other studies. Furthermore, the total-mass density slopes ($\gamma$tot) appear to be universal over this broad stellar mass range, with an average value of $\gamma$tot= -2.24± 0.05, i.e. slightly steeper than isothermal. We compare our results to model galaxies from the Magneticum and EAGLE cosmological hydrodynamic simulations, in order to probe the mechanisms that are responsible for varying total-mass density profile slopes. The simulated-galaxy slopes are shallower than the observed values by {\$\sim${}}0.3-0.5, indicating that the physical processes shaping the mass distributions of galaxies in cosmological simulations are still incomplete. For galaxies with M* {\textgreater} 1010.7M⊙ in the Magneticum simulations, we identify a significant anticorrelation between total-mass density profile slopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas this anticorrelation is weaker for lower stellar masses, implying that the measured total-mass density slopes for low-mass galaxies are less likely to be determined by merger activity.}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A and Romanowsky, Aaron J and Remus, Rhea Silvia and Stevens, Adam R H and Brodie, Jean P and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to {\$\sim${}}4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Wang2011, -abstract = {The hierarchical Dirichlet process (HDP) is a Bayesian nonparametric model that can be used to model mixed-membership data with a poten- tially infinite number of components. It has been applied widely in probabilistic topic modeling, where the data are documents and the compo- nents are distributions of terms that reflect recur- ring patterns (or “topics”) in the collection. Given a document collection, posterior inference is used to determine the number of topics needed and to characterize their distributions. One limitation of HDP analysis is that existing posterior infer- ence algorithms require multiple passes through all the data—these algorithms are intractable for very large scale applications. We propose an on- line variational inference algorithm for the HDP, an algorithm that is easily applicable to massive and streaming data. Our algorithm is significantly faster than traditional inference algorithms for the HDP, and lets us analyze much larger data sets. We illustrate the approach on two large collections of text, showing improved performance over on- line LDA, the finite counterpart to the HDP topic model.}, -author = {Wang, Chong and Paisley, John and Blei, David M}, -doi = {10.2196/medinform.3783}, -isbn = {1609258177}, -issn = {2291-9694}, -journal = {Icais}, -pages = {752--760}, -pmid = {25947632}, -title = {{Online Variational Inference for the Hierarchical Dirichlet Process}}, -url = {http://jmlr.org/proceedings/papers/v15/wang11a.html}, -volume = {15}, -year = {2011} -} -@article{Newman2015, -abstract = {We report the discovery of RG1M0150, a massive, recently quenched galaxy at z = 2.636 that is multiply imaged by the cluster MACSJ0150.3-1005. We derive a stellar mass of log M∗ = 11.49-0.16+0.10 and a half-light radius of Ee,maj = 1.8 ± 0.4 kpc. Taking advantage of the lensing magnification, we are able to spatially resolve a remarkably massive yet compact quiescent galaxy at z>2 in ground-based near-infrared spectroscopic observations using Magellan/FIRE and Keck/MOSFIRE. We find no gradient in the strength of the Balmer absorption lines over 0.6Re-1.6Re which are consistent with an age of 760 Myr. Gas emission in [N ii] broadly traces the spatial distribution of the stars and is coupled with weak H$\alpha$ emission (log [N ii]/H$\alpha$ = 0.6±0.2), indicating that OB stars are not the primary ionizing source. The velocity dispersion within the effective radius is $\sigma$e,stars = 271 ± 41 km s-1 We detect rotation in the stellar absorption lines for the first time beyond z∼1. Using a two-integral Jeans model that accounts for observational effects, we measure a dynamical mass of log Mdyn = 11.24 0.14 and V/$\sigma$ = 0.70 ± 0.21. This is a high degree of rotation considering the modest observed ellipticity of 0.12 ± 0.08, but it is consistent with predictions from dissipational merger simulations that produce compact remnants. The mass of RG1M0150 implies that it is likely to become a slowly rotating elliptical. If it is typical, this suggests that the progenitors of massive ellipticals retain significant net angular momentum after quenching which later declines, perhaps through accretion of satellites.}, -archivePrefix = {arXiv}, -arxivId = {1509.04345}, -author = {Newman, Andrew B. and Belli, Sirio and Ellis, Richard S.}, -doi = {10.1088/2041-8205/813/1/L7}, -eprint = {1509.04345}, -isbn = {0004000900}, -issn = {20418213}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: kinematics and dynamics,gravitational lensing: strong}, -month = {nov}, -number = {1}, -pages = {L7}, -title = {{Discovery of a strongly lensed massive quiescent galaxy at z = 2.636: Spatially resolved spectroscopy and indications of rotation}}, -url = {http://arxiv.org/abs/1509.04345}, -volume = {813}, -year = {2015} -} -@article{Brooks2015a, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brooks, Christensen - 2015 - Bulge formation via mergers in cosmological simulations.pdf:pdf}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Brainerd2005, -abstract = {The distribution of satellite galaxies relative to isolated host galaxies in the Sloan Digital Sky Survey (SDSS) is investigated. Host-satellite systems are selected using three different methods, yielding samples of $\sim$3300, $\sim$1600, and $\sim$950 satellites. In the plane of the sky, the distributions of all three samples show highly significant deviations from circular symmetry (>99.99%, >99.99%, and 99.79% confidence levels, respectively), and the degree of anisotropy is a strong function of the projected radius, r p , at which the satellites are found. For r p ##IMG## [http://ej.iop.org/icons/Entities/lesssim.gif] {lesssim} 100 kpc, the SDSS satellites are aligned preferentially with the major axes of the hosts. This is in stark contrast to the Holmberg effect, in which satellites are aligned with the minor axes of host galaxies. The degree of anisotropy in the distribution of the SDSS satellites decreases with r p and is consistent with an isotropic distribution at of order the 1 $\sigma$ level for 250 kpc ##IMG## [http://ej.iop.org/icons/Entities/lesssim.gif] {lesssim} r p ##IMG## [http://ej.iop.org/icons/Entities/lesssim.gif] {lesssim} 500 kpc.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408559}, -author = {Brainerd, Tereasa G.}, -doi = {10.1086/432713}, -eprint = {0408559}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brainerd - 2005 - Anisotropic Distribution of SDSS Satellite Galaxies Planar (Not Polar) Alignment(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L101--L104}, -primaryClass = {astro-ph}, -title = {{Anisotropic Distribution of SDSS Satellite Galaxies: Planar (Not Polar) Alignment}}, -url = {http://stacks.iop.org/1538-4357/628/i=2/a=L101}, -volume = {628}, -year = {2005} -} -@article{Guzzo2007, -abstract = {We have identified a large-scale structure at z$\sim$0.73 in the COSMOS field, coherently described by the distribution of galaxy photometric redshifts, an ACS weak-lensing convergence map and the distribution of extended X-ray sources in a mosaic of XMM observations. The main peak seen in these maps corresponds to a rich cluster with Tx= 3.51+0.60/-0.46 keV and Lx=(1.56+/-0.04) x 10^{44} erg/s ([0.1-2.4] keV band). We estimate an X-ray mass within $r500$ corresponding to M500$\sim$1.6 x 10^{14} Msun and a total lensing mass (extrapolated by fitting a NFW profile) M(NFW)=(6+/-3) x 10^15 Msun. We use an automated morphological classification of all galaxies brighter than I_AB=24 over the structure area to measure the fraction of early-type objects as a function of local projected density Sigma_10, based on photometric redshifts derived from ground-based deep multi-band photometry. We recover a robust morphology-density relation at this redshift, indicating, for comparable local densities, a smaller fraction of early-type galaxies than today. Interestingly, this difference is less strong at the highest densities and becomes more severe in intermediate environments. We also find, however, local "inversions'' of the observed global relation, possibly driven by the large-scale environment. In particular, we find direct correspondence of a large concentration of disk galaxies to (the colder side of) a possible shock region detected in the X-ray temperature map and surface brightness distribution of the dominant cluster. We interpret this as potential evidence of shock-induced star formation in existing galaxy disks, during the ongoing merger between two sub-clusters.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701482}, -author = {Guzzo, L. and Cassata, P. and Finoguenov, A. and Massey, R. and Scoville, N. Z. and Capak, P. and Ellis, R. S. and Mobasher, B. and Taniguchi, Y. and Thompson, D. and Ajiki, M. and Aussel, H. and Bohringer, H. and Brusa, M. and Calzetti, D. and Comastri, A. and Franceschini, A. and Hasinger, G. and Kasliwal, M. M. and Kitzbichler, M. G. and Kneib, J.‐P. and Koekemoer, A. and Leauthaud, A. and McCracken, H. J. and Murayama, T. and Nagao, T. and Rhodes, J. and Sanders, D. B. and Sasaki, S. and Shioya, Y. and Tasca, L. and Taylor, J. E.}, -doi = {10.1086/516588}, -eprint = {0701482}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Guzzo2007WeirdWLLens.pdf:pdf}, -issn = {0067-0049}, -journal = {ApJSS}, -number = {1}, -pages = {254--269}, -primaryClass = {astro-ph}, -title = {{The Cosmic Evolution Survey (COSMOS): A Large‐Scale Structure at z = 0.73 and the Relation of Galaxy Morphologies to Local Environment}}, -volume = {172}, -year = {2007} -} -@article{Gadotti2011, -abstract = {I present results from the modeling of stellar bars in nearly 300 barred galaxies in the local universe through parametric multi-component multi-band image fitting. The surface brightness radial profile of bars is described using a Sersic function, and parameters such as bar effective radius, ellipticity, boxiness, length and mass, and bar-to-total luminosity and mass ratios, are determined, which is unprecedented for a sample of this size. The properties of bars in galaxies with classical bulges and pseudo-bulges are compared. For a fixed bar-to-total mass ratio, pseudo-bulges are on average significantly less massive than classical bulges, indicating that, if pseudo-bulges are formed through bars, further processes are necessary to build a classical bulge. I find a correlation between bar ellipticity and boxiness, and define a new parameter as the product of these two quantities. I also find correlations between this product and normalised bar size, between the sizes of bars and bulges, and between normalised bar size and bulge-to-total ratio. Bars with different ellipticities follow parallel lines in the latter two correlations. These correlations can arise if, starting off with different normalised sizes and ellipticities, bars grow longer and stronger with dynamical age, as a result of angular momentum exchange from the inner to the outer parts of galaxies, consistent with previous theoretical predictions. A plausible consequence is that bar pattern speeds should become lower with bar dynamical age, and towards galaxies with more prominent bulges.}, -archivePrefix = {arXiv}, -arxivId = {1003.1719}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2011.18945.x}, -eprint = {1003.1719}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {3308--3318}, -title = {{Secular evolution and structural properties of stellar bars in galaxies}}, -volume = {415}, -year = {2011} -} -@article{Bentabol2016, -abstract = {We examine a sample of 1495 galaxies in the CANDELS fields to determine the evolution of two-component galaxies, including bulges and discs, within massive galaxies at the epoch 1 {\textless} z {\textless}3 when the Hubble sequence forms. We fit all of our galaxies' light profiles with a single S{\'{e}}rsic fit, as well as with a combination of exponential and S{\'{e}}rsic profiles. The latter is done in order to describe a galaxy with an inner and an outer component, or bulge and disc component. We develop and use three classification methods (visual, F-test and the residual flux fraction) to separate our sample into one-component galaxies (disc/spheroidslike galaxies) and two-component galaxies (galaxies formed by an 'inner part' or bulge and an 'outer part' or disc). We then compare the results from using these three different ways to classify our galaxies.We find that the fraction of galaxies selected as two-component galaxies increases on average 50 per cent from the lowest mass bin to the most massive galaxies, and decreases with redshift by a factor of 4 from z = 1 to 3. We find that single S{\'{e}}rsic 'disc-like' galaxies have the highest relative number densities at all redshifts, and that two-component galaxies have the greatest increase and become at par with S{\'{e}}rsic discs by z = 1. We also find that the systems we classify as two-component galaxies have an increase in the sizes of their outer components, or 'discs', by about a factor of 3 from z = 3 to 1.5, while the inner components or 'bulges' stay roughly the same size. This suggests that these systems are growing from the inside out, whilst the bulges or protobulges are in place early in the history of these galaxies. This is also seen to a lesser degree in the growth of single 'disc-like' galaxies versus 'spheroid-like' galaxies over the same epoch.}, -archivePrefix = {arXiv}, -arxivId = {1606.07405}, -author = {Margalef-Bentabol, Berta and Conselice, Christopher J and Mortlock, Alice and Hartley, Will and Duncan, Kenneth and Ferguson, Harry C and Dekel, Avishai and Primack, Joel R}, -doi = {10.1093/mnras/stw1451}, -eprint = {1606.07405}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure}, -number = {3}, -pages = {1--21}, -title = {{The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z {\textless} 3}}, -volume = {461}, -year = {2016} -} -@article{Holl2012, -abstract = {The Gaia mission has been designed to perform absolute astrometric measurements with unprecedented accuracy; the end-of-mission parallax standard error is required to be 30 micro-arcseconds for a G2V type star of magnitude 15. These requirements set a stringent constraint on the accuracy of the estimation of the location of the stellar image on the CCD for each observation: e.g., 0.3 milli-arseconds (mas) or 0.005 pixels for the same V=15 G2V star. However the Gaia CCDs will suffer from charge transfer inefficiency (CTI) caused by radiation damage that will degrade the stellar image quality and may degrade the astrometric performance of Gaia if not properly addressed. For the first time at this level of detail, the potential impact of radiation damage on the performance of Gaia is investigated. In this first paper we focus on the evaluation of the CTI impact on the image location accuracy. We show that CTI decreases the stellar image signal-to-noise ratio and irreversibly degrades the image location estimation precision. As a consequence the location estimation standard errors increase by up to 6{\%} for a radiation damage level equivalent to the end-of-mission. In addition the CTI-induced image distortion introduces a systematic bias in the image location estimation (up to 0.05 pixels or 3 mas in the Gaia operating conditions). We present a novel approach to CTI mitigation that enables, without correction of the raw data, the unbiased estimation of the image location and flux from damaged observations. Its implementation reduces the maximum measured location bias for the faintest magnitude to 0.005 pixels ({\$\sim${}}4e-4 pixels at magnitude 15). In a second paper we will investigate how the CTI effects affect the final astrometric accuracy of Gaia by propagating residual errors through the astrometric solution.}, -archivePrefix = {arXiv}, -arxivId = {1110.1547}, -author = {Holl, B and Prod'homme, T and Lindegren, L and Brown, A G A}, -doi = {10.1111/j.1365-2966.2012.20429.x}, -eprint = {1110.1547}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: numerical,Space vehicles}, -number = {4}, -pages = {2786--2807}, -title = {{The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solution}}, -volume = {422}, -year = {2012} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Costantin2017, -abstract = {Context. The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. Aims. We aim to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. Methods. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the i-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new (B=A, C=A) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. Results. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations of 25° ≤ $\theta$ ≤ 65° we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66{\%}), with a smaller fraction of prolate spheroids (19{\%}), and triaxial ellipsoids (15{\%}). The majority of triaxial bulges are in barred galaxies (75{\%}). Moreover, we found that bulges with low S{\'{e}}rsic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, bulges in late-type galaxies or in less massive galaxies have no preference for being oblate, prolate, or triaxial. On the contrary, bulges with high S{\'{e}}rsic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. Conclusions. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L and M{\'{e}}ndez-Abreu, J and Corsini, E M and Eliche-Moral, M C and Tapia, T and Morelli, L and Elena, Dalla Bont{\`{a}} and Pizzella, A}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -volume = {609}, -year = {2018} -} -@article{Hopkins2012, -abstract = {Feedback from massive stars is believed to play a critical role in driving galactic super-winds that enrich the intergalactic medium and shape the galaxy mass function, mass-metallicity relation and other global galaxy properties. In previous papers, we have introduced new numerical methods for implementing stellar feedback on sub-giant molecular cloud (sub-GMC) through galactic scales in numerical simulations of galaxies; the key physical processes include radiation pressure in the ultraviolet through infrared, supernovae (Type I and Type II), stellar winds ('fast' O star through 'slow' asymptotic giant branch winds), and Hii photoionization. Here, we show that these feedback mechanisms drive galactic winds with outflow rates as high as ∼10-20 times the galaxy star formation rate. The mass-loading efficiency (wind mass-loss rate divided by the star formation rate) scales roughly as M wind/M* ∞ V c-1 (where V c is the galaxy circular velocity), consistent with simple momentum-conservation expectations. We use our suite of simulations to study the relative contribution of each feedback mechanism to the generation of galactic winds in a range of galaxy models, from Small Magellanic Cloud like dwarfs and Milky Way (MW) analogues to z∼ 2 clumpy discs. In massive, gas-rich systems (local starbursts and high-z galaxies), radiation pressure dominates the wind generation. By contrast, for MW-like spirals and dwarf galaxies the gas densities are much lower and sources of shock-heated gas such as supernovae and stellar winds dominate the production of large-scale outflows. In all of our models, however, the winds have a complex multiphase structure that depends on the interaction between multiple feedback mechanisms operating on different spatial scales and time-scales: any single feedback mechanism fails to reproduce the winds observed. We use our simulations to provide fitting functions to the wind mass loading and velocities as a function of galaxy properties, for use in cosmological simulations and semi-analytic models. These differ from typically adopted formulae with an explicit dependence on the gas surface density that can be very important in both low-density dwarf galaxies and high-density gas-rich galaxies. {\textcopyright}2012 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.4638}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2012.20593.x}, -eprint = {1110.4638}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Stars: formation}, -number = {4}, -pages = {3522--3537}, -title = {{Stellar feedback in galaxies and the origin of galaxy-scale winds}}, -volume = {421}, -year = {2012} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work conducted to interpret this phenomenon has found that it is due to the non-spherical nature of dark matter halos. However, most studies overpredict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shapes of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations where satellite galaxies without associated subhalos ("orphan galaxies") are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region. {\textcopyright}2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W P and Kang, X and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%7B%5C%25%7D5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem%7B%5C&%7Dsid=IOPP%7B%5C%25%7D3Ajnl%7B%5C_%7Dref%7B%5C&%7Dspage=305%7B%5C&%7Dtitle=ArA%7B%5C&%7Dvolume=5%7B%5C&%7Ddate=1969%7B%5C&%7Dv%7B%5C}, -volume = {786}, -year = {2014} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) "CMASS" sample at {\$}z\backslashsim0.5{\$}. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogs which include selection effects, reproduce the overall SMF, the projected two-point correlation function {\$}w{\_}{\{}\backslashrm p{\}}{\$}, the CMASS {\$}dn/dz{\$}, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of "age matching" and show that these effects are markedly different compared to the ones explored by Hearin et al. (2013) at lower stellar masses. We construct two models, one in which galaxy color is stochastic ("AbM" model) as well as a model which contains assembly bias effects ("AgM" model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colors are not a stochastic process in high-mass halos. Our results suggest that the colors of galaxies in high-mass halos are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P and Bundy, Kevin and Zentner, Andrew R and Behroozi, Peter S and Reid, Beth A and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L and White, Martin and Schneider, Donald P}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Bosch2016, -abstract = {According to the Virial Theorem, all gravitational systems in equilibrium sit on a plane in the 3D parameter space defined by their mass, size and second moment of the velocity tensor. While these quantities cannot be directly observed, there are suitable proxies: the luminosity Lk, half-light radius Re and dispersion sigma_e. These proxies indeed lie on a very tight Fundamental Plane (FP). How do the black holes in the centers of galaxies relate to the FP? Their masses are known to exhibit no strong correlation with total galaxy mass, but they do correlate weakly with bulge mass (when present), and extremely well with the velocity dispersion through the Mbh = sigma_e^5.4 relation. These facts together imply that a tight plane must also exist defined by black hole mass, total galaxy mass and size. Here I show that this is indeed the case using a heterogeneous set of 230 black holes. The sample includes BHs from zero to 10 billion solar masses and host galaxies ranging from low surface brightness dwarfs, through bulge-less disks, to brightest cluster galaxies. The resulting BH-size-luminosity Mbh=(Lk/Re)^3.8 has the same amount of scatter as the M-sigma relation and is aligned with the galaxy FP, such that it is just a re-projection of sigma. The inferred BH-size-mass relation is Mbh=(M_star/Re)^2.9. These relationships are universal and extend to galaxies without bulges. This implies that the black hole is primarily correlated with its global velocity dispersion and not with the properties of the bulge. I show that the classical bulge--mass relation is a projection of the M-sigma relation. When the velocity dispersion cannot be measured (at high-z or low dispersions), the BH-size-mass relation should be used as a proxy for black hole mass in favor of just galaxy or bulge mass.}, -archivePrefix = {arXiv}, -arxivId = {1606.01246}, -author = {van den Bosch, Remco C. E.}, -doi = {10.3847/0004-637x/831/2/134}, -eprint = {1606.01246}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/VanDenBosch2016Unification.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {1,bulges,catalogs,dynamical scaling relations,fi gure set,fundamental parameters,galaxies,galaxies: bulges,galaxies: fundamental parameters,galaxies: kinematics and dynamics,gravitation,kinematics and dynamics,machine-readable tables,quasars,quasars: supermassive black holes,supermassive black holes,supporting material}, -number = {2}, -pages = {134}, -publisher = {IOP Publishing}, -title = {{Unification of the Fundamental Plane and Super Massive Black Hole Masses}}, -url = {http://dx.doi.org/10.3847/0004-637X/831/2/134}, -volume = {831}, -year = {2016} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Buckley2013, -abstract = {The dark matter halo of the Milky Way is expected to contain an abundance of smaller subhalos. These subhalos can be dense and produce potentially observable fluxes of gamma rays. In this paper, we search for dark matter subhalo candidates among the sources in the Fermi-LAT second source catalog which are not currently identified or associated with counterparts at other wavelengths. Of the nine high-significance, high-latitude (|b|>60°), nonvariable, unidentified sources contained in this catalog, only one or two are compatible with the spectrum of a dark matter particle heavier than approximately 50-100 GeV. The majority of these nine sources, however, feature a spectrum that is compatible with that predicted from a lighter (∼5-40GeV) dark matter particle. This population is consistent with the number of observable subhalos predicted for a dark matter candidate in this mass range and with an annihilation cross section of a simple thermal relic ($\sigma$v∼3×10 -26cm3/s). Observations in the direction of these sources at other wavelengths will be necessary to either reveal their astrophysical nature (as blazars or other active galactic nuclei, for example), or to further support the possibility that they are dark matter subhalos by failing to detect any non-gamma-ray counterpart. {\textcopyright} 2012 American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {1111.2613}, -author = {Belikov, Alexander V. and Buckley, Matthew R. and Hooper, Dan}, -doi = {10.1103/PhysRevD.86.043504}, -eprint = {1111.2613}, -issn = {15507998}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -number = {4}, -title = {{Searching for dark matter subhalos in the Fermi-LAT second source catalog}}, -volume = {86}, -year = {2012} -} -@article{Khochfar2011, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* > 1010.5M⊙ contributing $\sim$20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between $\sim$50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z > 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) > 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z < 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive (>1010M⊙) fast rotators being more than one order of magnitude more frequent at z$\sim$ 2. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R. and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Khochfar et al. - 2011 - The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies.pdf:pdf}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: structure}, -month = {oct}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Wang2013, -abstract = {We investigate the spatial distribution of galactic satellites in high-resolution simulations of structure formation in the $\Lambda$ cold dark matter ($\Lambda$CDM) model: the Aquarius dark matter simulations of individual haloes and the Millennium-II simulation of a large cosmological volume. To relate the simulations to observations of the Milky Way we use two alternative models to populate dark haloes with 'visible' galaxies: a semi-analytic model of galaxy formation and an abundance matching technique. We find that the radial density profile of massive satellites roughly follows that of the dark matter halo (unlike the distribution of dark matter subhaloes). Furthermore, our two galaxy formation models give resultsconsistent with the observed profile of the 11 classical satellites of the Milky Way. Our simulations predict that larger, fainter samples of satellites should still retain this profile at least up to samples of 100 satellites. The angular distribution of the classical satellites of the Milky Way is known to be highly anisotropic. Depending on the exact measure of flattening, 5-10 per cent of satellite systems in our simulations are as flat as the Milky Way's and this fraction does not change when we correct for possible obscuration of satellites by the Galactic disc. A moderate flattening ofsatellite systems is a general property of $\Lambda$CDM, best understood as the consequence of preferential accretion along filaments of the cosmic web. Accretion of a single rich group of satellites can enhance the flattening due to such anisotropic accretion. We verify that a typical Milky Way-mass cold dark matter halo does not acquire its 11 most massive satellites from a small number of rich groups. Single-group accretion becomes more likely for less massive satellites. Our model predictions should be testable with forthcoming studies of satellite systems in other galaxies and surveys of fainter satellites in the MilkyWay. {\textcopyright} 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1206.1340}, -author = {Wang, Jie and Frenk, Carlos S. and Cooper, Andrew P.}, -doi = {10.1093/mnras/sts442}, -eprint = {1206.1340}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang, Frenk, Cooper - 2013 - The spatial distribution of galactic satellites in the $\Lambda$ cold dark matter cosmology(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxy: formation,Galaxy: structure,Methods: numerical}, -number = {2}, -pages = {1502--1513}, -title = {{The spatial distribution of galactic satellites in the $\Lambda$ cold dark matter cosmology}}, -volume = {429}, -year = {2013} -} -@article{Krist2004, -abstract = {Point spread function (PSF) models are critical to Hubble Space Telescope (HST) data analysis. Astronomers unfamiliar with optical simulation techniques need access to PSF models that properly match the conditions of their observations, so any HST modeling software needs to be both easy-to-use and have detailed information on the telescope and instruments. The Tiny Tim PSF simulation software package has been the standard HST modeling software since its release in early 1992. We discuss the evolution of Tiny Tim over the years as new instruments and optical properties have been incorporated. We also demonstrate how Tiny Tim PSF models have been used for HST data analysis. Tiny Tim is freely available from tinytim.stsci.edu.}, -author = {Krist, John E. and Hook, Richard N. and Stoehr, Felix}, -doi = {10.1117/12.892762}, -isbn = {9780819487377}, -issn = {0277786X}, -journal = {Optical Modeling and Performance Predictions V}, -keywords = {hubble space telescope,point spread function}, -number = {2004}, -pages = {81270J}, -title = {{20 years of Hubble Space Telescope optical modeling using Tiny Tim}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.892762}, -volume = {8127}, -year = {2011} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ > 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright} 2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E. and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Raskutti, Greene, Murphy - 2014 - The stellar halos of massive elliptical galaxies. III. Kinematics at large radius(3).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{Veale2016, -abstract = {We present spatially-resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (MK {\textless}{\$\sim${}} -25.7 mag, stellar mass M* {\textgreater}{\$\sim${}} 10{\^{}}11.8 Msun) of the volume-limited (D {\textless} 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650 to 5850 A from the 246-fiber Mitchell integral-field spectrograph (IFS) at McDonald Observatory, covering a 107" x 107" field of view (often reaching 2 to 3 effective radii). We measure the 2-D spatial distribution of each galaxy's angular momentum (lambda and fast or slow rotator status), velocity dispersion (sigma), and higher-order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ({\$\sim${}}80{\%} ) of slow and non-rotators with lambda {\textless}{\$\sim${}} 0.2. When combined with the lower-mass ETGs in the ATLAS3D survey, we find the fraction of slow-rotators to increase dramatically with galaxy mass, reaching {\$\sim${}}50{\%} at MK {\$\sim${}} -25.5 mag and {\$\sim${}}90{\%} at MK {\textless}{\$\sim${}} -26 mag. All of our fast rotators show a clear anti-correlation between h3 and V/sigma, and the slope of the anti-correlation is steeper in more round galaxies. The radial profiles of sigma show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK {\textless}{\$\sim${}} -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat sigma profiles, whereas five of the seven "isolated" galaxies are all fainter than MK = -25.8 mag and have falling sigma. All of our galaxies have positive average h4; the most luminous galaxies have average h4 {\$\sim${}} 0.05 while less luminous galaxies have a range of values between 0 and 0.05. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising sigma profiles. We discuss the implications for the relationship among dynamical mass, sigma, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E and McConnell, Nicholas J and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ > 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright} 2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E. and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Raskutti, Greene, Murphy - 2014 - The stellar halos of massive elliptical galaxies. III. Kinematics at large radius(3).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -volume = {786}, -year = {2014} -} -@article{Barnabe2011, -abstract = {We combine in a self-consistent way the constraints from both gravitational lensing and stellar kinematics to perform a detailed investigation of the internal mass distribution, amount of dark matter, and dynamical structure of the 16 early-type lens galaxies from the Sloan Lens ACS Survey (SLACS Survey), at z= 0.08-0.33, for which both Hubble Space Telescope/Advanced camera for Surveys and NICMOS high-resolution imaging and Very Large Telescope VIMOS integral-field spectroscopy are available. Based on this data set, we analyse the inner regions of the galaxies, that is, typically within one (three-dimensional) effective radius re, under the assumption of axial symmetry and by constructing dynamical models supported by two-integral stellar distribution functions. For all systems, the total mass density distribution is found to be well approximated by a simple power law (with m being the ellipsoidal radius): this profile is on average slightly super-isothermal, with a logarithmic slope 〈$\gamma$'〉= 2.074+0.043-0.041 (errors indicate the 68 per cent confidence interval) and an intrinsic scatter, and is fairly round, with an average axial ratio 〈q〉= 0.77 ± 0.04. The lower limit for the dark matter fraction (fDM) inside re ranges, in individual systems, from nearly zero to almost a half, with a median value of 12 per cent. By including stellar masses derived from stellar population synthesis models with a Salpeter initial mass function (IMF), we obtain an average fDM= 31 per cent, and the corresponding stellar profiles are physically acceptable, with the exception of two cases where they only marginally exceed the total mass profile. fDM rises to 61 per cent if, instead, a Chabrier IMF is assumed. For both IMFs, the dark matter fraction increases with the total mass of the galaxy (correlation significant at the 3$\sigma$ level). Based on the intrinsic angular momentum parameter calculated from our models, we find that the galaxies can be divided into two dynamically distinct groups, which are shown to correspond to the usual classes of the (observationally defined) slow and fast rotators. Overall, the SLACS systems are structurally and dynamically very similar to their nearby counterparts, indicating that the inner regions of early-type galaxies have undergone little, if any, evolution since redshift z≈ 0.35. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1102.2261}, -author = {Barnab{\`{e}}, Matteo and Czoske, Oliver and Koopmans, L{\'{e}}on V.E. and Treu, Tommaso and Bolton, Adam S.}, -doi = {10.1111/j.1365-2966.2011.18842.x}, -eprint = {1102.2261}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: kinematics and dynamics,Galaxies: structure,Gravitational lensing: strong}, -month = {aug}, -number = {3}, -pages = {2215--2232}, -title = {{Two-dimensional kinematics of SLACS lenses - III. Mass structure and dynamics of early-type lens galaxies beyond z ≃ 0.1}}, -volume = {415}, -year = {2011} -} -@article{Newman2012a, -abstract = {The presence of extremely compact galaxies at z ∼ 2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 galaxies selected with 0.4 {\textless} z {\textless} 2.5 and stellar masses M* {\textgreater} 1010.7 M {\textperiodcentered}in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and the mean size of these systems at fixed stellar mass grows by a factor of 3.5 0.3 over this redshift interval. The data are sufficiently deep to identify companions to these hosts whose stellar masses are ten times smaller. By searching for these around 404 quiescent hosts within a physical annulus 10 h -1 kpc {\textless} R {\textless} 30 h -1 kpc, we estimate the minor merger rate over 0.4 {\textless} z {\textless} 2. We find that 13{\%}-18{\%} of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6{\%} ± 2{\%} per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers may explain most of the size evolution observed at z ≲ 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes. {\textcopyright}2012 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1110.1637}, -author = {Newman, Andrew B and Ellis, Richard S and Bundy, Kevin and Treu, Tommaso}, -doi = {10.1088/0004-637X/746/2/162}, -eprint = {1110.1637}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: structure}, -number = {2}, -title = {{Can minor merging account for the size growth of quiescent galaxies? New results from the CANDELS survey}}, -volume = {746}, -year = {2012} -} -@article{Mendez-Abreu2010, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M{\textgreater}10{\^{}}11 M{\_}sun) galaxies at 1.7{\textless}z{\textless}3 utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our sample is almost an order of magnitude larger than previous studies at these redshifts, providing the first statistical study of massive galaxy sizes at z{\textgreater}2, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n{\textless}2) and spheroid-like (n{\textgreater}2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z{\$\sim${}}2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z{\textgreater}2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ({\$\sim${}}2x10{\^{}}10 M{\_}sun kpc{\^{}}-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J and Bouwens, Rychard J and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -isbn = {1005-0302}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61----L64}, -title = {{ Size Evolution of the Most Massive Galaxies at 1.7 {\textless} z {\textless} 3 from GOODS NICMOS Survey Imaging }}, -url = {http://arxiv.org/abs/0807.4141%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Blei2017a, -abstract = {One of the core problems of modern statistics is to approximate difficult-to-compute probability densities. This problem is especially important in Bayesian statistics, which frames all inference about unknown quantities as a calculation involving the posterior density. In this article, we review variational inference (VI), a method from machine learning that approximates probability densities through optimization. VI has been used in many applications and tends to be faster than classical methods, such as Markov chain Monte Carlo sampling. The idea behind VI is to first posit a family of densities and then to find a member of that family which is close to the target density. Closeness is measured by Kullback–Leibler divergence. We review the ideas behind mean-field variational inference, discuss the special case of VI applied to exponential family models, present a full example with a Bayesian mixture of Gaussians, and derive a variant that uses stochastic optimization to scale up to massive data. We discuss modern research in VI and highlight important open problems. VI is powerful, but it is not yet well understood. Our hope in writing this article is to catalyze statistical research on this class of algorithms. Supplementary materials for this article are available online.}, -archivePrefix = {arXiv}, -arxivId = {1601.00670}, -author = {Blei, David M and Kucukelbir, Alp and McAuliffe, Jon D}, -doi = {10.1080/01621459.2017.1285773}, -eprint = {1601.00670}, -issn = {1537274X}, -journal = {Journal of the American Statistical Association}, -keywords = {Algorithms,Computationally intensive methods,Statistical computing}, -number = {518}, -pages = {859--877}, -title = {{Variational Inference: A Review for Statisticians}}, -volume = {112}, -year = {2017} -} -@article{Goulding2016a, -abstract = {Studies of the physical properties of local elliptical galaxies (e.g., gas temperatures, halo masses, stellar kinematics) are shedding new light on galaxy formation. Here we present the hot X-ray gas properties of 33 early-type systems within the MASSIVE galaxy survey sample that have archival Chandra X-ray observations. Through careful X-ray spectral modeling, we derive X-ray luminosities (L{\_}X) and plasma temperatures (T{\_}gas) for the diffuse gas components in these galaxies. We combine the MASSIVE sample with 41 galaxies from the ATLAS{\^{}}3D survey to investigate the X-ray and optical properties of a statistically significant sample of nearby early-type galaxies across a wide-range of environments. We deduce that all early-type galaxies (independent of galaxy mass and rotational support) follow a universal scaling law such that L{\_}X{\$\sim${}}T{\_}gas{\^{}}4.5. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, the wide-scale environment does not contribute to the intrinsic scatter ({\$\sim${}}0.5dex) within the scaling relation. We further demonstrate that the scatter in L{\_}X around both K-band luminosity (L{\_}K) and the galaxy stellar velocity dispersion is primarily driven by T{\_}gas, with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the origin of the gas directly to either the stellar mass or the galaxy potential. Indeed, our data require a steeper relation between L{\_}X, L{\_}K, and sigma{\_}e than predicted by standard mass-loss models. Finally, we find a statistically significant correlation between sigma{\_}e and T{\_}gas, suggesting that T{\_}gas is set by the galaxy potential inside the optical effective radius. We conclude that within the inner-most 10-30kpc region, early-types maintain pressure-supported hot gas, with a minimum T{\_}gas set by the virial temperature, but the majority show evidence for some additional heating.}, -archivePrefix = {arXiv}, -arxivId = {1604.01764}, -author = {Goulding, Andy D and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Bogdan, Akos and Nyland, Kristina and Blakeslee, John P and McConnell, Nicholas J and Thomas, Jens}, -doi = {10.3847/0004-637x/826/2/167}, -eprint = {1604.01764}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {167}, -title = {{the Massive Survey. Iv. the X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe}}, -url = {http://arxiv.org/abs/1604.01764%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/826/2/167}, -volume = {826}, -year = {2016} -} -@article{Johnston2016, -abstract = {With the availability of large integral-field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, how galaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present BUDDI, a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GalfitM, a modified form of Galfit which can fit multi-waveband images simultaneously. The benefit of this technique over traditional multi-waveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the SDSS-IV Mapping Nearby Galaxies at APO (MaNGA) survey with redshifts z{\textless}0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec FWHM and field of view of {\textgreater}22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from the MaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data.}, -archivePrefix = {arXiv}, -arxivId = {1611.00609}, -author = {Johnston, Evelyn J and H{\"{a}}u{\ss}ler, Boris and Arag{\'{o}}n-Salamanca, Alfonso and Merrifield, Michael R and Bamford, Steven and Bershady, Matthew A and Bundy, Kevin and Drory, Niv and Fu, Hai and Law, David and Nitschelm, Christian and Thomas, Daniel and Lopes, Alexandre Roman and Wake, David and Yan, Renbin}, -doi = {10.1093/mnras/stw2823}, -eprint = {1611.00609}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content,Galaxies: structure}, -number = {2}, -pages = {2317--2341}, -title = {{SDSS-IV MaNGA: Bulge-disc decomposition of IFU data cubes (BUDDI)}}, -url = {http://arxiv.org/abs/1611.00609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2823}, -volume = {465}, -year = {2017} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -publisher = {MNRAS}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Smith2015, -abstract = {We present results from a blind survey to identify strong gravitational lenses among the population of low-redshift early-type galaxies. The SINFONI Nearby Elliptical Lens Locator Survey (SNELLS) uses integral-field infrared spectroscopy to search for lensed emission line sources behind massive lens candidates at z < 0.055. From 27 galaxies observed, we have recovered one previously known lens (ESO 325-G004) at z = 0.034, and discovered two new systems, at z = 0.031 and 0.052. All three lens galaxies have high velocity dispersions ($\sigma$ >300 km s-1) and $\alpha$-element abundances ([Mg/Fe]>0.3). From the lensing configurations we derive total J-band mass-to-light ratios of 1.8 ± 0.1, 2.1 ± 0.1 and 1.9 ± 0.2 within the $\sim$2 kpc Einstein radius. Correcting for estimated dark matter contributions, and comparing to stellar population models with a Milky Way (Kroupa) initial mass function (IMF), we determine the 'mass excess factor', $\alpha$. Assuming the lens galaxies have 'old' stellar populations (10 ± 1 Gyr), the average IMF mass factor is 〈$\alpha$〉 = 1.10 ± 0.08 ± 0.10, where the first error is random and the second is systematic. If we instead fit the stellar populations from 6dF optical survey spectra, all three galaxies are consistent with being old, but the age errors are 3-4 Gyr, due to limited signal-to-noise ratio. The IMF constraints are therefore looser in this case, with 〈$\alpha$〉 = 1.23+0.16 -0.13 ± 0.10. Our results are thus consistent with a Kroupa IMF ($\alpha$ = 1.00) on average, and strongly reject very heavy IMFs with $\alpha$ ≳ 2. A Salpeter IMF ($\alpha$ = 1.55) is inconsistent at the 3.5$\sigma$ level if the galaxies are old, but cannot be excluded using age constraints derived from the currently available optical spectra.}, -archivePrefix = {arXiv}, -arxivId = {1503.02661}, -author = {Smith, Russell J. and Lucey, John R. and Conroy, Charlie}, -doi = {10.1093/mnras/stv518}, -eprint = {1503.02661}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: stellar content,Gravitational lensing: strong,Stars: luminosity function,cD,mass function}, -number = {4}, -pages = {3441--3457}, -pmid = {8392081}, -title = {{The SINFONI nearby elliptical lens locator survey: Discovery of two new low-redshift strong lenses and implications for the initial mass function in giant early-type galaxies}}, -volume = {449}, -year = {2015} -} -@article{Grant2006, -abstract = {Soon after launch, the Advanced CCD Imaging Spectrometer (ACIS), one of the focal plane instruments on the Chandra X-ray Observatory, suffered radiation damage from exposure to soft protons during passages through the Earth's radiation belts. The primary effect of the damage was to increase the charge transfer inefficiency (CTI) of the eight front illuminated CCDs by more than two orders of magnitude. The ACIS instrument team is continuing to study the properties of the damage with an emphasis on developing techniques to mitigate CTI and spectral resolution degradation. We present the initial temperature dependence of ACIS CTI from -120 to -60 degrees Celsius and the current temperature dependence after more than six years of continuing slow radiation damage. We use the change of shape of the temperature dependence to speculate on the nature of the damaging particles.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0606178}, -author = {Grant, C E and Bautz, M W and Kissel, S E and LaMarr, B and Prigozhin, G Y}, -doi = {10.1117/12.672019}, -eprint = {0606178}, -isbn = {0819463418}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy II}, -keywords = {acis,chandra,charge coupled devices,charge transfer inefficiency,radiation damage}, -pages = {62761O}, -primaryClass = {astro-ph}, -title = {{Temperature dependence of charge transfer inefficiency in Chandra X-ray CCDs}}, -url = {http://arxiv.org/abs/astro-ph/0606178%7B%5C%25%7D0Ahttp://dx.doi.org/10.1117/12.672019}, -volume = {6276}, -year = {2006} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the 'Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a (100 cMpc)3 and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts 0 and 1, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar 'downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G. and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S. and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rosas-Guevara et al. - 2016 - Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Chirivi2017, -abstract = {Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we aim to present the first attempt at modelling line-of-sight (LOS) mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We have focussed on the Hubble Frontier Field cluster MACS J0416.1-2403, and our multi-plane model reproduces the observed image positions with a rms offset of {\$\sim${}}0.′′53. Starting from this best-fitting model, we simulated a mock cluster that resembles MACS J0416.1-2403 in order to explore the effects of LOS structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms {\$\sim${}}0.′′3); accounting for LOS galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factor of the lensed multiple images are recovered within {\$\sim${}}10{\%} for {\$\sim${}}95{\%} of them, those {\$\sim${}}5{\%} that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models. In addition, LOS galaxies cannot explain the apparent discrepancy in the properties of massive sub-halos between MACS J0416.1-2403 and N-body simulated clusters. Since our model of MACS J0416.1-2403 with LOS galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities would be needed in future models of MACS J0416.1-2403.}, -archivePrefix = {arXiv}, -arxivId = {1706.07815}, -author = {Chiriv{\`{i}}, G and Suyu, S H and Grillo, C and Halkola, A and Balestra, I and Caminha, G B and Mercurio, A and Rosati, P}, -doi = {10.1051/0004-6361/201731433}, -eprint = {1706.07815}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Dark matter,Galaxies: clusters: general,Galaxies: clusters: individual: MACS J0416.1-2403,Gravitational lensing: strong}, -pages = {1--29}, -title = {{MACS J0416.1-2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters}}, -url = {http://arxiv.org/abs/1706.07815%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731433}, -volume = {614}, -year = {2018} -} -@article{Pontzen2012, -abstract = {We propose and successfully test against new cosmological simulations a novel analytical description of the physical processes associated with the origin of cored dark matter density profiles. In the simulations, the potential in the central kiloparsec changes on sub-dynamical time-scales over the redshift interval 4 > z > 2, as repeated, energetic feedback generates large underdense bubbles of expanding gas from centrally concentrated bursts of star formation. The model demonstrates how fluctuations in the central potential irreversibly transfer energy into collisionless particles, thus generating a dark matter core. A supply of gas undergoing collapse and rapid expansion is therefore the essential ingredient. The framework, based on a novel impulsive approximation, breaks with the reliance on adiabatic approximations which are inappropriate in the rapidly changing limit. It shows that both outflows and galactic fountains can give rise to cusp flattening, even when only a few per cent of the baryons form stars. Dwarf galaxies maintain their core to the present time. The model suggests that constant density dark matter cores will be generated in systems of a wide mass range if central starbursts or active galactic nucleus phases are sufficiently frequent and energetic. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1106.0499}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1111/j.1365-2966.2012.20571.x}, -eprint = {1106.0499}, -isbn = {doi:10.1111/j.1365-2966.2012.20571.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: dwarf}, -month = {apr}, -number = {4}, -pages = {3464--3471}, -title = {{How supernova feedback turns dark matter cusps into cores}}, -volume = {421}, -year = {2012} -} -@article{Arango-Toro2023, -abstract = {Context. Radio used as a tracer of the star formation rate (SFR) presents enormous advantages because it is not affected by dust and radio sources that are located at the subarcsecond level. The interpretation of the low-frequency 1.4 GHz luminosity is hampered by the difficulty of modeling the paths of cosmic rays in the interstellar medium, however, and by their interactions with the magnetic field. Aims. We compare the SFR derived from radio observations and the SFRs derived from spectral energy distribution (SED) modeling. We aim at better understanding the behavior of the SFR radio tracer, with a specific emphasis on the link to star formation histories (SFHs). Methods. The analysis is based on a subsample of 1584 star-forming galaxies extracted from the Cosmic Evolution Survey (COSMOS) with observations of the Very large array project at 3 GHz. We used the SED modeling code investigating galaxy emission, CIGALE, with a nonparametric model for the SFH and fit the data over the wavelength range from the ultraviolet (UV) to the mid-infrared (mid-IR). We interpret the difference between radio and SED-based SFR tracers in the light of recent gradients in the derived SFH. To validate the robustness of the results, we searched for any remaining contribution of active galaxy nuclei and tested the impact of our SFH modeling approach. Results. Approximately 27% our galaxies present a radio SFR (SFRradio) that is at least ten times higher than the instantaneous SFR from SED fitting (SFRSED). This trend primarily affects the galaxies whose SFH activity decreased over the last 300 Myr. Both SFR indicators converge toward a consistent value when the SFHs are averaged over a period longer than 150 Myr to derive SFRSED. Conclusions. Although the radio at a low frequency of 1.4 GHz is a good tracer of the star formation activity of galaxies with a constant or increasing SFH, our results indicate that this is not the case for quenched galaxies. Our analysis suggests that the star formation time sensitivity of the low radio frequency might be longer than 150 Myr. Interestingly, the discrepancy between the SFRradio and SFRSED can be used as diagnostic to select post-starburst galaxies.}, -author = {Arango-Toro, R. C. and Ciesla, L. and Ilbert, O. and Magnelli, B. and Jim{\'{e}}nez-Andrade, E. F. and Buat, V.}, -doi = {10.1051/0004-6361/202345848}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/ArangoToro2023CIGALE.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Galaxies: statistics}, -pages = {1--10}, -title = {{Probing the timescale of the 1.4 GHz radio emissions as a star formation tracer}}, -volume = {675}, -year = {2023} -} -@article{Morningstar2019, -abstract = {We present a machine learning method for the reconstruction of the undistorted images of background sources in strongly lensed systems. This method treats the source as a pixelated image and utilizes the Recurrent Inference Machine (RIM) to iteratively reconstruct the background source given a lens model. Our architecture learns to minimize the likelihood of the model parameters (source pixels) given the data using the physical forward model (ray tracing simulations) while implicitly learning the prior of the source structure from the training data. This results in better performance compared to linear inversion methods, where the prior information is limited to the 2-point covariance of the source pixels approximated with a Gaussian form, and often specified in a relatively arbitrary manner. We combine our source reconstruction network with a convolutional neural network that predicts the parameters of the mass distribution in the lensing galaxies directly from telescope images, allowing a fully automated reconstruction of the background source images and the foreground mass distribution.}, -archivePrefix = {arXiv}, -arxivId = {1901.01359}, -author = {Morningstar, Warren R and Levasseur, Laurence Perreault and Hezaveh, Yashar D and Blandford, Roger and Marshall, Phil and Putzky, Patrick and Rueter, Thomas D and Wechsler, Risa and Welling, Max}, -eprint = {1901.01359}, -title = {{Data-Driven Reconstruction of Gravitationally Lensed Galaxies using Recurrent Inference Machines}}, -url = {http://arxiv.org/abs/1901.01359}, -year = {2019} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism, which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio (M/L) and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R, z) and characterized by the classic anisotropy parameter. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters ($\beta$z and the inclination), the models generally provide remarkably good descriptions of the shape of the first (V) and second () velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the dynamical structure of these objects. With the observationally motivated assumption that $\beta$z ≳ 0, the method is able to recover the inclination. The technique can be used to determine the dynamical M/L and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modelling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy and multiple kinematic components. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Salvatier2016, -abstract = {Probabilistic programming allows for automatic Bayesian inference on user-defined probabilistic models. Recent advances in Markov chain Monte Carlo (MCMC) sampling allow inference on increasingly complex models. This class of MCMC, known as Hamiltonian Monte Carlo, requires gradient information which is often not readily available. PyMC3 is a new open source probabilistic programming framework written in Python that uses Theano to compute gradients via automatic differentiation as well as compile probabilistic programs on-the-fly to C for increased speed. Contrary to other probabilistic programming languages, PyMC3 allows model specification directly in Python code. The lack of a domain specific language allows for great flexibility and direct interaction with the model. This paper is a tutorial-style introduction to this software package.}, -archivePrefix = {arXiv}, -arxivId = {1507.08050}, -author = {Salvatier, John and Wiecki, Thomas V and Fonnesbeck, Christopher}, -doi = {10.7717/peerj-cs.55}, -eprint = {1507.08050}, -issn = {23765992}, -journal = {PeerJ Computer Science}, -keywords = {Bayesian statistic,Markov chain Monte Carlo,Probabilistic Programming,Python,Statistical modeling}, -number = {4}, -pages = {1--24}, -title = {{Probabilistic programming in Python using PyMC3}}, -volume = {2016}, -year = {2016} -} -@article{Bouwens2012, -abstract = {Ultra-deep Advanced Camera for Surveys (ACS) and WFC3/IR HUDF+HUDF09 data, along with the wide-area GOODS+ERS+CANDELS data over the CDF-S GOODS field, are used to measure UV colors, expressed as the UV-continuum slope $\beta$, of star-forming galaxies over a wide range of luminosity (0.1L* z = 3 to 2L*z = 3) at high redshift (z ∼ 7 to z ∼ 4). $\beta$ is measured using all ACS and WFC3/IR passbands uncontaminated by Ly$\alpha$ and spectral breaks. Extensive tests show that our $\beta$ measurements are only subject to minimal biases. Using a different selection procedure, Dunlop et al. recently found large biases in their $\beta$ measurements. To reconcile these different results, we simulated both approaches and found that $\beta$ measurements for faint sources are subject to large biases if the same passbands are used both to select the sources and to measure $\beta$. High-redshift galaxies show a well-defined rest-frame UV color-magnitude (CM) relationship that becomes systematically bluer toward fainter UV luminosities. No evolution is seen in the slope of the UV CM relationship in the first 1.5Gyr, though there is a small evolution in the zero point to redder colors from z ∼ 7 to z ∼ 4. This suggests that galaxies are evolving along a well-defined sequence in the L UV-color ($\beta$) plane (a "star-forming sequence"?). Dust appears to be the principal factor driving changes in the UV color $\beta$ with luminosity. These new larger $\beta$ samples lead to improved dust extinction estimates at z ∼ 4-7 and confirm that the extinction is essentially zero at low luminosities and high redshifts. Inclusion of the new dust extinction results leads to (1) excellent agreement between the star formation rate (SFR) density at z ∼ 4-8 and that inferred from the stellar mass density; and (2) to higher specific star formation rates (SSFRs) at z ≳ 4, suggesting that the SSFR may evolve modestly (by factors of 2) from z ∼ 4-7 to z ∼ 2. {\textcopyright} 2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1109.0994}, -author = {Bouwens, R. J. and Illingworth, G. D. and Oesch, P. A. and Franx, M. and Labb{\'{e}}, I. and Trenti, M. and {Van Dokkum}, P. and Carollo, C. M. and Gonz{\'{a}}lez, V. and Smit, R. and Magee, D.}, -doi = {10.1088/0004-637X/754/2/83}, -eprint = {1109.0994}, -isbn = {0004-637X}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: high-redshift}, -month = {aug}, -number = {2}, -pages = {83}, -title = {{UV-continuum slopes at z ∼ 4-7 from the HUDF09+ERS+CANDELS observations: Discovery of a well-defined UV color-magnitude relationship for z ≥ 4 star-forming galaxies}}, -url = {http://adsabs.harvard.edu/abs/2012ApJ...754...83B}, -volume = {754}, -year = {2012} -} -@article{Iwanus2017, -abstract = {We describe and test a novel Dark Matter Annihilation Feedback (DMAF) scheme that has been implemented into the well known cosmological simulation code {\$}\backslash{\$}textsf{\{}GADGET-2{\}}. In the models considered here, dark matter can undergo self-annihilation/decay into radiation and baryons. These products deposit energy into the surrounding gas particles and then the dark matter/baryon fluid is self-consistently evolved under gravity and hydrodynamics. We present tests of this new feedback implementation in the case of idealised dark matter halos with gas components for a range of halo masses, concentrations and annihilation rates. For some dark matter models, DMAF's ability to evacuate gas is enhanced in lower mass, concentrated halos where the injected energy is comparable to its gravitational binding energy. Therefore, we expect the strongest signs of dark matter annihilation to imprint themselves onto the baryonic structure of concentrated dwarf galaxies through their baryonic fraction and star formation history. Finally we present preliminary results of the first self-consistent DMAF cosmological box simulations showing that the small scale substructure is washed out for large annihilation rates.}, -archivePrefix = {arXiv}, -arxivId = {1707.06770}, -author = {Iwanus, N and Elahi, P J and Lewis, G F}, -doi = {10.1093/MNRAS/STX1974}, -eprint = {1707.06770}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Large-scale structure of Universe}, -number = {1}, -pages = {1214--1225}, -title = {{Dark matter annihilation feedback in cosmological simulations - I: Code convergence and idealized haloes}}, -url = {http://arxiv.org/abs/1707.06770%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1974}, -volume = {472}, -year = {2017} -} -@article{Sahu2019, -abstract = {Analyzing a sample of 84 early-type galaxies with directly-measured super-massive black hole masses---nearly doubling the sample size of such galaxies with multi-component decompositions---a symmetric linear regression on the reduced (merger-free) sample of 76 galaxies reveals {\$}M{\_}{\{}BH{\}}\backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.27\backslashpm 0.07{\}}{\$} with a total scatter of {\$}\backslashDelta{\_}{\{}rms{\}}={\$} 0.52 dex in the {\$}\backslashlog(M{\_}{\{}BH{\}}){\$} direction. However, and importantly, we discover that the ES/S0-type galaxies with disks are offset from the E-type galaxies by more than a factor of ten in their {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio, with ramifications for formation theories, simulations, and some virial factor measurements used to convert AGN virial masses into {\$}M{\_}{\{}BH{\}}{\$}. Separately, each population follows a steeper relation with slopes of {\$}1.86\backslashpm0.20{\$} and {\$}1.90\backslashpm0.20{\$}, respectively. The offset mass ratio is mainly due to the exclusion of the disk mass, with the two populations offset by only a factor of two in their {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,gal{\}}{\$} ratio in the {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,gal{\}}{\$} diagram where {\$}M{\_}{\{}BH{\}}\backslashpropto M{\_}{\{}*,gal{\}}{\^{}}{\{}1.8\backslashpm 0.2{\}}{\$} and {\$}\backslashDelta{\_}{\{}rms{\}}=0.6\backslashpm 0.1{\$} dex depending on the sample. For {\$}M{\_}{\{}BH{\}} \backslashgtrsim 10{\^{}}7 M{\_}{\{}\backslashodot{\}}{\$}, we detect no significant bend nor offset in either the {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,sph{\}}{\$} or {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,gal{\}}{\$} relations due to barred versus non-barred, or core-S$\backslash$'ersic versus S$\backslash$'ersic, early-type galaxies. For reference, the ensemble of late-type galaxies (which invariably are S$\backslash$'ersic galaxies) follow {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}{\$}-{\$}M{\_}{\{}*,gal{\}}{\$} relations with slopes equal to {\$}2.16\backslashpm 0.32{\$} and {\$}3.05\backslashpm 0.70{\$}, respectively. Finally, we provide some useful conversion coefficients, {\$}\backslashupsilon{\$}, accounting for the different stellar mass-to-light ratios used in the literature, and we report the discovery of a local, compact massive spheroid in NGC 5252.}, -archivePrefix = {arXiv}, -arxivId = {1903.04738}, -author = {Sahu, Nandini and Graham, Alister W and Davis, Benjamin L}, -doi = {10.3847/1538-4357/ab0f32}, -eprint = {1903.04738}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {black hole physics,bulges,cd,elliptical and lenticular,evolution,galaxies,photometry,structure}, -number = {2}, -pages = {155}, -title = {{ Black Hole Mass Scaling Relations for Early-type Galaxies. I. M BH – M *, sph and M BH – M *,gal }}, -volume = {876}, -year = {2019} -} -@misc{Grogin2010c, -author = {Grogin, N}, -howpublished = {HST Proposal}, -month = {sep}, -title = {{CCD Stability Monitor}}, -year = {2010} -} -@article{Dekel2014, -abstract = {We study the origin of high-redshift, compact, quenched spheroids (red nuggets) through the dissipative shrinkage of gaseous discs into compact star-forming systems (blue nuggets). The discs, fed by cold streams, undergo violent disc instability that drives gas into the centre (along with mergers). The inflow is dissipative when its time-scale is shorter than the star formation time-scale. This implies a threshold of $\sim$0.28 in the cold-to-total mass ratio within the disc radius. For the typical gas fraction $\sim$0.5 at z $\sim$ 2, this threshold is traced back to a maximum spin parameter of $\sim$0.05, implying that $\sim$half the star-forming galaxies contract to blue nuggets, while the rest form extended stellar discs. Thus, the surface density of blue galaxies is expected to be bimodal about $\sim$109M⊙ kpc-2, slightly increasing with mass. The blue nuggets are expected to be rare at low z when the gas fraction is low. The blue nuggets quench to red nuggets by complementary internal and external mechanisms. Internal quenching by a compact bulge, in a fast mode and especially at high z, may involve starbursts, stellar and active galactic nucleus feedback, or Q-quenching. Quenching due to hot-medium haloes above 1012M⊙ provides maintenance and a slower mode at low redshift. These predictions are confirmed in simulations and are consistent with observations at z = 0-3. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1310.1074}, -author = {Dekel, A. and Burkert, A.}, -doi = {10.1093/mnras/stt2331}, -eprint = {1310.1074}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Spiral,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics}, -month = {feb}, -number = {2}, -pages = {1870--1879}, -title = {{Wet disc contraction to galactic blue nuggets and quenching to red nuggets}}, -url = {http://arxiv.org/abs/1310.1074%0Ahttp://dx.doi.org/10.1093/mnras/stt2331}, -volume = {438}, -year = {2014} -} -@article{Wang2018a, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}} \backslashbackslashleqslant M{\_}{\{}\backslashbackslashast{\{}\backslash{\}}{\}} \backslashbackslashleqslant 10{\^{}}{\{}11.9{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashbackslashlangle\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}\backslashbackslashrangle = 2.003 \backslashbackslashpm 0.008{\$} and a standard deviation of {\$}\backslashbackslashsigma{\{}\backslash{\_}{\}}{\{}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}mw{\{}\backslash{\}}{\}}{\}}{\^{}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}-f{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}DM{\{}\backslash{\}}{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -year = {2018} -} -@article{2001et, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Geometryeg, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Despali2018, -abstract = {We investigate how Einstein rings and magnified arcs are affected by small-mass dark-matter haloes placed along the line of sight to gravitational lens systems. By comparing the gravitational signature of line-of-sight haloes with that of substructures within the lensing galaxy, we derive a mass-redshift relation that allows us to rescale the detection threshold (i.e. lowest detectable mass) for substructures to a detection threshold for line-of-sight haloes at any redshift. We then quantify the line-of-sight contribution to the total number density of lowmass objects that can be detected through strong gravitational lensing. Finally, we assess the degeneracy between substructures and line-of-sight haloes of different mass and redshift to provide a statistical interpretation of current and future detections, with the aim of distinguishing between cold dark matter and warm dark matter. We find that line-of-sight haloes statistically dominate with respect to substructures, by an amount that strongly depends on the source and lens redshifts, and on the chosen dark-matter model. Substructures represent about 30 percent of the total number of perturbers for low lens and source redshifts (as for the SLACS lenses), but less than 10 per cent for high-redshift systems. We also find that for data with high enough signal-to-noise ratio and angular resolution, the non-linear effects arising from a double-lens-plane configuration are such that one is able to observationally recover the line-of-sight halo redshift with an absolute error precision of 0.15 at the 68 per cent confidence level.}, -archivePrefix = {arXiv}, -arxivId = {1710.05029}, -author = {Despali, Giulia and Vegetti, Simona and White, Simon D.M. and Giocoli, Carlo and van den Bosch, Frank C.}, -doi = {10.1093/mnras/sty159}, -eprint = {1710.05029}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Despali et al. - 2018 - Modelling the line-of-sight contribution in substructure lensing.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Gravitational lensing: strong,Large-scale structure of Universe-}, -number = {4}, -pages = {5424--5442}, -title = {{Modelling the line-of-sight contribution in substructure lensing}}, -volume = {475}, -year = {2018} -} -@article{Keeton1997, -abstract = {Galaxies modeled as singular isothermal ellipsoids with an axis ratio distribution similar to the observed axis ratio distribution of E and S0 galaxies are statistically consistent with both the observed numbers of two-image and four-image lenses and the inferred ellipticities of individual lenses. However, no four-image lens is well fit by the model (typical {\$}\backslashbackslashchi{\{}\backslash{\^{}}{\{}{\}}{\}}2/N{\_}{\{}dof{\}} \backslashbackslashsim 20{\$}), the axis ratio of the model can be significantly different from that of the observed lens galaxy, and the major axes of the model and the galaxy may be slightly misaligned. We found that models with a second, independent, external shear axis could fit the data well (typical {\$}\backslashbackslashchi{\{}\backslash{\^{}}{\{}{\}}{\}}2/N{\_}{\{}dof{\}} \backslashbackslashsim 1{\$}), while adding the same number of extra parameters to the radial mass distribution does not produce such a dramatic improvement in the fit. An independent shear axis can be produced by misalignments between the luminous galaxy and its dark matter halo, or by external shear perturbations due to galaxies and clusters correlated with the primary lens or along the line of sight. We estimate that the external shear perturbations have no significant effect on the expected numbers of two-image and four-image lenses, but that they can be important perturbations in individual lens models. However, the amplitudes of the external shears required to produce the good fits are larger than our estimates for typical external shear perturbations (10-15{\%} shear instead of 1-3{\%} shear) suggesting that the origin of the extra angular structure must be intrinsic to the primary lens galaxy in most cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610163}, -author = {Keeton, C R and Kochanek, C S and Seljak, U}, -doi = {10.1086/304172}, -eprint = {9610163}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Elliptical and Lenticular,cD,cosmology: theory}, -number = {2}, -pages = {604--620}, -primaryClass = {astro-ph}, -title = {{Shear and Ellipticity in Gravitational Lenses}}, -url = {http://arxiv.org/abs/astro-ph/9610163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/304172}, -volume = {482}, -year = {1996} -} -@article{Sonnenfeld2024, -abstract = {Strong gravitational lensing observations can provide extremely valuable information on the structure of galaxies, but their interpretation is made difficult by selection effects, which, if not accounted for, introduce a bias between the properties of strong lens galaxies and those of the general population. A rigorous treatment of the strong lensing bias requires, in principle, to fully forward model the lens selection process. However, doing so for existing lens surveys is prohibitively difficult. With this work we propose a practical solution to the problem: using an empirical model to capture the most complex aspects of the lens finding process, and constraining it directly from the data together with the properties of the lens population. We applied this method to real data from the SLACS sample of strong lenses. Assuming a power-law density profile, we recovered the mass distribution of the parent population of galaxies from which the SLACS lenses were drawn. We found that early-type galaxies with a stellar mass of $ odot =11.3$ and average size have a median projected mass enclosed within a $5$ kpc aperture of $ odot and an average logarithmic density slope of $ These values are respectively $0.02$ dex and $0.1$ lower than inferred when ignoring selection effects. According to our model, most of the bias is due to the prioritisation of SLACS follow-up observations based on the measured velocity dispersion. As a result, the strong lensing bias in gamma reduces to $ when controlling for stellar velocity dispersion.}, -archivePrefix = {arXiv}, -arxivId = {2407.04771}, -author = {Sonnenfeld, Alessandro}, -doi = {10.1051/0004-6361/202451341}, -eprint = {2407.04771}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnenfeld2024SlacsDebiased.pdf:pdf}, -issn = {0004-6361}, -journal = {Astronomy & Astrophysics}, -keywords = {cd - galaxies,elliptical and lenticular,fundamental parameters,gravitational lensing,strong - galaxies}, -pages = {325}, -title = {{The SLACS strong lens sample, debiased}}, -volume = {690}, -year = {2024} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism, which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio (M/L) and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R, z) and characterized by the classic anisotropy parameter. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters ($\beta$z and the inclination), the models generally provide remarkably good descriptions of the shape of the first (V) and second () velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the dynamical structure of these objects. With the observationally motivated assumption that $\beta$z ≳ 0, the method is able to recover the inclination. The technique can be used to determine the dynamical M/L and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modelling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy and multiple kinematic components. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cappellari - 2008 - Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stella(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Momcheva2015, -abstract = {We present the spectroscopic redshift catalog from a wide-field survey of the fields of 28 galaxy-mass strong gravitational lenses. We discuss the acquisition and reduction of the survey data, collected over 40 nights of 6.5 m MMT and Magellan time, employing four different multiobject spectrographs. We determine that no biases are introduced by combining data sets obtained with different telescope and spectrograph combinations. Special care is taken to determine redshift uncertainties using repeat observations. The redshift catalog consists of 9,768 new and unique galaxy redshifts. 82.4% of the catalog redshifts are between z = 0.1 and z = 0.7, and the catalog median redshift. The data from this survey will be used to study the lens environments and line-of-sight structures to gain a better understanding of the effects of large-scale structure on lens statistics and lens-derived parameters.}, -archivePrefix = {arXiv}, -arxivId = {1503.02074}, -author = {Momcheva, Ivelina G. and Williams, Kurtis A. and Cool, Richard J. and Keeton, Charles R. and Zabludoff, Ann I.}, -doi = {10.1088/0067-0049/219/2/29}, -eprint = {1503.02074}, -isbn = {1091-4269}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: distances and redshifts,galaxies: general,gravitational lensing: strong,surveys}, -number = {2}, -pages = {29}, -title = {{A SPECTROSCOPIC SURVEY of the FIELDS of 28 STRONG GRAVITATIONAL LENSES}}, -url = {http://stacks.iop.org/0067-0049/219/i=2/a=29?key=crossref.a5471e69f1ffb2b3fc0f578df7cf09b5}, -volume = {219}, -year = {2015} -} -@article{Birrer2018, -abstract = {We present a blind time-delay strong lensing (TDSL) cosmographic analysis of the doubly imaged quasar SDSS 1206+4332. We combine the relative time delay between the quasar images, Hubble Space Telescope imaging, the Keck stellar velocity dispersion of the lensing galaxy, and wide-field photometric and spectroscopic data of the field to constrain two angular diameter distance relations. The combined analysis is performed by forward modelling the individual data sets through a Bayesian hierarchical framework, and it is kept blind until the very end to prevent experimenter bias. After unblinding, the inferred distances imply a Hubble constant H 0 = 68.8 +5.4-5.1 km s '1 Mpc '1, assuming a flat cold dark matter cosmology with uniform prior on m in [0.05, 0.5]. The precision of our cosmographic measurement with the doubly imaged quasar SDSS 1206+4332 is comparable with those of quadruply imaged quasars and opens the path to perform on selected doubles the same analysis as anticipated for quads. Our analysis is based on a completely independent lensing code than our previous three H0LiCOW systems and the new measurement is fully consistent with those. We provide the analysis scripts paired with the publicly available software to facilitate independent analysis (footnote with link to www.h0licow.org). The consistency between blind measurements with independent codes provides an important sanity check on lens modelling systematics. By combining the likelihoods of the four systems under the same prior, we obtain H 0 = 72.5 +2.1-2.3 km s '1 Mpc '1. This measurement is independent of the distance ladder and other cosmological probes.}, -archivePrefix = {arXiv}, -arxivId = {1809.01274}, -author = {Birrer, S and Treu, T and Rusu, C E and Bonvin, V and Fassnacht, C D and Chan, J H H and Agnello, A and Shajib, A J and Chen, G C F and Auger, M and Courbin, F and Hilbert, S and Sluse, D and Suyu, S H and Wong, K C and Marshall, P and Lemaux, B C and Meylan, G}, -doi = {10.1093/mnras/stz200}, -eprint = {1809.01274}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmological parameters,dark energy,ravitational lensing: strong}, -number = {4}, -pages = {4726--4753}, -title = {{H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant}}, -url = {http://arxiv.org/abs/1809.01274}, -volume = {484}, -year = {2019} -} -@article{Geometryed, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Ma2014, -abstract = {Massive early-type galaxies represent the modern day remnants of the earliest major star formation episodes in the history of the universe. These galaxies are central to our understanding of the evolution of cosmic structure, stellar populations, and supermassive black holes, but the details of their complex formation histories remain uncertain. To address this situation, we have initiated the MASSIVE Survey, a volume-limited, multi-wavelength, integral-field spectroscopic (IFS) and photometric survey of the structure and dynamics of the ∼100 most massive early-type galaxies within a distance of 108 Mpc. This survey probes a stellar mass range M∗ ≳ 1011.5 M⊙ and diverse galaxy environments that have not been systematically studied to date. Our wide-field IFS data cover about two effective radii of individual galaxies, and for a subset of them, we are acquiring additional IFS observations on sub-arcsecond scales with adaptive optics. We are also acquiring deep K-band imaging to trace the extended halos of the galaxies and measure accurate total magnitudes. Dynamical orbit modeling of the combined data will allow us to simultaneously determine the stellar, black hole, and dark matter halo masses. The primary goals of the project are to constrain the black hole scaling relations at high masses, investigate systematically the stellar initial mass function and dark matter distribution in massive galaxies, and probe the late-time assembly of ellipticals through stellar population and kinematical gradients. In this paper, we describe the MASSIVE sample selection, discuss the distinct demographics and structural and environmental properties of the selected galaxies, and provide an overview of our basic observational program, science goals and early survey results.}, -archivePrefix = {arXiv}, -arxivId = {1407.1054}, -author = {Ma, Chung Pei and Greene, Jenny E and McConnell, Nicholas and Janish, Ryan and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/795/2/158}, -eprint = {1407.1054}, -isbn = {0000000000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content,galaxies: structure}, -number = {2}, -pages = {158}, -pmid = {28562576}, -title = {{The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...795..158M}, -volume = {795}, -year = {2014} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani} and Caldwell, Nelson}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Lipnicky2018, -abstract = {We reportHI observations of eight spiral galaxies that are strongly lensing background sources. Our targets were selected from the Sloan WFC (Wide Field Camera) Edge-on Late-type Lens Survey (SWELLS) using the Arecibo, Karl G. Jansky Very Large Array, and Green Bank telescopes. We securely detect J1703+2451 at z = 0.063 with a signal-to-noise ratio of 6.7 and W50 = 79 ± 13 km s-1, obtaining the first detection of HI emission in a strong spiral lens. We measure a mass of MHI = (1.77 ± 0.06 -0.75+0.35) × 109M⊙ for this source. We find that this lens is a normal spiral, with observable properties that are fairly typical of spiral galaxies. For three other sources, we did not secure a detection; however, we are able to place strong constraints on the HI masses of those galaxies. The observations for four of our sources were rendered unusable due to strong radio frequency interference.}, -archivePrefix = {arXiv}, -arxivId = {1802.01588}, -author = {Lipnicky, Andrew and Chakrabarti, Sukanya and Wright, Melvyn C H and Blitz, Leo and Heiles, Carl and Cotton, William and Frayer, David and Blandford, Roger and Shu, Yiping and Bolton, Adam S}, -doi = {10.1093/mnras/sty326}, -eprint = {1802.01588}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Radio lines: galaxies}, -number = {3}, -pages = {3097--3105}, -title = {{The first detection of neutral hydrogen in emission in a strong spiral lens}}, -url = {http://arxiv.org/abs/1802.01588%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty326}, -volume = {476}, -year = {2018} -} -@article{Xie2015, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Wood2014, -abstract = {The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D and Hall, D J and Murray, N J and Gow, J P D and Holland, A and Turner, P and Burt, D}, -doi = {10.1088/1748-0221/9/12/C12028}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv,visible and ir photons (s}, -number = {12}, -pages = {C12028--------C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{Liao2016, -abstract = {The standard galaxy formation theory assumes that baryons and dark matter are initially well mixed before becoming segregated due to radiative cooling. We use non-radiative hydrodynamical simulations to explicitly examine this assumption and find that baryons and dark matter can also be segregated due to different characteristics of gas and dark matter during the buildup of the halo. As a result, baryons in many haloes do not originate from the same Lagrangian region as the dark matter. When using the fraction of corresponding dark matter and gas particles in the initial conditions (the 'paired fraction') as a proxy of the dark matter and gas segregation strength of a halo, on average about 25 per cent of the baryonic and dark matter of the final halo are segregated in the initial conditions. This is at odds with the assumption of the standard galaxy formation model. A consequence of this effect is that the baryons and dark matter of the same halo initially experience different tidal torques and thus their angular momentum vectors are often misaligned. The degree of the misalignment is largely preserved during later halo assembly and can be understood with the tidal torque theory. The result challenges the precision of some semi-analytical approaches that utilize dark matter halo merger trees to infer properties of gas associated with dark matter haloes.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.07592}, -author = {Liao, Shihong and Gao, Liang and Frenk, Carlos S. and Guo, Qi and Wang, Jie}, -doi = {10.1093/mnras/stx1391}, -eprint = {1610.07592}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Liao et al. - 2017 - The segregation of baryons and dark matter during halo assembly(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {2}, -pages = {2262--2269}, -title = {{The segregation of baryons and dark matter during halo assembly}}, -url = {http://arxiv.org/abs/1610.07592}, -volume = {470}, -year = {2017} -} -@article{Hezaveh2015, -abstract = {We examine the prospects of detecting demagnified images of gravitational lenses in observations of strongly lensed millimeter-wave molecular emission lines with ALMA. We model the lensing galaxies as a superposition of a dark matter component, a stellar component, and a central super-massive black hole (SMBH) and assess the detectability of the central images for a range of relevant parameters (e.g., stellar core, black hole mass, and source size). We find that over a large range of plausible parameters, future deep observations of lensed molecular lines with ALMA should enable the detection of the central images at ≳3 significance. We use a Fisher analysis to examine the constraints that could be placed on these parameters in various scenarios and find that for large stellar cores, both the core size and the mass of the central SMBHs can be accurately measured. We also study the prospects for detecting binary SMBHs with such observations and find that only under rare conditions and with very long integrations (∼40 hr) the masses of both SMBHs may be measured using the distortions of central images.}, -archivePrefix = {arXiv}, -arxivId = {1501.0175}, -author = {Hezaveh, Yashar D. and Marshall, Philip J. and Blandford, Roger D.}, -doi = {10.1088/2041-8205/799/2/L22}, -eprint = {1501.0175}, -issn = {20418213}, -journal = {ApJL}, -keywords = {Black hole physics,Galaxies: formation,Grfavitational lensing: strong}, -month = {feb}, -number = {2}, -pages = {1--5}, -title = {{Probing the inner kiloparsec of massive galaxies with strong gravitational lensing}}, -url = {http://arxiv.org/abs/1501.01757%5Cnhttp://stacks.iop.org/2041-8205/799/i=2/a=L22?key=crossref.afc1aafe0fcf1999390667157d5b7ef0}, -volume = {799}, -year = {2015} -} -@article{Gilman2020, -abstract = {The mass-concentration relation of dark matter haloes reflects the assembly history of objects in hierarchical structure formation scenarios and depends on fundamental quantities in cosmology such as the slope of the primordial matter power spectrum. This relation is unconstrained by observations on sub-galactic scales. We derive the first measurement of the mass-concentration relation using the image positions and flux ratios from 11 quadruple-image strong gravitational lenses (quads) in the mass range $10{6}-10{10} {, mathrm{M}_{odot }}$, assuming cold dark matter. We model both subhaloes and line-of-sight haloes, finite-size background sources, and marginalize over nuisance parameters describing the lens macromodel. We also marginalize over the logarithmic slope and redshift evolution of the mass-concentration relation, using flat priors that encompass the range of theoretical uncertainty in the literature. At z = 0, we constrain the concentration of $10{8} , mathrm{M}-{odot }$ haloes $c=12-{-5}{+6}$ at $68 {{ rm per cent}}$ CI, and $c=12-{-9}{+15}$ at $95 {{ rm per cent}}$ CI. For a $10{7} {, mathrm{M}-{odot }}$ halo, we obtain $68 {{ rm per cent}}$ ($95 {{ rm per cent}}$) constraints $c=15-{-8}{+9}$ ($c=15-{-11}{+18}$), while for $10{9} , mathrm{M}-{odot }$ haloes $c=10-{-4}{+7}$ ($c=10-{-7}{+14}$). These results are consistent with the theoretical predictions from mass-concentration relations in the literature and establish strong lensing by galaxies as a powerful probe of halo concentrations on sub-galactic scales across cosmological distance.}, -archivePrefix = {arXiv}, -arxivId = {1909.02573}, -author = {Gilman, Daniel and Du, Xiaolong and Benson, Andrew and Birrer, Simon and Nierenberg, Anna and Treu, Tommaso}, -doi = {10.1093/mnrasl/slz173}, -eprint = {1909.02573}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gilman et al. - 2020 - Constraints on the mass-concentration relation of cold dark matter haloes with 11 strong gravitational lenses.pdf:pdf}, -issn = {17453933}, -journal = {MNRAS Letters}, -keywords = {dark matter,galaxies: structure,gravitational lensing: strong,methods: statistical}, -number = {1}, -pages = {L12--L16}, -title = {{Constraints on the mass-concentration relation of cold dark matter haloes with 11 strong gravitational lenses}}, -volume = {492}, -year = {2020} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by a global driving force and a local positive feedback mechanism, which creates regular geometric and/or temporal patterns, and decreases the entropy locally, in contrast to random processes. Here we investigate for the first time a comprehensive number of (17) self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous “order out of randomness”, during the evolution from an initially disordered system to an ordered quasi-stationary system, mostly by quasi-periodic limit-cycle dynamics, but also by harmonic (mechanical or gyromagnetic) resonances. The global driving force can be due to gravity, electromagnetic forces, mechanical forces (e.g., rotation or differential rotation), thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational (Balbus-Hawley) instability, the convective (Rayleigh-B{\'{e}}nard) instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or a loss-cone instability. Physical models of astrophysical self-organization processes require hydrodynamic, magneto-hydrodynamic (MHD), plasma, or N-body simulations. Analytical formulations of self-organizing systems generally involve coupled differential equations with limit-cycle solutions of the Lotka-Volterra or Hopf-bifurcation type.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J. and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C.M. and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G. and Scargle, Jeffrey D. and Melatos, Andrew and Wagoner, Robert V. and Trimble, Virginia and Green, William H.}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Aschwanden et al. - 2018 - Order out of Randomness Self-Organization Processes in Astrophysics.pdf:pdf}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Wang2019, -abstract = {We study the evolutionary trend of the total density profile of early-type galaxies (ETGs) in IllustrisTNG. To this end, we trace ETGs from z = 0 to 4 and measure the power-law slope $\gamma$ ' of the total density profile for their main progenitors. We find that their slopes $\gamma$ ' steepen on average during z ∼ 4-2, then becoming shallower until z = 1, after which they remain almost constant, aside from a residual trend of becoming shallower towards z = 0. We also compare to a statistical sample of ETGs at different redshifts, selected based on their luminosity profiles and stellar masses. Due to different selection effects, the average slopes of the statistical samples follow a modified evolutionary trend. They monotonically decrease since z = 3, and after z ≈ 1, they remain nearly invariant with a mild increase towards z = 0. These evolutionary trends are mass dependent for both samples, with low-mass galaxies having in general steeper slopes than their more massive counterparts. Galaxies that transitioned to ETGs more recently have steeper mean slopes as they tend to be smaller and more compact at any given redshift. By analysing the impact of mergers and AGN feedback on the progenitors' evolution, we conjecture a multiphase path leading to isothermality in ETGs: dissipation associated with rapid wet mergers tends to steepen $\gamma$ ' from z = 4 to 2, whereas subsequent AGN feedback (especially in the kinetic mode) makes $\gamma$ ' shallower again from z = 2 to 1. Afterwards, passive evolution from z = 1 to 0, mainly through gas-poor mergers, mildly decreases $\gamma$ ' and maintains the overall mass distribution close to isothermal.}, -archivePrefix = {arXiv}, -arxivId = {1910.08552}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Shen, Xuejian and Mao, Shude and Barnes, David and Li, Hui and Marinacci, Federico and Torrey, Paul and Springel, Volker and Hernquist, Lars}, -doi = {10.1093/mnras/stz2907}, -eprint = {1910.08552}, -file = {:C\:/Users/Jammy/Documents/Papers/MassiveEllPaper/Wang2019IllustrisSlopeEvo.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: formation,Galaxies: structure,Galaxy: evolution,Methods: numerical}, -number = {4}, -pages = {5722--5738}, -title = {{Early-type galaxy density profiles from IllustrisTNG - II. Evolutionary trend of the total density profile}}, -volume = {490}, -year = {2019} -} -@article{astropy:2018, -author = {Price-Whelan, A.$\sim$M. and Sip\Hocz, B.$\sim$M. and G{\"{u}}nther, H.$\sim$M. and Lim, P.$\sim$L. and Crawford, S.$\sim$M. and Conseil, S and Shupe, D.$\sim$L. and Craig, M.$\sim$W. and Dencheva, N and Ginsburg, A and VanderPlas, J.$\sim$T. and Bradley, L.$\sim$D. and P{\'{e}}rez-Su{\'{a}}rez, D and de Val-Borro, M and {Paper Contributors}, (Primary and Aldcroft, T.$\sim$L. and Cruz, K.$\sim$L. and Robitaille, T.$\sim$P. and Tollerud, E.$\sim$J. and {Coordination Committee}, (Astropy and Ardelean, C and Babej, T and Bach, Y.$\sim$P. and Bachetti, M and Bakanov, A.$\sim$V. and Bamford, S.$\sim$P. and Barentsen, G and Barmby, P and Baumbach, A and Berry, K.$\sim$L. and Biscani, F and Boquien, M and Bostroem, K.$\sim$A. and Bouma, L.$\sim$G. and Brammer, G.$\sim$B. and Bray, E.$\sim$M. and Breytenbach, H and Buddelmeijer, H and Burke, D.$\sim$J. and Calderone, G and {Cano Rodr\'\iguez}, J.$\sim$L. and Cara, M and Cardoso, J.$\sim$V.$\sim$M. and Cheedella, S and Copin, Y and Corrales, L and Crichton, D and D\textquoterightAvella, D and Deil, C and Depagne, {\'{E}} and Dietrich, J.$\sim$P. and Donath, A and Droettboom, M and Earl, N and Erben, T and Fabbro, S and Ferreira, L.$\sim$A. and Finethy, T and Fox, R.$\sim$T. and Garrison, L.$\sim$H. and Gibbons, S.$\sim$L.$\sim$J. and Goldstein, D.$\sim$A. and Gommers, R and Greco, J.$\sim$P. and Greenfield, P and Groener, A.$\sim$M. and Grollier, F and Hagen, A and Hirst, P and Homeier, D and Horton, A.$\sim$J. and Hosseinzadeh, G and Hu, L and Hunkeler, J.$\sim$S. and Ivezi{\'{c}}, {\v{Z}} and Jain, A and Jenness, T and Kanarek, G and Kendrew, S and Kern, N.$\sim$S. and Kerzendorf, W.$\sim$E. and Khvalko, A and King, J and Kirkby, D and Kulkarni, A.$\sim$M. and Kumar, A and Lee, A and Lenz, D and Littlefair, S.$\sim$P. and Ma, Z and Macleod, D.$\sim$M. and Mastropietro, M and McCully, C and Montagnac, S and Morris, B.$\sim$M. and Mueller, M and Mumford, S.$\sim$J. and Muna, D and Murphy, N.$\sim$A. and Nelson, S and Nguyen, G.$\sim$H. and Ninan, J.$\sim$P. and N{\"{o}}the, M and Ogaz, S and Oh, S and Parejko, J.$\sim$K. and Parley, N and Pascual, S and Patil, R and Patil, A.$\sim$A. and Plunkett, A.$\sim$L. and Prochaska, J.$\sim$X. and Rastogi, T and {Reddy Janga}, V and Sabater, J and Sakurikar, P and Seifert, M and Sherbert, L.$\sim$E. and Sherwood-Taylor, H and Shih, A.$\sim$Y. and Sick, J and Silbiger, M.$\sim$T. and Singanamalla, S and Singer, L.$\sim$P. and Sladen, P.$\sim$H. and Sooley, K.$\sim$A. and Sornarajah, S and Streicher, O and Teuben, P and Thomas, S.$\sim$W. and Tremblay, G.$\sim$R. and Turner, J.$\sim$E.$\sim$H. and Terr{\'{o}}n, V and van Kerkwijk, M.$\sim$H. and de la Vega, A and Watkins, L.$\sim$L. and Weaver, B.$\sim$A. and Whitmore, J.$\sim$B. and Woillez, J and Zabalza, V and Contributors, (Astropy}, -doi = {10.3847/1538-3881/aabc4f}, -journal = {AJ}, -keywords = {Astrophysics - Instrumentation and Methods for As,methods: data analysis,methods: miscellaneous,methods: statistical,reference systems}, -month = {sep}, -pages = {123}, -title = {{The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package}}, -volume = {156}, -year = {2018} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S$\backslash$'{\{}e{\}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as {\$}M{\_}{\{}h{\}}(M{\_}{\{}*{\}}) \backslashpropto r{\_}{\{}\backslashmathrm{\{}eff{\}}{\}}{\^{}}{\{}\backslasheta{\}}(M{\_}{\{}*{\}}){\$}. We find that on average, our lens galaxies have an {\$}\backslasheta = 0.42\backslashpm0.12{\$}, i.e. larger galaxies live in more massive dark matter haloes. The {\$}\backslasheta{\$} is strongest for high mass luminous red galaxies (LRGs). Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed {\$}M{\_}{\{}*{\}}{\$}, satellite galaxies have a larger {\$}\backslasheta{\$} and greater scatter in the {\$}M{\_}{\{}\backslashmathrm{\{}h{\}}{\}}{\$} and {\$}r{\_}{\{}\backslashmathrm{\{}eff{\}}{\}}{\$} relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J L and Hudson, Michael J and Balogh, Michael L and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Gavazzi2012, -abstract = {We study the relative alignment of mass and light in a sample of 16 massive early-type galaxies at z = 0.2-0.9 that act as strong gravitational lenses. The sample was identified from deep multi-band images obtained as part of the Canada-France-Hawaii Telescope Legacy Survey and as part of the Strong Lensing Legacy Survey (SL2S). Higher resolution follow-up imaging is available for a subset of 10 systems. We construct gravitational lens models and infer total enclosed mass, elongation, and position angle of the mass distribution. By comparison with the observed distribution of light we infer that there is a substantial amount of external shear with mean value 〈$\gamma$ ext〉 = 0.12 ± 0.05, arising most likely from the environment of the SL2S lenses. In a companion paper, we combine these measurements with follow-up Keck spectroscopy to study the evolution of the stellar and dark matter content of early-type galaxies as a function of cosmic time. {\textcopyright} 2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1202.3852}, -author = {Gavazzi, Rapha{\"{e}}l and Treu, Tommaso and Marshall, Philip J. and Brault, Florence and Ruff, Andrea}, -doi = {10.1088/0004-637X/761/2/170}, -eprint = {1202.3852}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: fundamental parameters,gravitational lensing: strong}, -number = {2}, -pages = {170}, -title = {{The SL2S galaxy-scale gravitational lens sample. I. the alignment of mass and light in massive early-type galaxies at z = 0.2-0.9}}, -url = {http://arxiv.org/abs/1202.3852}, -volume = {761}, -year = {2012} -} -@article{Moore2018, -abstract = {The next generation of giant-segmented mirror telescopes ({\textgreater}20 m) will enable us to observe galactic nuclei at much higher angular resolution and sensitivity than ever before. These capabilities will introduce a revolutionary shift in our understanding of the origin and evolution of supermassive black holes by enabling more precise black hole mass measurements in a mass range that is unreachable today. We present simulations and predictions of the observations of nuclei that will be made with the Thirty Meter Telescope (TMT) and the adaptive optics assisted integral-field spectrograph IRIS, which is capable of diffraction-limited spectroscopy from Z band (0.9 $\mu$m) to K band (2.2 $\mu$m). These simulations, for the first time, use realistic values for the sky, telescope, adaptive optics system, and instrument to determine the expected signal-to-noise ratio of a range of possible targets spanning intermediate mass black holes of 104 M⊙to the most massive black holes known today of {\textgreater}1010 M ⊙. We find that IRIS will be able to observe Milky Way mass black holes out the distance of the Virgo Cluster, and will allow us to observe many more of the brightest cluster galaxies where the most massive black holes are thought to reside. We also evaluate how well the kinematic moments of the velocity distributions can be constrained at the different spectral resolutions and plate scales designed for IRIS. We find that a spectral resolution of 8000 will be necessary to measure the masses of intermediate mass black holes. By simulating the observations of galaxies found in Sloan Digital Sky Survey DR7, we find that over 105 massive black holes will be observable at distances between 0.005 {\textless} z {\textless} 0.18 with the estimated sensitivity and angular resolution provided by access to Z-band (0.9 $\mu$m) spectroscopy from IRIS and the TMT adaptive optics system. These observations will provide the most accurate dynamical measurements of black hole masses to enable the study of the demography of massive black holes, address the origin of the M BH-$\sigma$ and M BH-L relationships, and evolution of black holes through cosmic time. {\textcopyright}2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1401.7988}, -author = {Do, Tuan and Wright, Shelley A and Barth, Aaron J and Barton, Elizabeth J and Simard, Luc and Larkin, James E and Moore, Anna M and Wang, Lianqi and Ellerbroek, Brent}, -doi = {10.1088/0004-6256/147/4/93}, -eprint = {1401.7988}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {adaptive opticsinstrumentation,galaxies,imaging spectroscopytelescopes,kinematics and dynamicsinstrumentation,spectrographstechniques}, -number = {4}, -pages = {1--19}, -title = {{Prospects for measuring supermassive black hole masses with future extremely large telescopes}}, -volume = {147}, -year = {2014} -} -@article{Ravasi2019, -abstract = {Linear operators and optimisation are at the core of many algorithms used in signal and image processing, remote sensing, and inverse problems. For small to medium-scale problems, existing software packages (e.g., MATLAB, Python numpy and scipy) allow for explicitly building dense (or sparse) matrices and performing algebraic operations (e.g., computation of matrix-vector products and manipulation of matrices) with syntax that closely represents their corresponding analytical forms. However, many real application, large-scale operators do not lend themselves to explicit matrix representations, usually forcing practitioners to forego of the convenient linear-algebra syntax available for their explicit-matrix counterparts. PyLops is an open-source Python library providing a flexible and scalable framework for the creation and combination of so-called linear operators, class-based entities that represent matrices and inherit their associated syntax convenience, but do not rely on the creation of explicit matrices. We show that PyLops operators can dramatically reduce the memory load and CPU computations compared to explicit-matrix calculations, while still allowing users to seamlessly use their existing knowledge of compact matrix-based syntax that scales to any problem size because no explicit matrices are required.}, -archivePrefix = {arXiv}, -arxivId = {1907.12349}, -author = {Ravasi, Matteo and Vasconcelos, Ivan}, -eprint = {1907.12349}, -journal = {Software X}, -number = {100361}, -title = {{PyLops -- A Linear-Operator Python Library for large scale optimization}}, -url = {https://doi.org/10.1016/j.softx.2019.100361}, -volume = {11}, -year = {2019} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by a global driving force and a local positive feedback mechanism, which creates regular geometric and/or temporal patterns, and decreases the entropy locally, in contrast to random processes. Here we investigate for the first time a comprehensive number of (17) self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous “order out of randomness”, during the evolution from an initially disordered system to an ordered quasi-stationary system, mostly by quasi-periodic limit-cycle dynamics, but also by harmonic (mechanical or gyromagnetic) resonances. The global driving force can be due to gravity, electromagnetic forces, mechanical forces (e.g., rotation or differential rotation), thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational (Balbus-Hawley) instability, the convective (Rayleigh-B{\'{e}}nard) instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or a loss-cone instability. Physical models of astrophysical self-organization processes require hydrodynamic, magneto-hydrodynamic (MHD), plasma, or N-body simulations. Analytical formulations of self-organizing systems generally involve coupled differential equations with limit-cycle solutions of the Lotka-Volterra or Hopf-bifurcation type.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C M and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G and Scargle, Jeffrey D and Melatos, Andrew and Wagoner, Robert V and Trimble, Virginia and Green, William H}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9602085}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{Seabroke2011, -abstract = {Gaia will only achieve its unprecedented measurement accuracy {\$}\backslash{\$}nrequirements with detailed calibration and correction for radiation{\$}\backslash{\$}ndamage. We present our Silvaco 3D engineering software model of the Gaia{\$}\backslash{\$}nCCD pixel and two of its applications for Gaia: (1) physically{\$}\backslash{\$}ninterpreting supplementary buried channel (SBC) capacity measurements{\$}\backslash{\$}n(pocket-pumping and first pixel response) in terms of e2v manufacturing{\$}\backslash{\$}ndoping alignment tolerances; and (2) deriving electron densities within{\$}\backslash{\$}na charge packet as a function of the number of constituent electrons and{\$}\backslash{\$}n3D position within the charge packet as input to microscopic models{\$}\backslash{\$}nbeing developed to simulate radiation damage.}, -archivePrefix = {arXiv}, -arxivId = {1009.2431}, -author = {Seabroke, G M and Prod'homme, T and Hopkinson, G and Burt, D and Robbins, M and Holland, A}, -doi = {10.1051/eas/1045077}, -eprint = {1009.2431}, -isbn = {1633-4760}, -issn = {1633-4760}, -journal = {EAS Publications Series}, -pages = {433--436}, -title = {{Modelling Gaia CCD pixels with Silvaco 3D engineering software}}, -url = {http://www.eas-journal.org/10.1051/eas/1045077}, -volume = {45}, -year = {2010} -} -@article{Toomre1972, -abstract = {Abstract image available at: http://adsabs.harvard.edu/abs/1972ApJ...178..623T}, -author = {Toomre, Alar and Toomre, Juri}, -doi = {10.1086/151823}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {dec}, -pages = {623}, -pmid = {14680119}, -title = {{Galactic Bridges and Tails}}, -url = {http://adsabs.harvard.edu/doi/10.1086/151823}, -volume = {178}, -year = {1972} -} -@article{Xu2014, -abstract = {Discrepancies between the observed and model-predicted radio flux ratios are seen in a number of quadruply-lensed quasars. The most favoured interpretation of these anomalies is that cold dark matter (CDM) substructures present in lensing galaxies perturb the lens potentials and alter image magnifications and thus flux ratios. So far no consensus has emerged regarding whether or not the predicted CDM substructure abundance fully accounts for the lensing flux anomaly observations. Accurate modelling relies on a realistic lens sample in terms of both the lens environment and internal structures and substructures. In this paper, we construct samples of generalized and specific lens potentials, to which we add (rescaled) subhalo populations from the galaxy-scale Aquarius and the cluster-scale Phoenix simulation suites. We further investigate the lensing effects from subhaloes of masses several orders of magnitude below the simulation resolution limit. The resulting flux-ratio distributions are compared to the currently best available sample of radio lenses. The observed anomalies in B0128+437, B0712+472 and B1555+375 are more likely to be caused by propagation effects or oversimplified/improper lens modelling, signs of which are already seen in the data. Among the quadruple systems that have closely located image triplets/pairs, the anomalous flux ratios ofMG0414+0534 can be reproduced by adding CDM subhaloes to its macroscopic lens potential, with a probability of 5-20 per cent; for B0712+472, B1422+231, B1555+375 and B2045+265, these probabilities are only of a fewper cent. We hence find that CDM substructures are unlikely to be the whole reason for radio flux anomalies. We discuss other possible effects that might also be at work.}, -archivePrefix = {arXiv}, -arxivId = {1410.3282}, -author = {Xu, Dandan and Sluse, Dominique and Gao, Liang and Wang, Jie and Frenk, Carlos and Mao, Shude and Schneider, Peter and Springel, Volker}, -doi = {10.1093/mnras/stu2673}, -eprint = {1410.3282}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {4}, -pages = {3189--3206}, -title = {{How well can cold dark matter substructures account for the observed radio flux-ratio anomalies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2013arXiv1307.4220X&link_type=ABSTRACT%5Cnpapers://dcc533b5-8613-47b7-b88c-2b0c0d39c33f/Paper/p4964}, -volume = {447}, -year = {2015} -} -@article{Falco1985, -abstract = {The images of a background source formed by a foreground mass \ndistribution in a matter-dominated Friedmann cosmology are considered. A \ntransformation is presented that leaves unchanged the image observables, \nincluding positions, relative magnifications, apparent luminosities, and \ndifferences in propagation times associated with image pairs. The \nobservables are related to the parameters of the source and of a \ngeneralized lens model. The transformation is applied to these relations \nto scale the value of H(0) and to modify the mass distribution of the \nlens and move the position of the source. One lens model for Q0957 + 561 }, -author = {Falco, E. E. and Gorenstein, M. V. and Shapiro, I. I.}, -doi = {10.1086/184422}, -isbn = {9781416033431}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {ASTRONOMICAL MODELS,Background Radiation,GALACTIC CLUSTERS,Geometrical Optics,Gravitational Lenses,Hubble Diagram,MASS DISTRIBUTION,Quasars,Radiation Sources}, -pages = {L1}, -title = {{On model-dependent bounds on H(0) from gravitational images Application of Q0957 + 561A,B}}, -url = {http://adsabs.harvard.edu/doi/10.1086/184422}, -volume = {289}, -year = {1985} -} -@article{Saito2016, -abstract = {We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) 'CMASS' sample at z {\$\sim${}} 0.5. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogues which include selection effects, reproduce the overall SMF, the projected two-point correlation function wp, the CMASS dn/dz, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of 'age matching' and show that these effects are markedly different compared to the ones explored by Hearin et al. at lower stellar masses. We construct two models, one in which galaxy colour is stochastic ('AbM' model) as well as a model which contains assembly bias effects ('AgM' model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colours are not a stochastic process in high-mass haloes. Our results suggest that the colours of galaxies in high-mass haloes are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.}, -archivePrefix = {arXiv}, -arxivId = {1509.00482}, -author = {Saito, Shun and Leauthaud, Alexie and Hearin, Andrew P and Bundy, Kevin and Zentner, Andrew R and Behroozi, Peter S and Reid, Beth A and Sinha, Manodeep and Coupon, Jean and Tinker, Jeremy L and White, Martin and Schneider, Donald P}, -doi = {10.1093/mnras/stw1080}, -eprint = {1509.00482}, -isbn = {978-972-40-3722-6}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Large-scale structure of Universe}, -number = {2}, -pages = {1457--1475}, -title = {{Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?}}, -volume = {460}, -year = {2016} -} -@article{Jin2018, -abstract = {We present a “super-deblended” far-infrared (FIR) to (sub)millimeter photometric catalog in the Cosmic Evolution Survey (COSMOS), prepared with the method recently developed by Liu et al., with key adaptations. We obtain point-spread function fitting photometry at fixed prior positions including 88,008 galaxies detected in VLA 1.4, 3 GHz, and/or MIPS 24 $\mu$ m images. By adding a specifically carved mass-selected sample (with an evolving stellar mass limit), a highly complete prior sample of 194,428 galaxies is achieved for deblending FIR/(sub)mm images. We performed “active” removal of nonrelevant priors at FIR/(sub)mm bands using spectral energy distribution fitting and redshift information. In order to cope with the shallower COSMOS data, we subtract from the maps the flux of faint nonfitted priors and explicitly account for the uncertainty of this step. The resulting photometry (including data from Spitzer , Herschel , SCUBA2, AzTEC, MAMBO, and NSF's Karl G. Jansky Very Large Array at 3 and 1.4 GHz) displays well-behaved quasi-Gaussian uncertainties calibrated from Monte Carlo simulations and tailored to observables (crowding, residual maps). Comparison to ALMA photometry for hundreds of sources provides a remarkable validation of the technique. We detect 11,220 galaxies over the 100–1200 $\mu$ m range extending to z phot ∼ 7. We conservatively selected a sample of 85 z > 4 high-redshift candidates significantly detected in the FIR/(sub)mm, often with secure radio and/or Spitzer /IRAC counterparts. This provides a chance to investigate the first generation of vigorous starburst galaxies (SFRs ∼ 1000 M ⊙ yr −1 ). The photometric and value-added catalogs are publicly released.}, -archivePrefix = {arXiv}, -arxivId = {1807.04697}, -author = {Jin, Shuowen and Daddi, Emanuele and Liu, Daizhong and Smol{\v{c}}i{\'{c}}, Vernesa and Schinnerer, Eva and Calabr{\`{o}}, Antonello and Gu, Qiusheng and Delhaize, Jacinta and Delvecchio, Ivan and Gao, Yu and Salvato, Mara and Puglisi, Annagrazia and Dickinson, Mark and Bertoldi, Frank and Sargent, Mark and Novak, Mladen and Magdis, Georgios and Aretxaga, Itziar and Wilson, Grant W. and Capak, Peter}, -doi = {10.3847/1538-4357/aad4af}, -eprint = {1807.04697}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Jin2018DustRandomLens.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -number = {1}, -pages = {56}, -title = {{“Super-deblended” Dust Emission in Galaxies. II. Far-IR to (Sub)millimeter Photometry and High-redshift Galaxy Candidates in the Full COSMOS Field}}, -volume = {864}, -year = {2018} -} -@article{Pillepich2017, -abstract = {We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multi-mode feedback. In this paper we give a comprehensive description of the physical and numerical advances which form the core of the IllustrisTNG (The Next Generation) framework. We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content, and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black hole driven kinetic feedback at low accretion rates, magnetohydrodynamics, and improvements to the numerical scheme. Using a suite of (25 Mpc {\$}h{\^{}}{\{}-1{\}}{\$}){\$}{\^{}}3{\$} cosmological boxes we assess the outcome of the new model at our fiducial resolution. The presence of a self-consistently amplified magnetic field is shown to have an important impact on the stellar content of {\$}10{\^{}}{\{}12{\}} M{\_}{\{}\backslashbackslashrm sun{\}}{\$} haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low mass end of the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {1703.02970}, -author = {Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R{\"{u}}diger and Hernquist, Lars and Torrey, Paul and Vogelsberger, Mark and Weinberger, Rainer and Marinacci, Federico}, -doi = {10.1093/mnras/stx2656}, -eprint = {1703.02970}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {4077--4106}, -title = {{Simulating galaxy formation with the IllustrisTNG model}}, -url = {http://arxiv.org/abs/1703.02970%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx2656}, -volume = {473}, -year = {2018} -} -@article{Mendez-Abreu2016, -abstract = {We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area data release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log (M∗/MȮ) {\textgreater} 11), the galaxy population is dominated by galaxies modelled with a single S{\'{e}}rsic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T {\textgreater} 0.2. At intermediate masses (9.5 {\textless} log (M∗/MȮ) {\textless} 11), galaxies described with bulge+disc but B/T {\textless} 0.2 are preponderant, whereas, at the low mass end (log (M∗/MȮ) {\textless} 9.5), the prevailing population is constituted by galaxies modelled with either purediscs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57{\%} of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5 {\textless} log (M∗/MȮ) {\textless} 11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62{\%}, 28{\%}, and 10{\%} for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.}, -archivePrefix = {arXiv}, -arxivId = {1610.05324}, -author = {M{\'{e}}ndez-Abreu, J and Ruiz-Lara, T and S{\'{a}}nchez-Menguiano, L and {De Lorenzo-C{\'{a}}ceres}, A and Costantin, L and Catal{\'{a}}n-Torrecilla, C and Florido, E and Aguerri, J A L and Bland-Hawthorn, J and Corsini, E M and Dettmar, R J and Galbany, L and Garc{\'{i}}a-Benito, R and Marino, R A and M{\'{a}}rquez, I and Ortega-Minakata, R A and Papaderos, P and S{\'{a}}nchez, S F and S{\'{a}}nchez-Blazquez, P and Spekkens, K and {Van De Ven}, G and Wild, V and Ziegler, B}, -doi = {10.1051/0004-6361/201629525}, -eprint = {1610.05324}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -title = {{Two-dimensional multi-component photometric decomposition of CALIFA galaxies}}, -url = {http://arxiv.org/abs/1610.05324%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201629525}, -volume = {598}, -year = {2017} -} -@article{Bullock:2005aa, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted $\sim$100-200 luminous satellite galaxies in the past \$\sim$12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ($\sim$80%) coming from the \$\sim$15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of $\sim$9 Gyr in the past, while surviving satellite systems have median accretion times of $\sim$5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S. and Johnston, Kathryn V.}, -doi = {10.1086/497422}, -eprint = {0506467}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bullock, Johnston - 2005 - Tracing Galaxy Formation with Stellar Halos. I. Methods.pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {dec}, -number = {2}, -pages = {931--949}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Furlong2017, -abstract = {We present the evolution of galaxy sizes, from redshift 2 to 0, for actively star forming and passive galaxies in the cosmological hydrodynamical 1003 cMpc3 simulation of the EAGLE project. We find that the sizes increase with stellar mass, but that the relation weakens with increasing redshift. Separating galaxies by their star formation activity, we find that passive galaxies are typically smaller than active galaxies at a fixed stellar mass. These trends are consistent with those found in observations and the level of agreement between the predicted and observed size-mass relations is of the order of 0.1 dex for z < 1 and 0.2-0.3 dex from redshift 1 to 2. We use the simulation to compare the evolution of individual galaxies with that of the population as a whole. While the evolution of the size-stellar mass relation for active galaxies provides a good proxy for the evolution of individual galaxies, the evolution of individual passive galaxies is not well represented by the observed size-mass relation due to the evolving number density of passive galaxies. Observations of z $\sim$ 2 galaxies have revealed an abundance of massive red compact galaxies, which depletes below z $\sim$ 1. We find that a similar population forms naturally in the simulation. Comparing these galaxies with their z = 0 descendants, we find that all compact galaxies grow in size due to the high-redshift stars migrating outwards. Approximately 60 per cent of the compact galaxies increase in size further due to renewed star formation and/or mergers.}, -archivePrefix = {arXiv}, -arxivId = {1510.05645}, -author = {Furlong, M. and Bower, R. G. and Crain, R. A. and Schaye, J. and Theuns, T. and Trayford, J. W. and Qu, Y. and Schaller, M. and Berthet, M. and Helly, J. C.}, -doi = {10.1093/mnras/stw2740}, -eprint = {1510.05645}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Furlong et al. - 2017 - Size evolution of normal and compact galaxies in the EAGLE simulation(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: star formation,Galaxies: structure}, -number = {1}, -pages = {722--738}, -title = {{Size evolution of normal and compact galaxies in the EAGLE simulation}}, -volume = {465}, -year = {2017} -} -@article{Devour2017, -abstract = {Accurate measurement of galaxy structures is a prerequisite for quantitative investigation of galaxy properties or evolution. Yet, the impact of galaxy inclination and dust on commonly used metrics of galaxy structure is poorly quantified. We use infrared data sets to select inclination-independent samples of disc and flattened elliptical galaxies. These samples show strong variation in S{\$}\backslash{\$}'{\{}e{\}}rsic index, concentration, and half-light radii with inclination. We develop novel inclination-independent galaxy structures by collapsing the light distribution in the near-infrared on to the major axis, yielding inclination-independent `linear' measures of size and concentration. With these new metrics we select a sample of Milky Way analogue galaxies with similar stellar masses, star formation rates, sizes and concentrations. Optical luminosities, light distributions, and spectral properties are all found to vary strongly with inclination: When inclining to edge-on, {\$}r{\$}-band luminosities dim by {\$}{\textgreater}{\$}1 magnitude, sizes decrease by a factor of 2, `dust-corrected' estimates of star formation rate drop threefold, metallicities decrease by 0.1 dex, and edge-on galaxies are half as likely to be classified as star forming. These systematic effects should be accounted for in analyses of galaxy properties.}, -archivePrefix = {arXiv}, -arxivId = {1702.06528}, -author = {Devour, Brian and Bell, Eric}, -doi = {10.1093/mnrasl/slx021}, -eprint = {1702.06528}, -issn = {1745-3925}, -journal = {Mnras}, -keywords = {dust,extinction,galaxies,general,photometric,techniques}, -number = {February}, -pages = {1--5}, -pmid = {18462818}, -title = {{Revealing strong bias in common measures of galaxy properties using new inclination-independent structures}}, -url = {http://arxiv.org/abs/1702.06528%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnrasl/slx021}, -volume = {000}, -year = {2017} -} -@techreport{Biretta1997, -author = {Biretta, John and Mutchler, Max}, -booktitle = {Space Telescope WFPC2 Instrument Science Report}, -keywords = {HST,Hubble Space Telescope,Space Telescope Science Institute,WFC3,Wide Field Camera 3}, -month = {may}, -pages = {1--11}, -title = {{Charge Trapping and CTE Residual Images in the WFPC2 CCDs}}, -year = {1998} -} -@article{Carpenter2017, -abstract = {Stan is a probabilistic programming language for specifying statistical models. A Stan program imperatively defines a log probability function over parameters conditioned on specified data and constants. As of version 2.14.0, Stan provides full Bayesian inference for continuous-variable models through Markov chain Monte Carlo methods such as the No-U-Turn sampler, an adaptive form of Hamiltonian Monte Carlo sampling. Penalized maximum likelihood estimates are calculated using optimization methods such as the limited memory Broyden-Fletcher-Goldfarb-Shanno algorithm. Stan is also a platform for computing log densities and their gradients and Hessians, which can be used in alternative algorithms such as variational Bayes, expectation propagation, and marginal inference using approximate integration. To this end, Stan is set up so that the densities, gradients, and Hessians, along with intermediate quantities of the algorithm such as acceptance probabilities, are easily accessible. Stan can be called from the command line using the cmdstan package, through R using the rstan package, and through Python using the pystan package. All three interfaces support sampling and optimization-based inference with diagnostics and posterior analysis. rstan and pystan also provide access to log probabilities, gradients, Hessians, parameter transforms, and specialized plotting.}, -author = {Carpenter, Bob and Gelman, Andrew and Hoffman, Matthew D. and Lee, Daniel and Goodrich, Ben and Betancourt, Michael and Brubaker, Marcus A. and Guo, Jiqiang and Li, Peter and Riddell, Allen}, -doi = {10.18637/jss.v076.i01}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Carpenter et al. - 2017 - Stan A probabilistic programming language.pdf:pdf}, -issn = {15487660}, -journal = {Journal of Statistical Software}, -keywords = {Algorithmic differentiation,Bayesian inference,Probabilistic program,Stan}, -number = {1}, -title = {{Stan: A probabilistic programming language}}, -volume = {76}, -year = {2017} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Brownstein2012, -abstract = {We present a catalog of 25 definite and 11 probable strong galaxy-galaxy gravitational lens systems with lens redshifts 0.4 ≲ z ≲ 0.7, discovered spectroscopically by the presence of higher-redshift emission lines within the Baryon Oscillation Spectroscopic Survey (BOSS) of luminous galaxies, and confirmed with high-resolution Hubble Space Telescope (HST) images of 44 candidates. Our survey extends the methodology of the Sloan Lens Advanced Camera for Surveys survey (SLACS) to higher redshift. We describe the details of the BOSS spectroscopic candidate detections, our HST ACS image processing and analysis methods, and our strong gravitational lens modeling procedure. We report BOSS spectroscopic parameters and ACS photometric parameters for all candidates, and mass-distribution parameters for the best-fit singular isothermal ellipsoid models of definite lenses. Our sample to date was selected using only the first six months of BOSS survey-quality spectroscopic data. The full five-year BOSS database should produce a sample of several hundred strong galaxy-galaxy lenses and in combination with SLACS lenses at lower redshift, strongly constrain the redshift evolution of the structure of elliptical, bulge-dominated galaxies as a function of luminosity, stellar mass, and rest-frame color, thereby providing a powerful test for competing theories of galaxy formation and evolution.}, -archivePrefix = {arXiv}, -arxivId = {1112.3683}, -author = {Brownstein, Joel R. and Bolton, Adam S. and Schlegel, David J. and Eisenstein, Daniel J. and Kochanek, Christopher S. and Connolly, Natalia and Maraston, Claudia and Pandey, Parul and Seitz, Stella and Wake, David A. and Wood-Vasey, W. Michael and Brinkmann, Jon and Schneider, Donald P. and Weaver, Benjamin A.}, -doi = {10.1088/0004-637X/744/1/41}, -eprint = {1112.3683}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: distances and redshifts,galaxies: evolution,galaxies: high-redshift,gravitational lensing: strong,large-scale structure of universe,surveys}, -number = {1}, -pages = {41}, -title = {{The boss emission-line lens survey (Bells). I. A large spectroscopically selected sample of lens galaxies at redshift 0.5}}, -url = {http://stacks.iop.org/0004-637X/744/i=1/a=41?key=crossref.048b7a8362da2c6d3c9b5c518d91756c}, -volume = {744}, -year = {2012} -} -@article{Duffy2010, -abstract = {The back-reaction of baryons on the dark matter halo density profile is of great interest, not least because it is an important systematic uncertainty when attempting to detect the dark matter. Here, we draw on a large suite of high-resolution cosmological hydrodynamical simulations to systematically investigate this process and its dependence on the baryonic physics associated with galaxy formation. The effects of baryons on the dark matter distribution are typically not well described by adiabatic contraction models. In the inner 10 per cent of the virial radius the models are only successful if we allow their parameters to vary with baryonic physics, halo mass and redshift, thereby removing all predictive power. On larger scales the profiles from dark matter only simulations consistently provide better fits than adiabatic contraction models, even when we allow the parameters of the latter models to vary. The inclusion of baryons results in significantly more concentrated density profiles if radiative cooling is efficient and feedback is weak. The dark matter halo concentration can in that case increase by as much as 30 (10) per cent on galaxy (cluster) scales. The most significant effects occur in galaxies at high redshift, where there is a strong anticorrelation between the baryon fraction in the halo centre and the inner slope of both the total and the dark matter density profiles. If feedback is weak, isothermal inner profiles form, in agreement with observations of massive, early-type galaxies. However, we find that active galactic nuclei (AGN) feedback, or extremely efficient feedback from massive stars, is necessary to match observed stellar fractions in groups and clusters, as well as to keep the maximum circular velocity similar to the virial velocity as observed for disc galaxies. These strong feedback models reduce the baryon fraction in galaxies by a factor of 3 relative to the case with no feedback. The AGN is even capable of reducing the baryon fraction by a factor of 2 in the inner region of group and cluster haloes. This in turn results in inner density profiles which are typically shallower than isothermal and the halo concentrations tend to be lower than in the absence of baryons. We therefore conclude that the disagreement between the concentrations inferred from observations of groups of galaxies and predictions from simulations that was identified by Duffy et al. is not alleviated by the inclusion of baryons. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1001.3447}, -author = {Duffy, Alan R. and Schaye, Joop and Kay, Scott T. and Vecchia, Claudio Dalla and Battye, Richard A. and Booth, C. M.}, -doi = {10.1111/j.1365-2966.2010.16613.x}, -eprint = {1001.3447}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Gravitation,Hydrodynamics,Methods: numerical}, -month = {jul}, -number = {4}, -pages = {2161--2178}, -title = {{Impact of baryon physics on dark matter structures: A detailed simulation study of halo density profiles}}, -volume = {405}, -year = {2010} -} -@article{Dekel2009b, -abstract = {The massive galaxies in the young universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids (Genzel et al. 2006, 2008). Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are stream-fed galaxies, formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes (Dekel {\&} Birnboim 2006; Keres et al. 2005). A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duy cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid (Noguchi 1999; Genzel et al. 2008, Elmegreen, Bournaud {\&} Elmegreen 2008, Dekel, Sari {\&} Ceverino 2009). This stream-driven scenario for the formation of disks and spheroids is an alternative to the merger picture.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {https://ui.adsabs.harvard.edu/%7B%5C#%7Dabs/2009Natur.457..451D/abstract}, -volume = {457}, -year = {2009} -} -@article{Pub---ae2019, -abstract = {Strong-gravitational lens systems with quadruply imaged quasars (quads) are unique probes to address several fundamental problems in cosmology and astrophysics. Although they are intrinsically very rare, ongoing and planned wide-field deep-sky surveys are set to discover thousands of such systems in the next decade. It is thus paramount to devise a general framework to model strong-lens systems to cope with this large influx without being limited by expert investigator time. We propose such a general modelling framework (implemented with the publicly available software lenstronomy) and apply it to uniformly model three-band Hubble Space Telescope Wide Field Camera 3 images of 13 quads. This is the largest uniformly modelled sample of quads to date and paves the way for a variety of studies. To illustrate the scientific content of the sample, we investigate the alignment between the mass and light distribution in the deflectors. The position angles of these distributions are well-aligned, except when there is strong external shear. However, we find no correlation between the ellipticity of the light and mass distributions. We also show that the observed flux-ratios between the images depart significantly from the predictions of simple smooth models. The departures are strongest in the bluest band, consistent with microlensing being the dominant cause in addition to millilensing. Future papers will exploit this rich data set in combination with ground-based spectroscopy and time delays to determine quantities such as the Hubble constant, the free streaming length of dark matter, and the normalization of the initial stellar mass function.}, -archivePrefix = {arXiv}, -arxivId = {1807.09278}, -author = {Shajib, A J and Birrer, S and Treu, T and Auger, M W and Agnello, A and Anguita, T and Buckley-Geer, E J and Chan, J H H and Collett, T E and Courbin, F and Fassnacht, C D and Frieman, J and Kayo, I and Lemon, C and Lin, H and Marshall, P J and McMahon, R and More, A and Morgan, N D and Motta, V and Oguri, M and Ostrovski, F and Rusu, C E and Schechter, P L and Shanks, T and Suyu, S H and Meylan, G and Abbott, T M C and Allam, S and Annis, J and Avila, S and Bertin, E and Brooks, D and {Carnero Rosell}, A and {Carrasco Kind}, M and Carretero, J and Cunha, C E and {Da Costa}, L N and {De Vicente}, J and Desai, S and Doel, P and Flaugher, B and Fosalba, P and Garc{\'{i}}a-Bellido, J and Gerdes, D W and Gruen, D and Gruendl, R A and Gutierrez, G and Hartley, W G and Hollowood, D L and Hoyle, B and James, D J and Kuehn, K and Kuropatkin, N and Lahav, O and Lima, M and Maia, M A G and March, M and Marshall, J L and Melchior, P and Menanteau, F and Miquel, R and Plazas, A A and Sanchez, E and Scarpine, V and Sevilla-Noarbe, I and Smith, M and Soares-Santos, M and Sobreira, F and Suchyta, E and Swanson, M E C and Tarle, G and Walker, A R}, -doi = {10.1093/mnras/sty3397}, -eprint = {1807.09278}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: structure,gravitational lensing: strong,methods: data analysis}, -number = {4}, -pages = {5649--5671}, -title = {{Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 13 quadruply+ imaged quasars}}, -volume = {483}, -year = {2019} -} -@article{Sales2012, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {jun}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum {\$}j{\_}\backslashbackslashstar{\{}\backslash{\$}{\}} and the stellar mass {\$}M{\_}\backslashbackslashstar{\{}\backslash{\$}{\}} in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction {\$}f{\_}{\{}\backslashbackslashrm inf{\}}{\$} of baryons that infall toward the central regions of galaxies where star formation can occur. We find {\$}f{\_}{\{}\backslashbackslashrm inf{\}}\backslashbackslashapprox 1{\$} for LTGs and {\$}\backslashbackslashapprox 0.4{\$} for ETGs with an uncertainty of about {\$}0.25{\$} dex, consistent with a biased collapse. By comparing with the locally observed {\$}j{\_}\backslashbackslashstar{\{}\backslash{\$}{\}} vs. {\$}M{\_}\backslashbackslashstar{\{}\backslash{\$}{\}} relations for LTGs and ETGs we estimate the fraction {\$}f{\_}j{\$} of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find {\$}f{\_}j\backslashbackslashapprox 1.11{\^{}}{\{}+0.75{\}}{\_}{\{}-0.44{\}}{\$}, in line with the classic disc formation picture; for ETGs we infer {\$}f{\_}j\backslashbackslashapprox 0.64{\^{}}{\{}+0.20{\}}{\_}{\{}-0.16{\}}{\$}, that can be traced back to a {\$}z{\textless}1{\$} evolution via dry mergers. We also show that the observed scatter in the {\$}j{\_}{\{}\backslashbackslashstar{\{}\backslash{\}}{\}}{\$} vs. {\$}M{\_}{\{}\backslashbackslashstar{\{}\backslash{\}}{\}}{\$} relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at {\$}z\backslashbackslashsim 2{\$} is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, Jingjing and Lapi, Andrea and Mancuso, Claudia and Wang, Huiyuan and Danese, Luigi}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -issn = {1538-4357}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {1983}, -title = {{Angular Momentum of Early and Late Type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -year = {2017} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 < z < 0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 percent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.0763}, -author = {Lackner, C. N. and Gunn, J. E.}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lackner, Gunn - 2012 - Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012arXiv1201.0763L&link_type=ABSTRACT%5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Furlong:2017aa, -archivePrefix = {arXiv}, -arxivId = {arXiv:1510.05645v1}, -author = {Furlong, M and Bower, R G and Crain, R A and Schaye, J and Theuns, T and Trayford, J W and Qu, Y and Schaller, M and Berthet, M and Helly, J C}, -eprint = {arXiv:1510.05645v1}, -journal = {$\backslash$mnras}, -keywords = {evolution,galax-,galaxies,high-redshift,star formation}, -month = {feb}, -number = {October}, -pages = {1--17}, -title = {{Size evolution of normal and compact galaxies in the EAGLE simulation arXiv : 1510 . 05645v1 [ astro-ph . GA ] 19 Oct 2015}}, -volume = {17}, -year = {2018} -} -@article{Brainerd2005, -abstract = {The distribution of satellite galaxies relative to isolated host galaxies in the Sloan Digital Sky Survey (SDSS) is investigated. Host-satellite systems are selected using three different methods, yielding samples of {\$\sim${}}3300, {\$\sim${}}1600, and {\$\sim${}}950 satellites. In the plane of the sky, the distributions of all three samples show highly significant deviations from circular symmetry ({\textgreater}99.99{\%}, {\textgreater}99.99{\%}, and 99.79{\%} confidence levels, respectively), and the degree of anisotropy is a strong function of the projected radius, r p , at which the satellites are found. For r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 100 kpc, the SDSS satellites are aligned preferentially with the major axes of the hosts. This is in stark contrast to the Holmberg effect, in which satellites are aligned with the minor axes of host galaxies. The degree of anisotropy in the distribution of the SDSS satellites decreases with r p and is consistent with an isotropic distribution at of order the 1 $\sigma$ level for 250 kpc {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} r p {\#}{\#}IMG{\#}{\#} [http://ej.iop.org/icons/Entities/lesssim.gif] {\{}lesssim{\}} 500 kpc.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408559}, -author = {Brainerd, Tereasa G}, -doi = {10.1086/432713}, -eprint = {0408559}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L101----L104}, -primaryClass = {astro-ph}, -title = {{Anisotropic Distribution of SDSS Satellite Galaxies: Planar (Not Polar) Alignment}}, -url = {http://stacks.iop.org/1538-4357/628/i=2/a=L101}, -volume = {628}, -year = {2005} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, n=10[cm-3], results in strong expansion of the DM halo in galaxies with stellar masses in the range 107.5 ≤ Mstar ≤ 109.5 M⊙. We find that lower thresholds such as n = 0.1 (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e. ≤50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with n = 10 have gas fractions of ∼0.2 and variations of ∼0.1, while n = 0.1 simulations have order of magnitude lower gas fractions and hence do not expand the halo. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with n = 0.1 and n = 1, but in a reasonable agreement with n = 10. Star formation rates are more variable for higher n, lower galaxy masses, and when star formation is measured on shorter time-scales. For example, simulations with n = 10 have up to 0.4 dex higher scatter in specific star formation rates than simulations with n = 0.1. Thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625}, -author = {Dutton, Aaron A and MacCi{\`{o}}, Andrea V and Buck, Tobias and Dixon, Keri L and Blank, Marvin and Obreja, Aura}, -doi = {10.1093/mnras/stz889}, -eprint = {1811.10625}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure,methods: numerical}, -number = {1}, -pages = {655--671}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://arxiv.org/abs/1811.10625%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stz889}, -volume = {486}, -year = {2019} -} -@article{Veale2017a, -abstract = {We analyse the environmental properties of 370 local early-type galaxies (ETGs) in theMASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute K-band magnitude -21.5 ≳ MK ≳ -26.6, or stellar mass 8 × 109 ≲ M* ≲ 2 × 1012M⊙. We find these galaxies to reside in a diverse range of environments measured by four methods: group membership (whether a galaxy is a brightest group/cluster galaxy, satellite or isolated), halo mass, large-scale mass density (measured over a fewMpc) and local mass density (measured within the Nth neighbour). The spatially resolved IFS stellar kinematics provide robust measurements of the spin parameter $\lambda$e and enable us to examine the relationship among $\lambda$e, M* and galaxy environment. We find a strong correlation between $\lambda$e and M*, where the average $\lambda$e decreases from $\sim$0.4 to below 0.1 with increasing mass, and the fraction of slow rotators fslow increase from $\sim$10 to 90 per cent. We show for the first time that at fixed M*, there are almost no trends between galaxy spin and environment; the apparent kinematic morphology-density relation for ETGs is therefore primarily driven by M* and is accounted for by the joint correlations between M* and spin, and between M* and environment. A possible exception is that the increased fslow at high local density is slightly more than expected based only on these joint correlations. Our results suggest that the physical processes responsible for building up the present-day stellar masses of massive galaxies are also very efficient at reducing their spin, in any environment.}, -archivePrefix = {arXiv}, -arxivId = {1703.08573}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E. and Thomas, Jens and Blakeslee, John P. and McConnell, Nicholas and Walsh, Jonelle L. and Ito, Jennifer}, -doi = {10.1093/mnras/stx1639}, -eprint = {1703.08573}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Veale et al. - 2017 - The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxie.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {1428--1445}, -title = {{The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxies}}, -url = {http://arxiv.org/abs/1703.08573%0Ahttp://dx.doi.org/10.1093/mnras/stx1639}, -volume = {471}, -year = {2017} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR $\eta$(z) using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of 102 SGL with the measurement of corresponding velocity dispersion $\sigma$0 and Einstein radius $\theta$E. In addition, we also use a dataset of 12 two image lensing systems containing the measure of time delay $\Delta$ t between source images. Jointly these two datasets give us the angular diameter distance DAol of the lens. Further, for luminosity distance, we use the 740 observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ($\eta$=1) within 2$\sigma$ confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R F L}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287----a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{Brooks2015a, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brooks, Christensen - 2015 - Bulge formation via mergers in cosmological simulations.pdf:pdf}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Reynolds2015, -abstract = {Compact radio sources sometimes exhibit intervals of large, rapid changes in their flux-density, due to lensing by interstellar plasma crossing the line-of-sight. A novel survey program has made it possible to discover these "Extreme Scattering Events" (ESEs) in real time, resulting in a high-quality dynamic spectrum of an ESE observed in PKS 1939-315. Here we present a method for determining the column-density profile of a plasma lens, given only the dynamic radio spectrum of the lensed source, under the assumption that the lens is either axisymmetric or totally anisotropic. Our technique relies on the known, strong frequency dependence of the plasma refractive index in order to determine how points in the dynamic spectrum map to positions on the lens. We apply our method to high-frequency (4.2-10.8 GHz) data from the Australia Telescope Compact Array of the PKS 1939-315 ESE. The derived electron column-density profiles are very similar for the two geometries we consider, and both yield a good visual match to the data. However, the fit residuals are substantially above the noise level, and deficiencies are evident when we compare the predictions of our model to lower-frequency (1.6-3.1 GHz) data on the same ESE, thus motivating future development of more sophisticated inversion techniques.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1512.03411}, -author = {Tuntsov, Artem V and Walker, Mark A and Koopmans, Leon V E and Bannister, Keith W and Stevens, Jamie and Johnston, Simon and Reynolds, Cormac and Bignall, Hayley E}, -doi = {10.3847/0004-637x/817/2/176}, -eprint = {1512.03411}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {176}, -title = {{Dynamic Spectral Mapping of Interstellar Plasma Lenses}}, -url = {http://arxiv.org/abs/1512.03411%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/2/176}, -volume = {817}, -year = {2016} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P{\_}KS $\backslash$simeq 1.5 $\backslash$times 10{\^{}}{\{}-4{\}}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability $\backslash$simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R and Kravtsov, Andrey V and Gnedin, Oleg Y and Klypin, Anatoly A}, -doi = {10.1086/431355}, -eprint = {0502496}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Grant2006, -abstract = {Soon after launch, the Advanced CCD Imaging Spectrometer (ACIS), one of the focal plane instruments on the Chandra X-ray Observatory, suffered radiation damage from exposure to soft protons during passages through the Earth's radiation belts. The primary effect of the damage was to increase the charge transfer inefficiency (CTI) of the eight front illuminated CCDs by more than two orders of magnitude. The ACIS instrument team is continuing to study the properties of the damage with an emphasis on developing techniques to mitigate CTI and spectral resolution degradation. We present the initial temperature dependence of ACIS CTI from -120 to -60 degrees Celsius and the current temperature dependence after more than six years of continuing slow radiation damage. We use the change of shape of the temperature dependence to speculate on the nature of the damaging particles.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0606178}, -author = {Grant, C E and Bautz, M W and Kissel, S E and LaMarr, B and Prigozhin, G Y}, -doi = {10.1117/12.672019}, -eprint = {0606178}, -isbn = {0819463418}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy II}, -keywords = {acis,chandra,charge coupled devices,charge transfer inefficiency,radiation damage}, -pages = {62761O}, -primaryClass = {astro-ph}, -title = {{Temperature dependence of charge transfer inefficiency in Chandra X-ray CCDs}}, -url = {http://arxiv.org/abs/astro-ph/0606178%7B%5C%25%7D0Ahttp://dx.doi.org/10.1117/12.672019}, -volume = {6276}, -year = {2006} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Wang2018b, -abstract = {We explore the isothermal total density profiles of early-type galaxies (ETGs) in the IllustrisTNG simulation. For the selected 559 ETGs at z = 0 with stellar masses $10^{10.7}\, \mathrm{M}_{\odot } \leqslant M_{\ast } \leqslant 10^{11.9}\, \mathrm{M}_{\odot }$, the total power-law slope has a mean of 〈$\gamma$′〉 = 2.011 ± 0.007 and a scatter of $\sigma _{\gamma ^{\prime }} = 0.171$ over the radial range 0.4–4 times the stellar half-mass radius. Several correlations between $\gamma$′ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction, and in situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduces many correlation trends, and in particular, $\gamma$′ is almost constant with redshift below z = 2. Through analysing IllustrisTNG model variations, we show that black hole kinetic winds are crucial to lowering $\gamma$′ and matching observed galaxy correlations. The effects of stellar winds on $\gamma$′ are subdominant compared to active galactic nucleus (AGN) feedback, and differ due to the presence of AGN feedback from previous works. The density profiles of the ETG dark matter haloes are well described by steeper than NFW profiles, and they are steeper in the full physics (FP) run than their counterparts in the dark matter-only (DMO) run. Their inner density slopes anticorrelate (remain constant) with the halo mass in the FP (DMO) run, and anticorrelate with the halo concentration parameter c200 in both the types of runs. The dark matter haloes of low-mass ETGs are contracted whereas high-mass ETGs are expanded, suggesting that variations in the total density profile occur through the different halo responses to baryons.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -doi = {10.1093/mnras/stz3348}, -eprint = {1811.06545}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2020 - Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons(2).pdf:pdf}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cd,elliptical and lenticular,evolution,formation,galaxies,kine-,matics and dynamics,stellar content}, -number = {4}, -pages = {5188--5215}, -title = {{Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {491}, -year = {2020} -} -@article{Hall2014, -abstract = {The science goals of space missions from the Hubble Space Telescope through to Gaia and Euclid require ultraprecise positional, photometric, and shape measurement information. However, in the radiation environment of the space telescopes, damage to the focal plane detectors through high-energy protons leads to the creation of traps, a loss of charge transfer efficiency, and a consequent deterioration in measurement accuracy. An understanding of the traps produced and their properties in the CCD during operation is essential to allow optimization of the devices and suitable modeling to correct the effect of the damage through the postprocessing of images. The technique of 'pumping single traps' has allowed the study of individual traps in high detail that cannot be achieved with other techniques, such as deep level transient spectroscopy, whilst also locating each trap to the subpixel level in the device. Outlining the principles used, we have demonstrated the technique for the A-center, the most influential trap in serial readout, giving results consistent with the more general theoretical values, but here showing new results indicating the spread in the emission times achieved and the variation in capture probability of individual traps with increasing signal levels. This technique can now be applied to other time and temperature regimes in the CCD to characterize individual traps in situ under standard operating conditions such that dramatic improvements can be made to optimization processes and modeling techniques. {\textcopyright}2013 IEEE.}, -author = {Hall, David J and Murray, Neil J and Holland, Andrew D and Gow, Jason and Clarke, Andrew and Burt, David}, -doi = {10.1109/TNS.2013.2295941}, -isbn = {9781467350570}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {A-centre,CCD image sensors,Euclid,Si-A,defect,pocket pumping,radiation damage,trap pumping}, -number = {4}, -pages = {1826--1833}, -title = {{Determination of in situ trap properties in CCDs using a "single-trap pumping" technique}}, -volume = {61}, -year = {2014} -} -@article{Report2011, -abstract = {Modelling students' behaviour in relation to tuition fees is a complex task since students' 'talent' is not common knowledge. Students observe a private noisy signal of their abilities, while university receives noisy information based on the quantitative and qualitative data provided by university applicants. In this article, we add the heterogeneity of the population to this model: we assume that this heterogeneity means that the perception of skills among a part of the population is biased and underestimates the capabilities of its members to succeed in the higher education system. Our conclusions differ from those derived in the literature and show in particular that the optimal tuition fees for a given number of students are lower than those obtained for a homogeneous population. {\textcopyright} 2013 Copyright Taylor and Francis Group, LLC.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Flacher, Harari-Kermadec - 2013 - Tuition fees, self-esteem and social heterogeneity.pdf:pdf}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Pillepich2017, -abstract = {We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multimode feedback. In this paper, we give a comprehensive description of the physical and numerical advances that form the core of the IllustrisTNG (The Next Generation) framework.We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black-hole-driven kinetic feedback at low accretion rates, magnetohydrodynamics and improvements to the numerical scheme. Using a suite of (25Mpc h-1)3 cosmological boxes, we assess the outcome of the new model at our fiducial resolution. The presence of a selfconsistently amplified magnetic field is shown to have an important impact on the stellar content of 1012M⊙ haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low-mass end of the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {1703.02970}, -author = {Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R{\"{u}}diger and Hernquist, Lars and Torrey, Paul and Vogelsberger, Mark and Weinberger, Rainer and Marinacci, Federico}, -doi = {10.1093/mnras/stx2656}, -eprint = {1703.02970}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {4077--4106}, -title = {{Simulating galaxy formation with the IllustrisTNG model}}, -url = {http://arxiv.org/abs/1703.02970%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx2656}, -volume = {473}, -year = {2018} -} -@article{VandeSande2016, -abstract = {Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h3 ($\sim$skewness) and h4 ($\sim$kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using 2D integral field data from the SAMI Galaxy Survey. A proxy for the spin parameter ($\lambda_{R_e}$) and ellipticity ($\epsilon_e$) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h3 versus $V/\sigma$ anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h3 and $V/\sigma$. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h3 versus $V/\sigma$ signatures. We identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar $\lambda_{R_e}-\epsilon_e$ values can show distinctly different h3-$V/\sigma$ signatures. Class 5 objects are previously unidentified fast rotators that show a weak h3 versus $V/\sigma$ anti-correlation. These objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h3 versus $V/\sigma$ as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.}, -archivePrefix = {arXiv}, -arxivId = {1611.07039}, -author = {van de Sande, Jesse and Bland-Hawthorn, Joss and Fogarty, Lisa M. R. and Cortese, Luca and D'Eugenio, Francesco and Croom, Scott M. and Scott, Nicholas and Allen, James T. and Brough, Sarah and Bryant, Julia J. and Cecil, Gerald and Colless, Matthew and Couch, Warrick J. and Davies, Roger and Elahi, Pascal J. and Foster, Caroline and Goldstein, Gregory and Goodwin, Michael and Groves, Brent and Ho, I-Ting and Jeong, Hyunjin and Jones, D. Heath and Konstantopoulos, Iraklis S. and Lawrence, Jon S. and Leslie, Sarah K. and L{\'{o}}pez-S{\'{a}}nchez, {\'{A}}ngel R. and McDermid, Richard M. and McElroy, Rebecca and Medling, Anne M. and Oh, Sree and Owers, Matt S. and Richards, Samuel N. and Schaefer, Adam L. and Sharp, Rob and Sweet, Sarah M. and Taranu, Dan and Tonini, Chiara and Walcher, C. Jakob and Yi, Sukyoung K.}, -doi = {10.3847/1538-4357/835/1/104}, -eprint = {1611.07039}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sande et al. - 2017 - the Sami Galaxy Survey Revisiting Galaxy Classification Through High-Order Stellar Kinematics.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cosmology,dynamics,evolution,formation,galaxies,kinematics and,observations,stellar content,structure}, -number = {1}, -pages = {104}, -title = {{the Sami Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics}}, -url = {http://arxiv.org/abs/1611.07039%0Ahttp://dx.doi.org/10.3847/1538-4357/835/1/104}, -volume = {835}, -year = {2017} -} -@article{Zehavi2017, -abstract = {We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -- halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto- and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.}, -archivePrefix = {arXiv}, -arxivId = {1706.07871}, -author = {Zehavi, Idit and Contreras, Sergio and Padilla, Nelson and Smith, Nicholas J and Baugh, Carlton M and Norberg, Peder}, -doi = {10.3847/1538-4357/aaa54a}, -eprint = {1706.07871}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {clustering,cosmology,evolution,galaxies,halos,large-scale structure of universe,statistics,theory}, -number = {1}, -pages = {84}, -title = {{The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos}}, -url = {http://arxiv.org/abs/1706.07871%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaa54a}, -volume = {853}, -year = {2018} -} -@article{deNaray2008, -abstract = {We present high-resolution optical velocity fields from DensePak integral field spectroscopy, along with derived rotation curves, for a sample of low surface brightness galaxies. In the limit of no baryons, we fit the NFW and pseudoisothermal halo models to the data and find the rotation curve shapes and halo central densities to be better described by the isothermal halo. For those galaxies with photometry, we present halo fits for three assumptions of the stellar mass-to-light ratio. We find that the velocity contribution from the baryons is significant enough in the maximum disk case that maximum disk and the NFW halo are mutually exclusive. We find a substantial cusp mass excess at the centers of the galaxies, with at least two times more mass expected in the cuspy CDM halo than is allowed by the data. We also find that to reconcile the data with LCDM, $\sim$20 km/s noncircular motions are needed and/or the power spectrum has a lower amplitude on the scales we probe.}, -archivePrefix = {arXiv}, -arxivId = {0712.0860}, -author = {de Naray, Rachel Kuzio and McGaugh, Stacy S. and de Blok, W. J. G.}, -doi = {10.1086/527543}, -eprint = {0712.0860}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Fundamental Parameters,Galaxies: Kinematics and Dynamics}, -month = {apr}, -number = {2}, -pages = {920--943}, -title = {{Mass Models for Low Surface Brightness Galaxies with High‐Resolution Optical Velocity Fields}}, -url = {http://arxiv.org/abs/0712.0860%0Ahttp://dx.doi.org/10.1086/527543}, -volume = {676}, -year = {2008} -} -@article{Strateva2001, -abstract = {We study the optical colors of 147,920 galaxies brighter than g* = 21, observed in five bands by the Sloan Digital Sky Survey (SDSS) over $\sim$100 sq. deg. of high Galactic latitude sky along the Celestial Equator. The distribution of galaxies in the g*-r* vs. u*-g* color--color diagram is strongly bimodal, with an optimal color separator of u*-r* = 2.22. We use visual morphology and spectral classification of subsamples of 287 and 500 galaxies respectively, to show that the two peaks correspond roughly to early (E, S0, Sa) and late (Sb, Sc, Irr) type galaxies, as expected from their different stellar populations. We also find that the colors of galaxies are correlated with their radial profiles, as measured by the concentration index and by the likelihoods of exponential and de Vaucouleurs' profile fits. While it is well known that late type galaxies are bluer than early type galaxies, this is the first detection of a local minimum in their color distribution. In all SDSS bands, the counts vs. apparent magnitude relations for the two color types are significantly different, and indicate that the fraction of blue galaxies increases towards the faint end.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0107201}, -author = {Strateva, Iskra and Ivezi{\'{c}}, {\v{Z}}eljko and Knapp, Gillian R. and Narayanan, Vijay K. and Strauss, Michael A. and Gunn, James E. and Lupton, Robert H. and Schlegel, David and Bahcall, Neta A. and Brinkmann, Jon and Brunner, Robert J. and Budav{\'{a}}ri, Tam{\'{a}}s and Csabai, Istv{\'{a}}n and Castander, Francisco Javier and Doi, Mamoru and Fukugita, Masataka and Győry, Zsuzsanna and Hamabe, Masaru and Hennessy, Greg and Ichikawa, Takashi and Kunszt, Peter Z. and Lamb, Don Q. and McKay, Timothy A. and Okamura, Sadanori and Racusin, Judith and Sekiguchi, Maki and Schneider, Donald P. and Shimasaku, Kazuhiro and York, Donald}, -doi = {10.1086/323301}, -eprint = {0107201}, -isbn = {doi:10.1086/323301}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {fundamental parameters,galaxies}, -month = {oct}, -number = {4}, -pages = {1861--1874}, -primaryClass = {astro-ph}, -title = {{Color Separation of Galaxy Types in the Sloan Digital Sky Survey Imaging Data}}, -url = {http://arxiv.org/abs/astro-ph/0107201%0Ahttp://dx.doi.org/10.1086/323301}, -volume = {122}, -year = {2001} -} -@article{Richard2014, -abstract = {Extending over three Hubble Space Telescope (HST) cycles, the Hubble Frontier Fields (HFF) initiative constitutes the largest commitment ever of HST time to the exploration of the distant Universe via gravitational lensing by massive galaxy clusters. Here, we present models of the mass distribution in the six HFF cluster lenses, derived from a joint strong- and weak-lensing analysis anchored by a total of 88 multiple-image systems identified in existing HST data. The resulting maps of the projected mass distribution and of the gravitational magnification effectively calibrate the HFF clusters as gravitational telescopes. Allowing the computation of search areas in the source plane, these maps are provided to the community to facilitate the exploitation of forthcoming HFF data for quantitative studies of the gravitationally lensed population of background galaxies. Our models of the gravitational magnification afforded by the HFF clusters allow us to quantify the lensing-induced boost in sensitivity over blank-field observations and predict that galaxies at z > 10 and as faint as m(AB) = 32 will be detectable, up to 2 mag fainter than the limit of the Hubble Ultra Deep Field.}, -author = {Richard, Johan and Jauzac, Mathilde and Limousin, Marceau and Jullo, Eric and Cl{\'{e}}ment, Benjamin and Ebeling, Harald and Kneib, Jean Paul and Atek, Hakim and Natarajan, Priya and Egami, Eiichi and Livermore, Rachael and Bower, Richard}, -doi = {10.1093/mnras/stu1395}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Richard et al. - 2014 - Mass and magnification maps for the hubble space telescope frontier fields clusters Implications for high-redshi.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies clusters: individual: A1063S,Galaxies clusters: individual: Abell 370,Galaxies clusters: individual: MACS J0416.1-2403,Galaxies clusters: individual: MACS J0717.5+3745,Galaxies clusters: individual: MACS J1149.5+2223,galaxies clusters: individual: Abell 2744}, -number = {1}, -pages = {268--289}, -title = {{Mass and magnification maps for the hubble space telescope frontier fields clusters: Implications for high-redshift studies}}, -volume = {444}, -year = {2014} -} -@article{pyswarms, -author = {Miranda, Lester James V}, -doi = {10.21105/joss.00433}, -journal = {Journal of Open Source Software}, -number = {21}, -title = {{{P}y{S}warms, a research-toolkit for {P}article {S}warm {O}ptimization in {P}ython}}, -url = {https://doi.org/10.21105/joss.00433}, -volume = {3}, -year = {2018} -} -@article{Morishita2018, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Governato2015, -abstract = {We use high-resolution Hydro+N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass {\$\sim${}}106-7 M⊙, total mass 1010 M⊙) in $\Lambda$-dominated cold dark matter (CDM) and 2 keV warm dark matter (WDM) cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the dark matter (DM) model, but proportionally to the SF efficiency, gas outflows lower the central mass density through 'dynamical heating', such that all realizations have circular velocities {\textless} 20 km s-1 at 500 pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial colour- magnitude diagrams and star formation histories (SFHs) in order to directly compare to available observations. The simulated galaxies formed most of their stars in many {\$\sim${}}10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including 'baryon physics' in simulations when (1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and (2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F and Weisz, D and Pontzen, A and Loebman, S and Reed, D and Brooks, A M and Behroozi, P and Christensen, C and Madau, P and Mayer, L and Shen, S and Walker, M and Quinn, T and Keller, B W and Wadsley, J}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright}2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular it demands highly efficient machine learning and image analysis algorithms. But scalability is not the only challenge: Astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. We argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. In the following, we will present this exciting application area for data scientists. We will focus on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Lagattuta2012, -abstract = {We present new mass models for the gravitational lens system B1938+666, using multiwavelength data acquired from Keck adaptive optics (AO) and Hubble Space Telescope (HST) observations. These models are the first results from the Strong lensing at High Angular Resolution Program (SHARP), a project designed to study known quadruple image and Einstein ring lenses using high-resolution imaging, in order to probe their mass distributions in unprecedented detail. Here, we specifically highlight differences between AO- and HST-derived lens models, finding that - at least when the lens and source galaxies are both bright and red, and the system has a high degree of circular symmetry - AO-derived models place significantly tighter constraints on model parameters. Using this improved precision, we infer important physical properties about the B1938+666 system, including the mass density slope of the lensing galaxy ($\gamma$ = 2.045), the projected dark matter mass fraction within the Einstein radius (M dark/M lens = 0.55) and the total magnification factor of the source galaxy ($\sim$13). Additionally, we measure an upper-limit constraint on luminous substructure (M V > 16.2), based on the non-detection of bright satellite galaxies in all data sets. Finally, we utilize the improved image resolution of the AO data to reveal the presence of faint arcs outside of the primary Einstein ring. The positions and orientations of these arcs raise the intriguing possibility that B1938+666 has a second source galaxy, located at a more distant redshift. However, future work is needed to verify this hypothesis. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1206.1681}, -author = {Lagattuta, D. J. and Vegetti, S. and Fassnacht, C. D. and Auger, M. W. and Koopmans, L. V.E. and Mckean, J. P.}, -doi = {10.1111/j.1365-2966.2012.21406.x}, -eprint = {1206.1681}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: individual: JVAS B1938+666,Gravitational lensing: strong}, -number = {4}, -pages = {2800--2810}, -title = {{Sharp - I. A high-resolution multiband view of the infrared Einstein ring of JVAS B1938+666}}, -volume = {424}, -year = {2012} -} -@article{Rusin2003, -abstract = {We introduce a self-similar mass model for early-type galaxies, and constrain it using the aperture mass-radius relations determined from the geometries of 22 gravitational lenses. The model consists of two components: a concentrated component which traces the light distribution, and a more extended power-law component (rho propto r^-n) which represents the dark matter. We find that lens galaxies have total mass profiles which are nearly isothermal, or slightly steeper, on the several-kiloparsec radial scale spanned by the lensed images. In the limit of a single-component, power-law radial profile, the model implies n=2.07+/-0.13, consistent with isothermal (n=2). Models in which mass traces light are excluded at >99 percent confidence. An n=1 cusp (such as the Navarro-Frenk-White profile) requires a projected dark matter mass fraction of f_cdm = 0.22+/-0.10 inside 2 effective radii. These are the best statistical constraints yet obtained on the mass profiles of lenses, and provide clear evidence for a small but non-zero dark matter mass fraction in the inner regions of early-type galaxies. In addition, we derive the first strong lensing constraint on the relation between stellar mass-to-light ratio (Upsilon) and galaxy luminosity (L): Upsilon propto L^[0.14 (+0.16)(-0.12)], which is consistent with the relation suggested by the fundamental plane. Finally, we apply our self-similar mass models to current problems regarding the interpretation of time delays and flux ratio anomalies in gravitational lens systems.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306096}, -author = {Rusin, D. and Kochanek, C. S. and Keeton, C. R.}, -doi = {10.1086/377356}, -eprint = {0306096}, -issn = {0004-637X}, -journal = {ApJ}, -number = {1}, -pages = {29--42}, -primaryClass = {astro-ph}, -title = {{Self‐similar Models for the Mass Profiles of Early‐Type Lens Galaxies}}, -url = {http://stacks.iop.org/0004-637X/595/i=1/a=29}, -volume = {595} -} -@article{Spiniello2015, -abstract = {We present the X-Shooter Lens Survey (XLENS) data. The main goal of XLENS is to disentangle the stellar and dark matter content of massive early-type galaxies (ETGs), through combined strong gravitational lensing, dynamics and spectroscopic stellar population studies. The sample consists of 11 lens galaxies covering the redshift range from 0.1 to 0.45 and having stellar velocity dispersions between 250 and 380 km s-1. All galaxies have multiband, highquality HST imaging. We have obtained long-slit spectra of the lens galaxies with X-Shooter on the VLT.We are able to disentangle the dark and luminous mass components by combining lensing and extended kinematics data sets, and we are also able to precisely constrain stellar mass-to-light ratios and infer the value of the low-mass cut-off of the initial mass functions (IMF), by adding spectroscopic stellar population information. Our goal is to correlate these IMF parameters with ETG masses and investigate the relation between baryonic and nonbaryonic matter during the mass assembly and structure formation processes. In this paper, we provide an overview of the survey, highlighting its scientific motivations, main goals and techniques. We present the current sample, briefly describing the data reduction and analysis process, and we present the first results on spatially-resolved kinematics.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1507.02183v1}, -author = {Spiniello, C. and Koopmans, L. V.E. and Trager, S. C. and Barnab{\`{e}}, M. and Treu, T. and Czoske, O. and Vegetti, S. and Bolton, A.}, -doi = {10.1093/mnras/stv1490}, -eprint = {arXiv:1507.02183v1}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular, cD,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,Gravitational lensing: strong}, -number = {3}, -pages = {2434--2444}, -title = {{The X-Shooter Lens Survey - II. Sample presentation and spatially-resolved kinematics}}, -volume = {452}, -year = {2015} -} -@article{Goobar2016, -abstract = {We report the discovery of a multiply imaged, gravitationally lensed type Ia supernova, iPTF16geu (SN 2016geu), at redshift z = 0.409. This phenomenon was identified because the light from the stellar explosion was magnified more than 50 times by the curvature of space around matter in an intervening galaxy.We used high-spatial-resolution observations to resolve four images of the lensed supernova, approximately 0.3 arc seconds from the center of the foreground galaxy. The observations probe a physical scale of $\sim$1 kiloparsec, smaller than is typical in other studies of extragalactic gravitational lensing. The large magnification and symmetric image configuration imply close alignment between the lines of sight to the supernova and to the lens. The relative magnifications of the four images provide evidence for substructures in the lensing galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1611.00014}, -author = {Goobar, A. and Amanullah, R. and Kulkarni, S. R. and Nugent, P. E. and Johansson, J. and Steidel, C. and Law, D. and M{\"{o}}rtsell, E. and Quimby, R. and Blagorodnova, N. and Brandeker, A. and Cao, Y. and Cooray, A. and Ferretti, R. and Fremling, C. and Hangard, L. and Kasliwal, M. and Kupfer, T. and Lunnan, R. and Masci, F. and Miller, A. A. and Nayyeri, H. and Neill, J. D. and Ofek, E. O. and Papadogiannakis, S. and Petrushevska, T. and Ravi, V. and Sollerman, J. and Sullivan, M. and Taddia, F. and Walters, R. and Wilson, D. and Yan, L. and Yaron, O.}, -doi = {10.1126/science.aal2729}, -eprint = {1611.00014}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Goobar et al. - 2017 - IPTF16geu A multiply imaged, gravitationally lensed type ia supernova.pdf:pdf}, -isbn = {1095-9203 (Electronic) 0036-8075 (Linking)}, -issn = {10959203}, -journal = {Science}, -number = {6335}, -pages = {291--295}, -pmid = {28428419}, -title = {{IPTF16geu: A multiply imaged, gravitationally lensed type ia supernova}}, -url = {http://arxiv.org/abs/1611.00014}, -volume = {356}, -year = {2017} -} -@article{Zavala2012, -abstract = {We use the combined data sets of the Millennium I and II cosmological simulations to revisit the impact of mergers in the growth of bulges in central galaxies in the $\Lambda$ cold dark matter ($\Lambda$CDM) scenario. We seed galaxies within the growing CDM haloes using semi-empirical relations to assign stellar and gaseous masses, and an analytic treatment to estimate the transfer of stellar mass to the bulge of the remnant after a galaxy merger. We find that this model roughly reproduces the observed correlation between the bulge-to-total mass (B/T) ratio and stellar mass (M *) in present-day central galaxies as well as their observed demographics, although low-mass B/T < 0.1 (bulgeless) galaxies might be scarce relative to the observed abundance. In our merger-driven scenario, bulges have a composite stellar population made of (i) stars acquired from infalling satellites, (ii) stars transferred from the primary disc due to merger-induced perturbations and (iii) newly formed stars in starbursts triggered by mergers. We find that the first two are the main channels of mass assembly, with the first one being dominant for massive galaxies, creating large bulges with different stellar populations than those of the inner discs, while the second is dominant for intermediate/low-mass galaxies and creates small bulges with similar stellar populations to the inner discs. We associate the dominion of the first (second) channel to classical (pseudo) bulges, and compare the predicted fractions to observations. We emphasize that our treatment does not include other mechanisms of bulge growth such as intrinsic secular processes in the disc or misaligned gas accretion. Interestingly, we find that the evolution of the stellar and gaseous contents of the satellite as it spirals towards the central galaxy is a key ingredient in setting the morphology of the remnant galaxy, and that a good match to the observed bulge demographics occurs when this evolution proceeds closely to that of the central galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1204.0516}, -author = {Zavala, Jesus and Avila-Reese, Vladimir and Firmani, Claudio and Boylan-Kolchin, Michael}, -doi = {10.1111/j.1365-2966.2012.22100.x}, -eprint = {1204.0516}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: interactions,Galaxies: structure}, -number = {2}, -pages = {1503--1516}, -title = {{The growth of galactic bulges through mergers in $\Lambda$ CDM haloes revisited - I. Present-day properties}}, -volume = {427}, -year = {2012} -} -@article{Liu2024, -abstract = {Hyperluminous infrared galaxies (HyLIRGs) are the rarest and most extreme starbursts and found only in the distant Universe (z ≳ 1). They have intrinsic infrared (IR) luminosities LIR ≥ 1013 L⊙ and are commonly found to be major mergers. Recently, the Planck All-Sky Survey to Analyze Gravitationally-lensed Extreme Starbursts project (PASSAGES) searched $\sim$104 deg2 of the sky and found $\sim$20 HyLIRGs. We describe a detailed study of PJ0116-24, the brightest ($\mu$LIR ≈ 2.6 × 1014 L⊙, magnified with $\mu$ ≈ 17) Einstein-ring HyLIRG in the southern sky, at z = 2.125, with observations from the near-IR integral-field spectrograph VLT/ERIS and the submillimetre interferometer ALMA. We detected H$\alpha$, H$\beta$, [N ii] and [S ii] lines and obtained an extreme Balmer decrement (H$\alpha$/H$\beta$ ≈ 8.73 ± 1.14). We modelled the molecular-gas and ionized-gas kinematics with CO(3–2) and H$\alpha$ data at $\sim$100–300 pc and (sub)kiloparsec delensed scales, respectively, finding consistent regular rotation. We found PJ0116-24 to be highly rotationally supported (vrot/$\sigma$0, mol. gas ≈ 9.4) with a richer gaseous substructure than other known HyLIRGs. Our results imply that PJ0116-24 is an intrinsically massive (Mbaryon ≈ 1011.3 M⊙) and rare starbursty disk (star-formation rate, SFR = 1,490 M⊙ yr−1) probably undergoing secular evolution. This indicates that the maximal SFR (≳1,000 M⊙ yr−1) predicted by simulations could occur during a galaxy's secular evolution, away from major mergers.}, -author = {Liu, Daizhong and {F{\"{o}}rster Schreiber}, Natascha M. and Harrington, Kevin C. and Lee, Lilian L. and Kamieneski, Patrick S. and Davies, Richard I. and Lutz, Dieter and Renzini, Alvio and Wuyts, Stijn and Tacconi, Linda J. and Genzel, Reinhard and Burkert, Andreas and Herrera-Camus, Rodrigo and {Alcalde Pampliega}, Bel{\'{e}}n and Vishwas, Amit and Kaasinen, Melanie and Wang, Q. Daniel and Jim{\'{e}}nez-Andrade, Eric F. and Lowenthal, James and Foo, Nicholas and Frye, Brenda L. and Shangguan, Jinyi and Cao, Yixian and Agapito, Guido and Berbel, Alex Agudo and Barfety, Capucine and Baruffolo, Andrea and Berman, Derek and Black, Martin and Bonaglia, Marco and Briguglio, Runa and Carbonaro, Luca and Chapman, Lee and Chen, Jianhang and Cikota, Aleksandar and Concas, Alice and Cooper, Olivia and Cresci, Giovanni and Dallilar, Yigit and Deysenroth, Matthias and {Di Antonio}, Ivan and {Di Cianno}, Amico and {Di Rico}, Gianluca and Doelman, David and Dolci, Mauro and Eisenhauer, Frank and Espejo, Juan and Esposito, Simone and Fantinel, Daniela and Ferruzzi, Debora and Feuchtgruber, Helmut and Gao, Xiaofeng and {Garcia Diaz}, Carlos and Gillessen, Stefan and Grani, Paolo and Hartl, Michael and Henry, David and Huber, Heinrich and Jolly, Jean Baptiste and Keller, Christoph U. and Kenworthy, Matthew and Kravchenko, Kateryna and Lee, Minju M. and Lightfoot, John and Lunney, David and Macintosh, Mike and Mannucci, Filippo and Ott, Thomas and Pascale, Massimo and Pastras, Stavros and Pearson, David and Puglisi, Alfio and Pulsoni, Claudia and Rabien, Sebastian and Rau, Christian and Riccardi, Armando and Salasnich, Bernardo and Shimizu, Taro and Snik, Frans and Sturm, Eckhard and Taylor, William and Valentini, Angelo and Waring, Christopher and Wiezorrek, Erich and Xompero, Marco and Yun, Min S.}, -doi = {10.1038/s41550-024-02296-7}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Liu2024JyperLuminousSL.pdf:pdf}, -issn = {23973366}, -journal = {Nature Astronomy}, -number = {September}, -title = {{Detailed study of a rare hyperluminous rotating disk in an Einstein ring 10 billion years ago}}, -volume = {8}, -year = {2024} -} -@article{Pub---ae2019, -archivePrefix = {arXiv}, -arxivId = {arXiv:1807.09278v3}, -author = {Pub---ae, Fermilab and Shajib, A J and Birrer, S and Treu, T and Auger, M W and Agnello, A and Anguita, T and Chan, J H H and Collett, T E and Courbin, F and Fassnacht, C D and Frieman, J and Kayo, I and Lemon, C and Lin, H and Marshall, P J and Mcmahon, R and Morgan, N D and Motta, V and Oguri, M and Ostrovski, F and Rusu, C E and Schechter, P L and Shanks, T and Suyu, S H and Meylan, G and Abbott, T M C and Allam, S and Annis, J and Avila, S and Bertin, E and Brooks, D and Rosell, A Carnero and Kind, M Carrasco and Carretero, J and Cunha, C E and Costa, L N and Vicente, J De and Desai, S and Doel, P and Flaugher, B and Fosalba, P and Garc, J and Gerdes, D W and Gruen, D and Gruendl, R A and Gutierrez, G and Hartley, W G and Hollowood, D L and Hoyle, B and James, D J and Kuehn, K and Marshall, J L and Melchior, P and Menanteau, F and Miquel, R and Plazas, A A and Sobreira, F and Suchyta, E and Swanson, M E C and Tarle, G and Walker, A R}, -eprint = {arXiv:1807.09278v3}, -keywords = {cd,data analysis,ellip-,galaxies,gravitational lensing,methods,strong,structure,tical and lenticular}, -number = {January}, -pages = {1--20}, -title = {{Is every strong lens model unhappy in its own way ? Uniform modelling of a sample of 13 quadruply + imaged quasars}}, -volume = {20}, -year = {2019} -} -@article{Gentile2004, -abstract = {We present, for five spiral galaxies, H I data which, along with the Ha rotation curves, are used to derive the distribution of dark matter within these objects. A new method for extracting rotation curves from Hi data cubes is presented, which takes into account the existence of a warp and minimizes projection effects. The rotation curves obtained are tested by taking them as input in the construction of model data cubes that are compared with the observed ones: the agreement is excellent. Model data cubes built using rotation curves obtained with standard methods, such as the first-moment analysis, however, fail the test. The HI rotation curves agree well with the Ha data, where they coexist. Moreover, the combined H$\alpha$ + HI rotation curves are smooth, symmetric and extend to large radii. The rotation curves are decomposed into stellar, gaseous and dark matter contributions, and the inferred density distribution is compared with various mass distributions: dark haloes with a central density core, A cold dark matter ($\Lambda$CDM) haloes (NFW and Moore profiles), H I scaling and MOND. The observations point to haloes with constant-density cores of size r core ∼ r opt and central densities scaling approximately as $\rho$ 0 $\alpha$ r -2/3. ACDM models (which predict a central cusp in the density profile) are in clear conflict with the data. H I scaling and MOND cannot account for the observed kinematics: we find some counter-examples.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0403154}, -author = {Gentile, G. and Salucci, P. and Klein, U. and Vergani, D. and Kalberla, P.}, -doi = {10.1111/j.1365-2966.2004.07836.x}, -eprint = {0403154}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: kinematics and dynamics,Galaxies: spiral,Methods: data analysis}, -number = {3}, -pages = {903--922}, -primaryClass = {astro-ph}, -title = {{The cored distribution of dark matter in spiral galaxies}}, -volume = {351}, -year = {2004} -} -@article{Fergus2014, -abstract = {High dynamic range imagers aim to block or eliminate light from a very bright primary star in order to make it possible to detect and measure far fainter companions; in real systems, a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronagraph. The model uses principal components analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles, but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of the order of a percent of the brightness of the speckles, or up to 10-7 times the brightness of the primary star. This outperforms existing methods by a factor of two to three and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Spolaor2009, -abstract = {We present a newly observed relation between galaxy mass and radial metallicity gradients of early-type galaxies. Our sample of 51 early-type galaxies encompasses a comprehensive mass range from dwarfs to brightest cluster galaxies. The metallicity gradients are measured out to one effective radius by comparing nearly all of the Lick absorption-line indices to recent models of single stellar populations. The relation shows very different behavior at low and high masses, with a sharp transition being seen at a mass of 3.5 × 1010M (velocity dispersion of 140 km s-1, MB -19). Low-mass galaxies form a tight relation with mass, such that metallicity gradients become shallower with decreasing mass and positive at the very low mass end. Above the mass transition point several massive galaxies have steeper gradients, but a clear downturn is visible marked by a broad scatter. The results are interpreted in comparison with competing model predictions. We find that an early star-forming collapse could have acted as the main mechanism for the formation of low-mass galaxies, with star formation efficiency increasing with galactic mass. The high-mass downturn could be a consequence of merging and the observed larger scatter a natural result of different merger properties. These results suggest that galaxies above the mass threshold of 3.5 × 1010M might have formed initially by mergers of gas-rich disk galaxies and then subsequently evolved via dry merger events. The varying efficiency of the dissipative merger-induced starburst and feedback processes have shaped the radial metallicity gradients in these high-mass systems. {\textcopyright} 2009. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {0901.0548}, -author = {Spolaor, Max and Proctor, Robert N. and Forbes, Duncan A. and Couch, Warrick J.}, -doi = {10.1088/0004-637X/691/2/L138}, -eprint = {0901.0548}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: dwarf,Galaxies: elliptical and lenticular, cD,Galaxies: formation,Galaxies: stellar content}, -number = {2}, -pages = {5}, -title = {{THE mass-metallicity gradient relation of early-type galaxies}}, -url = {http://stacks.iop.org/1538-4357/691/i=2/a=L138?key=crossref.f993bf46fa11e4025dea4dbc112eb974%5Cnhttp://arxiv.org/abs/0901.0548}, -volume = {691}, -year = {2009} -} -@article{Libeskind2014, -abstract = {We examine the angular infall pattern of subhaloes on to host haloes in the context of the large-scale structure. We find that this infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are found to be preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that it is always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range (∼10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large-scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group. {\textcopyright} 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1407.0394}, -author = {Libeskind, Noam I. and Knebe, Alexander and Hoffman, Yehuda and Gottl{\"{o}}ber, Stefan}, -doi = {10.1093/mnras/stu1216}, -eprint = {1407.0394}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Libeskind et al. - 2014 - The universal nature of subhalo accretion(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Large-scale structure of universe}, -number = {2}, -pages = {1274--1280}, -title = {{The universal nature of subhalo accretion}}, -volume = {443}, -year = {2014} -} -@article{Murray2013, -abstract = {A multi-level clocking scheme has been developed to improve the parallel CTE of four-phase CCDs by suppressing the effects of traps located in the transport channel under barrier phases by inverting one of these phases throughout the transfer sequence. In parallel it was apparent that persistence following optical overload in Euclid VIS detectors would lead to undesirable signal released in subsequent rows and frames and that a suitable scheme for flushing this signal would be required. With care, the negatively biased electrodes during the multi-level transfer sequence can be made to pin the entire surface, row-by-row, and annihilate the problematic charges. This process can also be extended for use during integration to significantly reduce the unusable area of the detector, as per the clocked anti-blooming techniques developed many years ago; however, with the four-phase electrodes architecture of modern CCDs, we can take precautionary measures to avoid the problem of charge pumping and clock induced charge within the science frames. Clock induced charge is not all bad! We also propose the use of on-orbit trap-pumping for Euclid VIS to provide calibration input to ground based correction algorithms and as such a uniform, low noise background is require. Clock induced charge can be manipulated to provide a very suitable, low signal and noise background to the imaging array. Here we describe and present results of multi-level parallel clocking schemes for use in four-phase CCDs that could improve performance of high precision astronomy applications such as Euclid VIS. ? 2013 SPIE.}, -author = {Murray, Neil J. and Burt, David J. and Holland, Andrew D. and Stefanov, Konstantin D. and Gow, Jason P. D. and MacCormick, Calum and Dryer, Ben J. and Allanwood, Edgar A. H.}, -doi = {10.1117/12.2024839}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2013 - Multi-level parallel clocking of CCDs for improving charge transfer efficiency, clearing persistence, clocked ant.pdf:pdf}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {Blooming,CAB,CCD,CIC,CTE,Euclid VIS,Mu,[BFW}, -pages = {88600K}, -title = {{Multi-level parallel clocking of CCDs for: improving charge transfer efficiency, clearing persistence, clocked anti-blooming, and generating low-noise backgrounds for pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024839}, -volume = {8860}, -year = {2013} -} -@article{Naab2009, -abstract = {Using a high-resolution hydrodynamical cosmological simulation of the formation of a massive spheroidal galaxy we show that elliptical galaxies can be very compact and massive at high redshift in agreement with recent observations. Accretion of stripped infalling stellar material increases the size of the system with time and the central concentration is reduced by dynamical friction of the surviving stellar cores. In a specific case of a spheroidal galaxy with a final stellar mass of 1.5 × 1011 M ⊙ we find that the effective radius re increases from 0.7 ± 0.2 kpc at z = 3 to re = 2.4 ± 0.4 kpc at z = 0 with a concomitant decrease in the effective density of an order of magnitude and a decrease of the central velocity dispersion by approximately 20% over this time interval. A simple argument based on the virial theorem shows that during the accretion of weakly bound material (minor mergers) the radius can increase as the square of the mass in contrast to the usual linear rate of increase for major mergers. By undergoing minor mergers compact high-redshift spheroids can evolve into present-day systems with sizes and concentrations similar to observed local ellipticals. This indicates that minor mergers may be the main driver for the late evolution of sizes and densities of early-type galaxies. {\textcopyright} 2009 The American Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {0903.1636}, -author = {Naab, Thorsten and Johansson, Peter H. and Ostriker, Jeremiah P.}, -doi = {10.1088/0004-637X/699/2/L178}, -eprint = {0903.1636}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Naab, Johansson, Ostriker - 2010 - Minor mergers and the size evolution of elliptical galaxies.pdf:pdf}, -issn = {2041-821}, -journal = {Astrophysical Journal Letters}, -keywords = {Galaxies: elliptical and lenticular, cd,Galaxies: evolution,Galaxies: interactions,Galaxies: structure,Methods: numerical}, -month = {jul}, -number = {2 PART 2}, -pages = {L178--L182}, -title = {{Minor mergers and the size evolution of elliptical galaxies}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L178?key=crossref.405faa44137f4be9a7e3800a4c3e7dea}, -volume = {699}, -year = {2010} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 < z < 0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 percent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.0763}, -author = {Lackner, C. N. and Gunn, J. E.}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lackner, Gunn - 2012 - Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012arXiv1201.0763L&link_type=ABSTRACT%5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Handley2015, -abstract = {PolyChord is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of PolyChord v1.3, and provides an extensive account of the algorithm. PolyChord utilises slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelised using openMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in CosmoMC and CAMB, and is now in use in the CosmoChord and ModeChord codes. PolyChord is available for download at: http://ccpforge.cse.rl.ac.uk/gf/project/polychord/}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless}{\$}\sigma{\$}∗ {\textless}370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [{\$}\alpha{\$}/Fe] increase with increasing {\$}\sigma{\$}∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for {\$}\sigma{\$}∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history. {\textcopyright}2015. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and {\$}\backslash{\$}nspectroscopic ESA cornerstone mission, currently scheduled for launch in{\$}\backslash{\$}nlate 2011. Its primary science drivers are the composition, formation{\$}\backslash{\$}nand evolution of the Galaxy. Gaia will not achieve its scientific{\$}\backslash{\$}nrequirements without detailed calibration and correction for radiation{\$}\backslash{\$}ndamage. Microscopic models of Gaia's CCDs are being developed to{\$}\backslash{\$}nsimulate the effect of radiation damage, charge trapping, which causes{\$}\backslash{\$}ncharge transfer inefficiency. The key to calculating the probability of{\$}\backslash{\$}na photoelectron being captured by a trap is the 3D electron density{\$}\backslash{\$}nwithin each CCD pixel. However, this has not been physically modelled{\$}\backslash{\$}nfor Gaia CCD pixels. In this paper, the first of a series, we motivate{\$}\backslash{\$}nthe need for such specialised 3D device modelling and outline how its{\$}\backslash{\$}nfuture results will fit into Gaia's overall radiation calibration{\$}\backslash{\$}nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -isbn = {0277-786X}, -issn = {0277786X}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Tagore2017, -abstract = {Cosmological parameter constraints from observations of time-delay lenses are becoming increasingly precise. However, there may be significant bias and scatter in these measurements due to, among other things, the so-called mass-sheet degeneracy. To estimate these uncertainties, we analyse strong lenses from the largest EAGLE hydrodynamical simulation. We apply a mass-sheet transformation to the radial density profiles of lenses, and by selecting lenses near isothermality, we find that the bias on H0 can be reduced to 5 per cent with an intrinsic scatter of 10 per cent, confirming previous results performed on a different simulation data set. We further investigate whether combining lensing observables with kinematic constraints helps to minimize this bias. We do not detect any significant dependence of the bias on lens model parameters or observational properties of the galaxy, but depending on the source-lens configuration, a bias may still exist. Cross lenses provide an accurate estimate of the Hubble constant, while fold (double) lenses tend to be biased low (high). With kinematic constraints, double lenses show bias and intrinsic scatter of 6 per cent and 10 per cent, respectively, while quad lenses show bias and intrinsic scatter of 0.5 per cent and 10 per cent, respectively. For lenses with a reduced Χ2 > 1, a power-law dependence of the Χ2 on the lens environment (number of nearby galaxies) is seen. Lastly, we model, in greater detail, the cases of two double lenses that are significantly biased. We are able to remove the bias, suggesting that the remaining biases could also be reduced by carefully taking into account additional sources of systematic uncertainty.}, -archivePrefix = {arXiv}, -arxivId = {1706.07733}, -author = {Tagore, Amitpal S. and Barnes, David J. and Jackson, Neal and Kay, Scott T. and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx2965}, -eprint = {1706.07733}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tagore et al. - 2018 - Reducing biases on H0 measurements using strong lensing and galaxy dynamics Results from the eagle simulation(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Galaxies: kinematics and dynamics,Gravitational lensing: strong,Methods: numerical}, -number = {3}, -pages = {3403--3422}, -title = {{Reducing biases on H0 measurements using strong lensing and galaxy dynamics: Results from the eagle simulation}}, -url = {http://arxiv.org/abs/1706.07733}, -volume = {474}, -year = {2018} -} -@article{MinkaT.2008, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture}, -author = {Zarocostas, John}, -doi = {10.1136/bmj.d706}, -issn = {14685833}, -journal = {BMJ (Clinical research ed.)}, -pages = {16}, -pmid = {21285225}, -title = {{Gates and Cameron pledge new money to eradicate polio.}}, -volume = {342}, -year = {2011} -} -@article{Blanton2003, -abstract = {Using photometry and spectroscopy of 144,609 galaxies from the Sloan Digital Sky Survey, we present bivariate distributions of pairs of seven galaxy properties: four optical colors, surface brightness, radial profile shape as measured by the Sersic index, and absolute magnitude. In addition, we present the dependence of local galaxy density (smoothed on 8 h{\^{}}{\{}-1{\}} Mpc scales) on all of these properties. Several classic, well-known relations among galaxy properties are evident at extremely high signal-to-noise ratio: the color-color relations of galaxies, the color-magnitude relations, the magnitude-surface brightness relation, and the dependence of density on color and absolute magnitude. We show that most of the i-band luminosity density in the universe is in the absolute magnitude and surface brightness ranges used. Some of the relationships between parameters, in particular the color--magnitude relations, show stronger correlations for exponential galaxies and concentrated galaxies taken separately than for all galaxies taken together. We provide a simple set of fits of the dependence of galaxy properties on luminosity for these two sets of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0209479}, -author = {Blanton, Michael R and Hogg, David W and Bahcall, Neta A and Baldry, Ivan K and Brinkmann, J and Csabai, Istvan and Eisenstein, Daniel and Fukugita, Masataka and Gunn, James E and Ivezi{\'{c}}, {\v{Z}}eljko and Lamb, D Q and Lupton, Robert H and Loveday, Jon and Munn, Jeffrey A and Nichol, R C and Okamura, Sadanori and Schlegel, David J and Shimasaku, Kazuhiro and Strauss, Michael A and Vogeley, Michael S and Weinberg, David H}, -doi = {10.1086/375528}, -eprint = {0209479}, -isbn = {0004-6256}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Fundamental Parameters,Galaxies: Photometry,Galaxies: Statistics}, -month = {sep}, -number = {1}, -pages = {186--207}, -pmid = {19408790}, -primaryClass = {astro-ph}, -title = {{ The Broadband Optical Properties of Galaxies with Redshifts 0.02 {\textless} z {\textless} 0.22 }}, -url = {http://arxiv.org/abs/astro-ph/0209479%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/375528}, -volume = {594}, -year = {2003} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and disks are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disk components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to CALIFA integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component, and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -keywords = {elliptical and lenticular,galaxies,kinematics and dynamics}, -number = {December}, -pages = {1--11}, -title = {{Untangling galaxy components: full spectral bulge-disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {11}, -year = {2016} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Morishita2018, -abstract = {Observations have revealed massive (logM*/Msun>11) galaxies that were already dead when the universe was only $\sim$2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6 50% of their extant masses by $\sim$1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of $\sim$0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z$\sim$5.5 to $\sim$2.2 at a rate of $\sim$0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, $\sim$0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T. and Abramson, L. E. and Treu, T. and Brammer, G. B. and Jones, T. and Kelly, P. and Stiavelli, M. and Trenti, M. and Vulcani, B. and Wang, X.}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Morishita et al. - 2019 - Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enr(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1{\textless}z{\textless}3. Our analysis is based on a bulge-disk decomposition of 396 galaxies with Mstar{\textgreater}10{\^{}}11 Msolar from the CANDELS WFC3/IR imaging within the COSMOS and UKIDSS UDS survey fields. We find that, by modelling the H(160) image of each galaxy with a combination of a de Vaucouleurs bulge (Sersic index n=4) and an exponential disk (n=1), we can then lock all derived morphological parameters for the bulge and disk components, and successfully reproduce the shorter-wavelength J(125), i(814), v(606) HST images simply by floating the magnitudes of the two components. This then yields sub-divided 4-band HST photometry for the bulge and disk components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information we are able to properly determine the masses and star-formation rates for the bulge and disk components, and find that: i) from z=3 to z=1 the galaxies move from disk-dominated to increasingly bulge-dominated, but very few galaxies are pure bulges/ellipticals by z=1; ii) while most passive galaxies are bulge-dominated, and most star-forming galaxies disk-dominated, 18+/-5{\%} of passive galaxies are disk-dominated, and 11+/-3{\%} of star-forming galaxies are bulge-dominated, a result which needs to be explained by any model purporting to connect star-formation quenching with morphological transformations; iii) there exists a small but significant population of pure passive disks, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a{\$\sim${}}0.7); iv) flatter/larger disks re-emerge at the highest star-formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface-density for star-formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.1736}, -volume = {444}, -year = {2014} -} -@article{Minka2009, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture models is not well captured by factor graphs unless the entire mixture is represented by one factor, because the message equations have a containment structure. Gates capture this containment structure graphically, allowing both the independences and the message-passing equations for a model to be readily visualized. Different variational approximations for mixture models can be understood as different ways of drawing the gates in a model. We present general equations for expectation propagation and variational message passing in the presence of gates.}, -author = {Minka, Tom and Winn, John}, -doi = {10.5790/hongkong/9789888083091.003.0088}, -isbn = {9781605609492}, -issn = {0018702X}, -journal = {Advances in Neural Information Processing Systems 21 - Proceedings of the 2008 Conference}, -pages = {1073--1080}, -title = {{Gates}}, -year = {2009} -} -@article{Rines2013, -abstract = {The infall regions of galaxy clusters represent the largest gravitationally bound structures in a $\Lambda$CDM universe. Measuring cluster mass profiles into the infall regions provides an estimate of the ultimate mass of these halos. We use the caustic technique to measure cluster mass profiles from galaxy redshifts obtained with the Hectospec Cluster Survey (HeCS), an extensive spectroscopic survey of galaxy clusters with MMT/Hectospec. We survey 58 clusters selected by X-ray flux at 0.1 < z < 0.3. The survey includes 22,680 unique MMT/Hectospec redshifts for individual galaxies; 10,145 of these galaxies are cluster members. For each cluster, we acquired high signal-to-noise spectra for ∼200 cluster members and a comparable number of foreground/background galaxies. The cluster members trace out infall patterns around the clusters. The members define a very narrow red sequence. We demonstrate that the determination of velocity dispersion is insensitive to the inclusion of bluer members (a small fraction of the cluster population). We apply the caustic technique to define membership and estimate the mass profiles to large radii. The ultimate halo mass of clusters (the mass that remains bound in the far future of a $\Lambda$CDM universe) is on average (1.99 ± 0.11)M 200, a new observational cosmological test in essential agreement with simulations. Summed profiles binned in M 200 and in L X demonstrate that the predicted Navarro-Frenk-White form of the density profile is a remarkably good representation of the data in agreement with weak lensing results extending to large radius. The concentration of these summed profiles is also consistent with theoretical predictions. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1209.3786}, -author = {Rines, Kenneth and Geller, Margaret J. and Diaferio, Antonaldo and Kurtz, Michael J.}, -doi = {10.1088/0004-637X/767/1/15}, -eprint = {1209.3786}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Rines2013HeSC.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cosmology: observations,galaxies: clusters: general,galaxies: kinematics and dynamics}, -number = {1}, -pages = {15}, -title = {{Measuring the ultimate halo mass of galaxy clusters: Redshifts and mass profiles from the hectospec cluster survey (HECS)}}, -volume = {767}, -year = {2013} -} -@article{Halverson2016, -abstract = {We describe a detailed radial velocity error budget for the NASA-NSF Extreme Precision Doppler Spectrometer instrument concept NEID (NN-explore Exoplanet Investigations with Doppler spectroscopy). Such an instrument performance budget is a necessity for both identifying the variety of noise sources currently limiting Doppler measurements, and estimating the achievable performance of next generation exoplanet hunting Doppler spectrometers. For these instruments, no single source of instrumental error is expected to set the overall measurement floor. Rather, the overall instrumental measurement precision is set by the contribution of many individual error sources. We use a combination of numerical simulations, educated estimates based on published materials, extrapolations of physical models, results from laboratory measurements of spectroscopic subsystems, and informed upper limits for a variety of error sources to identify likely sources of systematic error and construct our global instrument performance error budget. While natively focused on the performance of the NEID instrument, this modular performance budget is immediately adaptable to a number of current and future instruments. Such an approach is an important step in charting a path towards improving Doppler measurement precisions to the levels necessary for discovering Earth-like planets.}, -archivePrefix = {arXiv}, -arxivId = {1607.05634}, -author = {Halverson, Samuel and Terrien, Ryan and Mahadevan, Suvrath and Roy, Arpita and Bender, Chad and Stef{\'{a}}nsson, Gudmundur K and Monson, Andrew and Levi, Eric and Hearty, Fred and Blake, Cullen and McElwain, Michael and Schwab, Christian and Ramsey, Lawrence and Wright, Jason and Wang, Sharon and Gong, Qian and Roberston, Paul}, -doi = {10.1117/12.2232761}, -eprint = {1607.05634}, -isbn = {9781510601956}, -issn = {1996756X}, -journal = {Ground-based and Airborne Instrumentation for Astronomy VI}, -keywords = {exoplanets,high resolution spectroscopy,radial velocity instrumentation,systems engineering}, -pages = {99086P}, -title = {{A comprehensive radial velocity error budget for next generation Doppler spectrometers}}, -url = {http://arxiv.org/abs/1607.05634%7B%5C%25%7D0Ahttp://dx.doi.org/10.1117/12.2232761}, -volume = {9908}, -year = {2016} -} -@article{Hsu2018, -abstract = {We present a new framework to characterize the occurrence rates of planet candidates identified by Kepler based on hierarchical Bayesian modeling, Approximate Bayesian Computing (ABC), and sequential importance sampling. For this study we adopt a simple 2-D grid in planet radius and orbital period as our model and apply our algorithm to estimate occurrence rates for Q1-Q16 planet candidates orbiting around solar-type stars. We arrive at significantly increased planet occurrence rates for small planet candidates ({\$}R{\_}p{\textless}1.25 R{\_}{\{}\backslashoplus{\}}{\$}) at larger orbital periods ({\$}P{\textgreater}80{\$}d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is {\$}1.6{\^{}}{\{}+1.2{\}}{\_}{\{}-0.5{\}}{\$} per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2{\$}R{\_}{\{}\backslashoplus{\}}{\$} that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C and Ford, Eric B and Ragozzine, Darin and Morehead, Robert C}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -number = {5}, -pages = {205}, -title = {{ Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation }}, -url = {http://arxiv.org/abs/1803.10787%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -volume = {155}, -year = {2018} -} -@article{Buchner2014, -abstract = {Context. Aims. Active galactic nuclei are known to have complex X-ray spectra that depend on both the properties of the accreting super-massive black hole (e.g. mass, accretion rate) and the distribution of obscuring material in its vicinity (i.e. the "torus"). Often however, simple and even unphysical models are adopted to represent the X-ray spectra of AGN, which do not capture the complexity and diversity of the observations. In the case of blank field surveys in particular, this should have an impact on e.g. the determination of the AGN luminosity function, the inferred accretion history of the Universe and also on our understanding of the relation between AGN and their host galaxies. Methods. We develop a Bayesian framework for model comparison and parameter estimation of X-ray spectra. We take into account uncertainties associated with both the Poisson nature of X-ray data and the determination of source redshift using photometric methods. We also demonstrate how Bayesian model comparison can be used to select among ten different physically motivated X-ray spectral models the one that provides a better representation of the observations. This methodology is applied to X-ray AGN in the 4 Ms Chandra Deep Field South. Results. For the {\$\sim${}}350 AGN in that field, our analysis identifies four components needed to represent the diversity of the observed X-ray spectra: (1) an intrinsic power law; (2) a cold obscurer which reprocesses the radiation due to photo-electric absorption, Compton scattering and Fe-K fluorescence; (3) an unabsorbed power law associated with Thomson scattering off ionised clouds; and (4) Compton reflection, most noticeable from a stronger-than-expected Fe-K line. Simpler models, such as a photo-electrically absorbed power law with a Thomson scattering component, are ruled out with decisive evidence (B {\textgreater} 100). We also find that ignoring the Thomson scattering component results in underestimation of the inferred column density, NH, of the obscurer. Regarding the geometry of the obscurer, there is strong evidence against both a completely closed (e.g. sphere), or entirely open (e.g. blob of material along the line of sight), toroidal geometry in favour of an intermediate case. Conclusions. Despite the use of low-count spectra, our methodology is able to draw strong inferences on the geometry of the torus. Simpler models are ruled out in favour of a geometrically extended structure with significant Compton scattering. We confirm the presence of a soft component, possibly associated with Thomson scattering off ionised clouds in the opening angle of the torus. The additional Compton reflection required by data over that predicted by toroidal geometry models, may be a sign of a density gradient in the torus or reflection off the accretion disk. Finally, we release a catalogue of AGN in the CDFS with estimated parameters such as the accretion luminosity in the 2-10 keV band and the column density, NH, of the obscurer. {\textcopyright}ESO, 2014.}, -archivePrefix = {arXiv}, -arxivId = {1402.0004}, -author = {Buchner, J and Georgakakis, A and Nandra, K and Hsu, L and Rangel, C and Brightman, M and Merloni, A and Salvato, M and Donley, J and Kocevski, D}, -doi = {10.1051/0004-6361/201322971}, -eprint = {1402.0004}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buchner et al. - 2014 - X-ray spectral modelling of the AGN obscuring region in the CDFS Bayesian model selection and catalogue.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Accretion,Galaxies: high-redshift,Galaxies: nuclei,Methods: data analysis,Methods: statistical,X-rays: galaxies,accretion disks}, -pages = {A125}, -title = {{X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue}}, -volume = {564}, -year = {2014} -} -@article{Blanton2003, -abstract = {Using photometry and spectroscopy of 144,609 galaxies from the Sloan Digital Sky Survey, we present bivariate distributions of pairs of seven galaxy properties: four optical colors, surface brightness, radial profile shape as measured by the Sersic index, and absolute magnitude. In addition, we present the dependence of local galaxy density (smoothed on 8 h^{-1} Mpc scales) on all of these properties. Several classic, well-known relations among galaxy properties are evident at extremely high signal-to-noise ratio: the color-color relations of galaxies, the color-magnitude relations, the magnitude-surface brightness relation, and the dependence of density on color and absolute magnitude. We show that most of the i-band luminosity density in the universe is in the absolute magnitude and surface brightness ranges used. Some of the relationships between parameters, in particular the color--magnitude relations, show stronger correlations for exponential galaxies and concentrated galaxies taken separately than for all galaxies taken together. We provide a simple set of fits of the dependence of galaxy properties on luminosity for these two sets of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0209479}, -author = {Blanton, Michael R. and Hogg, David W. and Bahcall, Neta A. and Baldry, Ivan K. and Brinkmann, J. and Csabai, Istvan and Eisenstein, Daniel and Fukugita, Masataka and Gunn, James E. and Ivezi{\'{c}}, {\v{Z}}eljko and Lamb, D. Q. and Lupton, Robert H. and Loveday, Jon and Munn, Jeffrey A. and Nichol, R. C. and Okamura, Sadanori and Schlegel, David J. and Shimasaku, Kazuhiro and Strauss, Michael A. and Vogeley, Michael S. and Weinberg, David H.}, -doi = {10.1086/375528}, -eprint = {0209479}, -isbn = {0004-6256}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Fundamental Parameters,Galaxies: Photometry,Galaxies: Statistics}, -month = {sep}, -number = {1}, -pages = {186--207}, -pmid = {19408790}, -primaryClass = {astro-ph}, -title = {{ The Broadband Optical Properties of Galaxies with Redshifts 0.02 < z < 0.22 }}, -url = {http://arxiv.org/abs/astro-ph/0209479%0Ahttp://dx.doi.org/10.1086/375528}, -volume = {594}, -year = {2003} -} -@article{Nightingale2018, -abstract = {This work presents AutoLens, the first entirely automated modeling suite for the analysis of galaxy-scale strong gravitational lenses. AutoLens simultaneously models the lens galaxy's light and mass whilst reconstructing the extended source galaxy on an adaptive pixel-grid. The method's approach to source-plane discretization is amorphous, adapting its clustering and regularization to the intrinsic properties of the lensed source. The lens's light is fitted using a superposition of Sersic functions, allowing AutoLens to cleanly deblend its light from the source. Single-component mass models representing the lens's total mass density profile are demonstrated, which in conjunction with light modeling can detect central images using a centrally cored profile. Decomposed mass modeling is also shown, which can fully decouple a lens's light and dark matter and determine whether the two components are geometrically aligned. The complexity of the light and mass models is automatically chosen via Bayesian model comparison. These steps form AutoLens's automated analysis pipeline, such that all results in this work are generated without any user intervention. This is rigorously tested on a large suite of simulated images, assessing its performance on a broad range of lens profiles, source morphologies, and lensing geometries. The method's performance is excellent, with accurate light, mass, and source profiles inferred for data sets representative of both existing Hubble imaging and future Euclid wide-field observations.}, -archivePrefix = {arXiv}, -arxivId = {1708.07377}, -author = {Nightingale, J W and Dye, S and Massey, Richard J}, -doi = {10.1093/mnras/sty1264}, -eprint = {1708.07377}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxy: structure,Gravitational lensing,Methods: data analysis}, -number = {4}, -pages = {4738--4784}, -title = {{AutoLens: Automated modeling of a strong lens's light, mass, and source}}, -url = {https://academic.oup.com/mnras/article/478/4/4738/5001434}, -volume = {478}, -year = {2018} -} -@article{Ferrero2017, -abstract = {The Tully-Fisher relation (TFR) links the stellar mass of a disc galaxy, Mstr, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling (M ∝ V3) of dark matter haloes, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to deviate substantially from a single power law and to evolve rapidly with redshift. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of $\Lambda$ cold dark matter ($\Lambda$CDM) cosmological simulations. Matching both relations requires disc sizes to satisfy constraints given by the concentration of haloes and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. $\Lambda$CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1607.03100}, -author = {Ferrero, Ismael and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw2691}, -eprint = {1607.03100}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {4}, -pages = {4736--4746}, -title = {{Size matters: Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE}}, -volume = {464}, -year = {2017} -} -@article{Algorry2016, -abstract = {We examine the properties of barred disc galaxies in a $\Lambda$CDM cosmological hydrodynamical simulation from the EAGLE project. Our study follows the formation of 269 discs identified at z = 0 in the stellar mass range 10.6 < logM∗/M⊙ < 11. These discs show a wide range of bar strengths, from unbarred discs (≈60 per cent) to weak bars (≈20 per cent) and to strongly barred systems (≈20 per cent). Bars in these systems develop after redshift ≈1.3, on timescales that depend sensitively on the strength of the pattern. Strong bars develop relatively quickly (in a few Gyr, or roughly∼10 disc rotation periods) in systems that are disc dominated, gas poor, and have declining rotation curves.Weak bars develop more slowly in systems where the disc is less gravitationally important, and are still growing at z = 0. Unbarred galaxies are comparatively gas-rich discs whose rotation speeds do not exceed the maximum circular velocity of the haloes they inhabit. Bar lengths compare favourably with observations, ranging from 0.2 to 0.8 times the radius containing 90 per cent of the stars. Bars slow down remarkably quickly as they grow, causing the inner regions of the surrounding dark halo to expand. At z = 0 strong bars in simulated galaxies have corotation radii roughly 10 times the bar length. Such slow bars are inconsistent with the few cases where pattern speeds have been measured or inferred observationally, a discrepancy that, if confirmed, might prove a challenge for disc galaxy formation in $\Lambda$CDM.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1609.05909}, -author = {Algorry, David G. and Navarro, Julio F. and Abadi, Mario G. and Sales, Laura V. and Bower, Richard G. and Crain, Robert A. and Vecchia, Claudio Dalla and Frenk, Carlos S. and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx1008}, -eprint = {1609.05909}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Algorry et al. - 2017 - Barred galaxies in the EAGLE cosmological hydrodynamical simulation(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Kinematics and dynamics,Galaxy: Disc,Galaxy: Formation,Galaxy: Structure}, -number = {1}, -pages = {1054--1064}, -title = {{Barred galaxies in the EAGLE cosmological hydrodynamical simulation}}, -url = {http://arxiv.org/abs/1609.05909%0Ahttp://dx.doi.org/10.1093/mnras/stx1008}, -volume = {469}, -year = {2017} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Leauthaud2017, -abstract = {We present high signal-to-noise galaxy-galaxy lensing measurements of the BOSS CMASS sample using 250 square degrees of weak lensing data from CFHTLenS and CS82. We compare this signal with predictions from mock catalogs trained to match observables including the stellar mass function and the projected and two dimensional clustering of CMASS. We show that the clustering of CMASS, together with standard models of the galaxy-halo connection, robustly predicts a lensing signal that is 20-40{\%} larger than observed. Detailed tests show that our results are robust to a variety of systematic effects. Lowering the value of {\$}S{\_}{\{}\backslashbackslashrm 8{\}}=\backslashbackslashsigma{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm 8{\}} \backslashbackslashsqrt{\{}\backslash{\{}{\}}\backslashbackslashOmega{\{}\backslash{\_}{\}}{\{}\backslash{\{}{\}}\backslashbackslashrm m{\{}\backslash{\}}{\}}/0.3{\{}\backslash{\}}{\}}{\$} compared to Planck2015 reconciles the lensing with clustering. However, given the scale of our measurement ({\$}r{\textless}10{\$} {\$}h{\^{}}{\{}-1{\}}{\$} Mpc), other effects may also be at play and need to be taken into consideration. We explore the impact of baryon physics, assembly bias, massive neutrinos, and modifications to general relativity on {\$}\backslashbackslashDelta\backslashbackslashSigma{\{}\backslash{\$}{\}} and show that several of these effects may be non-negligible given the precision of our measurement. Disentangling cosmological effects from the details of the galaxy-halo connection, the effects of baryons, and massive neutrinos, is the next challenge facing joint lensing and clustering analyses. This is especially true in the context of large galaxy samples from Baryon Acoustic Oscillation surveys with precise measurements but complex selection functions.}, -archivePrefix = {arXiv}, -arxivId = {1611.08606}, -author = {Leauthaud, Alexie and Saito, Shun and Hilbert, Stefan and Barreira, Alexandre and More, Surhud and White, Martin and Alam, Shadab and Behroozi, Peter and Bundy, Kevin and Coupon, Jean and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Mandelbaum, Rachel and Miller, Lance and Moraes, Bruno and Pereira, Maria E S and Rodr{\'{i}}guez-Torres, Sergio A and Schmidt, Fabian and Shan, Huan Yuan and Viel, Matteo and Villaescusa-Navarro, Francisco}, -doi = {10.1093/mnras/stx258}, -eprint = {1611.08606}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {3}, -pages = {3024--3047}, -title = {{Lensing is low: Cosmology, galaxy formation or new physics?}}, -volume = {467}, -year = {2017} -} -@article{denBrok2011, -abstract = {Using deep, high-spatial-resolution imaging from the Hubble Space Telescope/Advanced Camera for Surveys (HST/ACS) Coma Cluster Treasury Survey, we determine colour profiles of early-type galaxies in the Coma cluster. From 176 galaxies brighter than MF814W(AB)=-15mag that are either spectroscopically confirmed members of Coma or identified by eye as likely members from their low surface brightness, data are provided for 142 early-type galaxies. Typically, colour profiles are linear against log(R), sometimes with a nuclear region of distinct, often bluer colour associated with nuclear clusters. Colour gradients are determined for the regions outside the nuclear components. We find that almost all colour gradients are negative, both for elliptical and for lenticular galaxies. Most likely, earlier studies that report positive colour gradients in dwarf galaxies are affected by the bluer colours of the nuclear clusters, underlining that high-resolution data are essential to disentangle the colour properties of the different morphological components in galaxies. Colour gradients of dwarf galaxies form a continuous sequence with those of elliptical galaxies, becoming shallower towards fainter magnitudes. Interpreting the colours as metallicity tracers, our data suggest that dwarfs as well as giant early-type galaxies in the Coma cluster are less metal rich in their outer parts. We do not find evidence for environmental influence on the gradients, although we note that most of our galaxies are found in the central regions of the cluster. For a subset of galaxies with known morphological types, S0 galaxies have less steep gradients than elliptical galaxies. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1103.1218}, -author = {{Den Brok}, M. and Peletier, R. F. and Valentijn, E. A. and Balcells, M. and Carter, D. and Erwin, P. and Ferguson, H. C. and Goudfrooij, P. and Graham, A. W. and Hammer, D. and Lucey, J. R. and Trentham, N. and Guzm{\'{a}}n, R. and Hoyos, C. and {Verdoes Kleijn}, G. and Jogee, S. and Karick, A. M. and Marinova, I. and Mouhcine, M. and Weinzirl, T.}, -doi = {10.1111/j.1365-2966.2011.18606.x}, -eprint = {1103.1218}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: individual: Coma,Galaxies: dwarf,Galaxies: elliptical and lenticular, cD,Galaxies: structure}, -number = {4}, -pages = {3052--3070}, -title = {{The HST/ACS Coma Cluster Survey - VI. Colour gradients in giant and dwarf early-type galaxies}}, -volume = {414}, -year = {2011} -} -@article{Christensen2014, -abstract = {We present a detailed comparison between the photometric properties of the bulges of two simulated galaxies and those of a uniform sample of observed galaxies. This analysis shows that the simulated galaxies have bulges with realistic surface brightnesses for their sizes and magnitude. These two field disc galaxies have rotational velocities ̃100 km s-1 and were integrated to a redshift of zero in a fully cosmological $\delta$ cold dark matter context as part of high-resolution smoothed particle hydrodynamic simulations. We performed bulge- disc decompositions of the galaxies using artificial observations, in order to conduct a fair comparison to observations. We also dynamically decomposed the galaxies and compared the star formation histories of the bulges to those of the entire galaxies. These star formation histories showed that the bulges were primarily formed before z = 1 and during periods of rapid star formation. Both galaxies have large amounts of early star formation, which is likely related to the relatively high bulge-to-disc ratios also measured for them. Unlike almost all previous cosmological simulations, the realistically concentrated bulges of these galaxies do not lead to unphysically high rotational velocities, causing them to naturally lie along the observed Tully-Fisher relation. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1402.2702}, -author = {Christensen, C. R. and Brooks, A. M. and Fisher, D. B. and Governato, F. and McCleary, J. and Quinn, T. R. and Shen, S. and Wadsley, J.}, -doi = {10.1093/mnrasl/slu020}, -eprint = {1402.2702}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Christensen et al. - 2014 - Simulating disc galaxy bulges that are consistent with observed scaling relations.pdf:pdf}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Bulges,Formation,Galaxies,Methods,Numerical,Spiral,Structure}, -number = {1}, -pages = {1--6}, -title = {{Simulating disc galaxy bulges that are consistent with observed scaling relations}}, -volume = {440}, -year = {2014} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1{\textless}z{\textless}3. Our analysis is based on a bulge-disk decomposition of 396 galaxies with Mstar{\textgreater}10{\^{}}11 Msolar from the CANDELS WFC3/IR imaging within the COSMOS and UKIDSS UDS survey fields. We find that, by modelling the H(160) image of each galaxy with a combination of a de Vaucouleurs bulge (Sersic index n=4) and an exponential disk (n=1), we can then lock all derived morphological parameters for the bulge and disk components, and successfully reproduce the shorter-wavelength J(125), i(814), v(606) HST images simply by floating the magnitudes of the two components. This then yields sub-divided 4-band HST photometry for the bulge and disk components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information we are able to properly determine the masses and star-formation rates for the bulge and disk components, and find that: i) from z=3 to z=1 the galaxies move from disk-dominated to increasingly bulge-dominated, but very few galaxies are pure bulges/ellipticals by z=1; ii) while most passive galaxies are bulge-dominated, and most star-forming galaxies disk-dominated, 18+/-5{\%} of passive galaxies are disk-dominated, and 11+/-3{\%} of star-forming galaxies are bulge-dominated, a result which needs to be explained by any model purporting to connect star-formation quenching with morphological transformations; iii) there exists a small but significant population of pure passive disks, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a{\$\sim${}}0.7); iv) flatter/larger disks re-emerge at the highest star-formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface-density for star-formation activity.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1405.1736v1}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {arXiv:1405.1736v1}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.1736}, -volume = {444}, -year = {2014} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series that re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science data base, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies. This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution that limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ('encounter-driven') rings (such as ring and polar ring galaxies) are recognized in less than 1 per cent of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless} $\sigma$∗ {\textless} 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Minka2009, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture models is not well captured by factor graphs unless the entire mixture is represented by one factor, because the message equations have a containment structure. Gates capture this containment structure graphically, allowing both the independences and the message-passing equations for a model to be readily visualized. Different variational approximations for mixture models can be understood as different ways of drawing the gates in a model. We present general equations for expectation propagation and variational message passing in the presence of gates.}, -author = {Minka, Tom and Winn, John}, -doi = {10.5790/hongkong/9789888083091.003.0088}, -isbn = {9781605609492}, -issn = {0018702X}, -journal = {Advances in Neural Information Processing Systems 21 - Proceedings of the 2008 Conference}, -pages = {1073--1080}, -title = {{Gates}}, -year = {2009} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Amorisco2017, -abstract = {The accreted component of stellar halos is composed of the contributions of several satellites, falling onto their host with their different masses, at different times, on different orbits. This work uses a suite of idealised, collisionless N-body simulations of minor mergers and a particle tagging technique to understand how these different ingredients shape each contribution to the accreted halo, in both density and kinematics. I find that more massive satellites deposit their stars deeper into the gravitational potential of the host, with a clear segregation enforced by dynamical friction. Earlier accretion events contribute more to the inner regions of the halo; more concentrated subhaloes sink deeper through increased dynamical friction. The orbital circularity of the progenitor at infall is only important for low-mass satellites: dynamical friction efficiently radialises the most massive minor mergers erasing the imprint of the infall orbit for satellite-to-host virial mass ratios {\$}\backslashgtrsim1/20{\$}. The kinematics of the stars contributed by each satellite is also ordered with satellite mass: low-mass satellites contribute fast-moving populations, in both ordered rotation and radial velocity dispersion. In turn, contributions by massive satellites have lower velocity dispersion and lose their angular momentum to dynamical friction, resulting in a strong radial anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {1511.08806}, -author = {Amorisco, N C}, -doi = {10.1093/mnras/stw2229}, -eprint = {1511.08806}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {evolution,galaxies,galaxy,halo,interaction,kinematics and dynamics,structure}, -number = {3}, -pages = {2882--2895}, -title = {{Contributions to the accreted stellar halo: an atlas of stellar deposition}}, -url = {http://arxiv.org/abs/1511.08806%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2229}, -volume = {464}, -year = {2015} -} -@article{Greene2012, -abstract = {We use the Mitchell Spectrograph (formerly VIRUS-P) on the McDonald Observatory 2.7m Harlan J. Smith Telescope to search for the chemical signatures of massive elliptical galaxy assembly. The Mitchell Spectrograph is an integral-field spectrograph with a uniquely wide field of view (107x107 sq arcsec), allowing us to achieve remarkably high signal-to-noise ratios of {\$\sim${}}20-70 per pixel in radial bins of 2-2.5 times the effective radii of the eight galaxies in our sample. Focusing on a sample of massive elliptical galaxies with stellar velocity dispersions sigma* {\textgreater}150 km/s, we study the radial dependence in the equivalent widths (EWs) of key metal absorption lines. By twice the effective radius, the Mgb EWs have dropped by {\$\sim${}}50{\%}, and only a weak correlation between sigma* and Mgb EW remains. The Mgb EWs at large radii are comparable to those seen in the centers of elliptical galaxies that are approximately an order of magnitude less massive. We find that the well-known metallicity gradients often observed within an effective radius continue smoothly to 2.5R{\_}e, while the abundance ratio gradients remain flat. Much like the halo of the Milky Way, the stellar halos of our galaxies have low metallicities and high alpha-abundance ratios, as expected for very old stars formed in small stellar systems. Our observations support a picture in which the outer parts of massive elliptical galaxies are built by the accretion of much smaller systems whose star formation history was truncated at early times.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -volume = {786}, -year = {2014} -} -@article{Greene2017, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Siverd2009, -abstract = {We identify, categorize, and quantify alignment effects among host and satellite galaxies using a spectroscopically-confirmed, low-redshift (z{\textless}0.23) galaxy sample from the Sloan Digital Sky Survey Data Release 6. Consistent with other recent findings, we find that satellite galaxies (SGs) of red, centrally concentrated (elliptical) host galaxies (HGs) with radial velocity separation |Delta{\_}V|{\textless}600 km/s preferentially reside near the projected major axes of their HGs. Among these, this preference is strongest for highly concentrated, red SGs. We find that fractional anisotropy increases with decreasing $\backslash$Delta{\_}V and Delta{\_}R and is nearly 40{\%} greater among the closest SGs (Delta{\_}R{\textless}250 kpc/h) relative to more distant (Delta{\_}R{\textgreater}500 kpc/h) SGs. For highly concentrated SGs at small ({\textless}300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to {\textless}15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby ({\textless}40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ({\$\sim${}}3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R J and Ryden, B S and Gaudi, B S}, -eprint = {0903.2264}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of supermassive black hole (SMBH) formation and evolution is used, as in Tremmel et al., allowing us to explicitly follow the SMBH dynamics at the centre of galaxies. A high SIDM constant cross-section is chosen, $\sigma$ = 10 cm2gr-1, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in cold dark matter (CDM), with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals, the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80 per cent of the SMBH population is offcentred in the SIDM case, as opposed to the CDM case in which $\sim$90 per cent of SMBHs have reached their host's centre. SMBHs are found as far as $\sim$9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction time-scale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in core stalling. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to the SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Di Cintio et al. - 2017 - A rumble in the dark Signatures of self-interacting dark matter in supermassive black hole dynamics and gal(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}$\backslash${\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashsigma{\$} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and Gonzalez, Pablo G Perez and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -title = {{CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z{\$\sim${}}2}}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -year = {2017} -} -@article{Ritondale2019a, -abstract = {We use a sample of 17 strong gravitational lens systems from the BELLS GALLERY survey to quantify the amount of low-mass dark matter haloes within the lensing galaxies and along their lines of sight, and to constrain the properties of dark matter. Based on a detection criterion of 10$\sigma$, we report no significant detection in any of the lenses. Using the sensitivity function at the 10$\sigma$ level, we have calculated the predicted number of detectable cold dark matter (CDM) line-of-sight haloes to be $\mu$l = 1.17 ± 1.08, in agreement with our null detection. Assuming a detection sensitivity that improved to the level implied by a 5$\sigma$ threshold, the expected number of detectable line-of-sight haloes rises to $\mu$l = 9.0 ± 3.0. Whilst the current data find zero detections at this sensitivity level (which has a probability of P 5$\sigma$CDM (n det = 0) = 0.0001 and would be in strong tension with the CDM framework), we find that such a low-detection threshold leads to many spurious detections and non-detections and therefore the current lack of detections is unreliable and requires data with improved sensitivity. Combining this sample with a subsample of 11 SLACS lenses, we constrain the half-mode mass to be log (M hm ) < 12.26 at the 2$\sigma$ level. The latter is consistent with resonantly produced sterile neutrino masses m s < 0.8 keV at any value of the lepton asymmetry at the 2$\sigma$ level.}, -archivePrefix = {arXiv}, -arxivId = {1811.03627}, -author = {Ritondale, E. and Vegetti, S. and Despali, G. and Auger, M. W. and Koopmans, L. V.E. and McKean, J. P.}, -doi = {10.1093/mnras/stz464}, -eprint = {1811.03627}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ritondale et al. - 2019 - Low-mass halo perturbations in strong gravitational lenses at redshift z $\sim$ 0.5 are consistent with CDM.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Gravitational lensing,Haloes – galaxies,Strong – galaxies,Structure – darkmatter}, -number = {2}, -pages = {2179--2193}, -title = {{Low-mass halo perturbations in strong gravitational lenses at redshift z $\sim$ 0.5 are consistent with CDM}}, -volume = {485}, -year = {2019} -} -@article{Dominika2016, -abstract = {Spectral features introduced by instrumental chromaticity of radio interferometers have the potential to negatively impact the ability to perform Epoch of Reionisation (EoR) and Cosmic Dawn (CD) science using the redshifted neutral hydrogen emission line from the early Universe. We describe instrument calibration choices that influence the spectral characteristics of the science data, and assess their impact on EoR statistical and tomographic experiments. Principally, we consider the intrinsic spectral response of the receiving antennas, embedded within a complete frequency-dependent primary beam response, and frequency-dependent instrument sampling. We assess different options for bandpass calibration. The analysis is applied to the proposed SKA1-Low EoR/CD experiments. We provide tolerances on the smoothness of the SKA station primary beam bandpass, to meet the scientific goals of statistical and tomographic (imaging) EoR programs. Two calibration strategies are tested: (1) fitting of each fine channel independently, and (2) fitting of an nth-order polynomial for each $\sim$1$\sim$MHz coarse channel with (n+1)th-order residuals (n=2,3,4). Strategy (1) leads to uncorrelated power in the 2D power spectrum proportional to the thermal noise power, thereby reducing the overall array sensitivity. Strategy (2) leads to correlated residuals from the fitting, and residual signal power with (n+1)th-order curvature. For the residual power to be less than the thermal noise, the fractional amplitude of a fourth-order term in the bandpass across a single coarse channel must be <2.5% (50$\sim$MHz), <0.5% (150$\sim$MHz), <0.8% (200$\sim$MHz). The tomographic experiment places stringent constraints on phase residuals in the bandpass. We find that the root-mean-square variability over all stations of the change in phase across any fine channel (4.578$\sim$kHz) should not exceed 0.2 degrees.}, -archivePrefix = {arXiv}, -arxivId = {1604.03273}, -author = {Trott, Cathryn M. and Wayth, Randall B.}, -doi = {10.1017/pas.2016.xxx}, -eprint = {1604.03273}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Trott, Wayth - 2016 - Australian Aboriginal Astronomy and Navigation arXiv1607.02215v1.pdf:pdf}, -issn = {14486083}, -journal = {arXiv preprint arXiv: {\ldots}}, -keywords = {aboriginal astronomy,ethnoastronomy,history of astronomy}, -number = {3}, -pages = {15}, -title = {{Australian Aboriginal Astronomy and Navigation arXiv:1607.02215v1}}, -url = {http://arxiv.org/abs/1604.03273}, -volume = {447}, -year = {2016} -} -@article{Liao2016, -abstract = {The standard galaxy formation theory assumes that baryons and dark matter are initially well mixed before becoming segregated due to radiative cooling. We use non-radiative hydrodynamical simulations to explicitly examine this assumption and find that baryons and dark matter can also be segregated due to different characteristics of gas and dark matter during the buildup of the halo. As a result, baryons in many haloes do not originate from the same Lagrangian region as the dark matter. When using the fraction of corresponding dark matter and gas particles in the initial conditions (the 'paired fraction') as a proxy of the dark matter and gas segregation strength of a halo, on average about 25 per cent of the baryonic and dark matter of the final halo are segregated in the initial conditions. This is at odds with the assumption of the standard galaxy formation model. A consequence of this effect is that the baryons and dark matter of the same halo initially experience different tidal torques and thus their angular momentum vectors are often misaligned. The degree of the misalignment is largely preserved during later halo assembly and can be understood with the tidal torque theory. The result challenges the precision of some semi-analytical approaches that utilize dark matter halo merger trees to infer properties of gas associated with dark matter haloes.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.07592}, -author = {Liao, Shihong and Gao, Liang and Frenk, Carlos S and Guo, Qi and Wang, Jie}, -doi = {10.1093/mnras/stx1391}, -eprint = {1610.07592}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {2}, -pages = {2262--2269}, -title = {{The segregation of baryons and dark matter during halo assembly}}, -url = {http://arxiv.org/abs/1610.07592}, -volume = {470}, -year = {2017} -} -@article{Eales2015, -abstract = {Using results from the Herschel Astrophysical Terrahertz Large-Area Survey (H-ATLAS) and the Galaxy and Mass Assembly (GAMA) project, we show that, for galaxy masses above ≃ 108M⊙, 51 per cent of the stellar mass-density in the local Universe is in earlytype galaxies (ETGs; S{\'{e}}rsic n > 2.5) while 89 per cent of the rate of production of stellar mass-density is occurring in late-type galaxies (LTGs; S{\'{e}}rsic n < 2.5). From this zeroredshift benchmark, we have used a calorimetric technique to quantify the importance of the morphological transformation of galaxies over the history of the Universe. The extragalactic background radiation contains all the energy generated by nuclear fusion in stars since the big bang. By resolving this background radiation into individual galaxies using the deepest farinfrared survey with the Herschel Space Observatory and a deep near-infrared/optical survey with the Hubble Space Telescope (HST), and using measurements of the S{\'{e}}rsic index of these galaxies derived from the HST images, we estimate that ≃ 83 per cent of the stellarmass-density formed over the history of the Universe occurred in LTGs. The difference between this value and the fraction of the stellar mass-density that is in LTGs today implies there must have been a major transformation of LTGs into ETGs after the formation of most of the stars.}, -archivePrefix = {arXiv}, -arxivId = {1506.05466}, -author = {Eales, Stephen and Fullard, Andrew and Allen, Matthew and Smith, M. W.L. and Baldry, Ivan and Bourne, Nathan and Clark, C. J.R. and Driver, Simon and Dunne, Loretta and Dye, Simon and Graham, Alister W. and Ibar, Edo and Hopkins, Andrew and Ivison, Rob and Kelvin, Lee S. and Maddox, Steve and Maraston, Claudia and Robotham, Aaron S.G. and Smith, Dan and Taylor, Edward N. and Valiante, Elisabetta and {Van Der Werf}, Paul and Baes, Maarten and Brough, Sarah and Clements, David and Cooray, Asantha and Gomez, Haley and Loveday, Jon and Phillipps, Steven and Scott, Douglas and Serjeant, Steve}, -doi = {10.1093/mnras/stv1300}, -eprint = {1506.05466}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: star formation}, -number = {4}, -pages = {3489--3507}, -title = {{H-ATLAS/GAMA: Quantifying the morphological evolution of the galaxy population using cosmic calorimetry}}, -volume = {452}, -year = {2015} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism, which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio (M/L) and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R, z) and characterized by the classic anisotropy parameter. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters ($\beta$z and the inclination), the models generally provide remarkably good descriptions of the shape of the first (V) and second () velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the dynamical structure of these objects. With the observationally motivated assumption that $\beta$z ≳ 0, the method is able to recover the inclination. The technique can be used to determine the dynamical M/L and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modelling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy and multiple kinematic components. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Greene2013, -abstract = {We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions $\sigma$* ≳ 150 km s-1. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼ 10 Gyr), relatively metal-poor ([Fe/H] ≈ -0.5), and $\alpha$-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z ≈ 1.5-2). {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1308.2682}, -author = {Greene, Jenny E and Murphy, Jeremy D and Graves, Genevieve J and Gunn, James E and Raskutti, Sudhir and Comerford, Julia M and Gebhardt, Karl}, -doi = {10.1088/0004-637X/776/2/64}, -eprint = {1308.2682}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: abundances,galaxies: elliptical and lenticular,galaxies: evolution}, -number = {2}, -title = {{The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius}}, -volume = {776}, -year = {2013} -} -@article{Weijmans2014, -abstract = {We use the ATLAS3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation $\sigma$q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and $\sigma$q = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrizations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P T and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F and Davies, Roger L and Davis, Timothy A and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular,Galaxies,Structure,cD- galaxies}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Tinker2013, -abstract = {We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z=[0.2,1.0]. For massive galaxies, M*{\textgreater}{\$\sim${}}10{\^{}}10.6 Msol, our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z=1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M*{\$\sim${}}10{\^{}}10 Msol, the fraction of central galaxies on the red sequence increases by a factor of ten over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z=1 to z=0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency.}, -archivePrefix = {arXiv}, -arxivId = {1308.2974}, -author = {Tinker, Jeremy L and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H}, -doi = {10.1088/0004-637X/778/2/93}, -eprint = {1308.2974}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: halos}, -number = {2}, -title = {{Evolution of the stellar-to-dark matter relation: Separating star-forming and passive galaxies from z = 1 to 0}}, -volume = {778}, -year = {2013} -} -@article{Kormendy2015a, -abstract = {Bulge components of disc galaxies are the high-density centers interior to their outer discs. Once thought to be equivalent to elliptical galaxies, their observed properties and formation histories turn out to be richer and more varied than those of ellipticals. This book reviews progress in many areas of bulge studies. Two advances deserve emphasis: (1) Observations divide bulges into "classical bulges" that look indistinguishable from ellipticals and "pseudobulges" that are discier and (except in S0s) more actively star-forming than are ellipticals. Classical bulges and ellipticals are thought to form by major galaxy mergers. Discy pseudobulges are a product of the slow ("secular") evolution of galaxy discs. Nonaxisymmetries such as bars and oval distortions transport some disc gas toward the center, where it starbursts and builds a dense central component that is discier in structure than are classical bulges. Secular evolution explains many regular structures (e.g., rings) seen in galaxy discs. It is a new area of galaxy evolution work that complements hierarchical clustering. (2) Studies of high-redshift galaxies reveal that their discs are so gas-rich that they are violently unstable to the formation of mass clumps that sink to the center and merge. This is an alternative channel for the formation of classical bulges. This chapter summarizes big-picture successes and unsolved problems in the formation of bulges and ellipticals and their coevolution (or not) with supermassive black holes. I present an observer's perspective on simulations of cold dark matter galaxy formation including baryonic physics. Our picture of the quenching of star formation is becoming general and secure at redshifts z < 1. I conclude with a list of major uncertainties and problems. The biggest challenge is to produce realistic bulgesCellipticals and realistic discs that overlap over a factor of >1000 in mass but that differ from each other as we observe over that whole range. A related difficulty is how hierarchical clustering makes so many giant, bulgeless galaxies in field but not cluster environments. I present arguments that we rely too much on star-formation feedback and AGN feedback to solve these challenges.}, -archivePrefix = {arXiv}, -arxivId = {1504.03330}, -author = {Kormendy, John}, -doi = {10.1007/978-3-319-19378-6_16}, -eprint = {1504.03330}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kormendy - 2015 - Elliptical galaxies and bulges of disc galaxies Summary of progress and outstanding issues.pdf:pdf}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {431--477}, -title = {{Elliptical galaxies and bulges of disc galaxies: Summary of progress and outstanding issues}}, -volume = {418}, -year = {2015} -} -@article{Rhodes2001, -abstract = {Weak lensing by large-scale structure provides a unique method to directly measure matter fluctuations in the universe and has recently been detected from the ground. Here we report the first detection of this ``cosmic shear'' based on space-based images. The detection was derived from the Hubble Space Telescope (HST) Survey Strip (or ``Groth Strip''), a 4'x42' set of 28 contiguous Wide Field Planetary Camera 2 (WFPC2) pointings with I〈27. The small size of the HST point-spread function affords both a lower statistical noise and a much weaker sensitivity to systematic effects, a crucial limiting factor of cosmic shear measurements. Our method and treatment of systematic effects were discussed in an earlier paper. We measure an rms shear of 1.8{\%} on the WFPC2 chip scale (1.27′), in agreement with the predictions of cluster-normalized cold dark matter (CDM) models. Using a maximum likelihood analysis, we show that our detection is significant at the 99.5{\%} confidence level (CL) and measure the normalization of the matter power spectrum to be $\sigma${\textless}SUB{\textgreater}8{\textless}/SUB{\textgreater}$\Omega${\textless}SUP{\textgreater}0.48{\textless}/SUP{\textgreater}{\textless}SUB{\textgreater}m{\textless}/SUB{\textgreater}= 0.51{\textless}SUP{\textgreater}+0.14{\textless}/SUP{\textgreater}{\textless}SUB{\textgreater}-0.17{\textless}/SUB{\textgreater}, in a $\Lambda$CDM universe. These 68{\%} CL errors include (Gaussian) cosmic variance, systematic effects, and the uncertainty in the redshift distribution of the background galaxies. The signal comes primarily from the chip scale (1.27′) with gradually decreasing contributions up to roughly 10'. Our result is consistent with earlier lensing measurements from the ground and with the normalization derived from cluster abundance. We discuss how our measurement can be improved with the analysis of a large number of independent WFPC2 fields.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0101213}, -author = {Rhodes, Jason and Refregier, Alexandre and Groth, Edward J}, -doi = {10.1086/320336}, -eprint = {0101213}, -issn = {0004637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L85----L88}, -primaryClass = {astro-ph}, -title = {{Detection of Cosmic Shear with the [ITAL]Hubble Space Telescope[/ITAL] Survey Strip}}, -volume = {552}, -year = {2001} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within {\$\sim${}}30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M sun and a factor of 3 at 107 M sun. The most massive subhalos with 1010 M sun survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1138?key=crossref.6ebb2a01dc7b45f1fa5c66089a37542b}, -volume = {709}, -year = {2010} -} -@article{Devour2017, -abstract = {Accurate measurement of galaxy structures is a prerequisite for quantitative investigation of galaxy properties or evolution. Yet, the impact of galaxy inclination and dust on commonly used metrics of galaxy structure is poorly quantified. We use infrared data sets to select inclination-independent samples of disc and flattened elliptical galaxies. These samples show strong variation in S\'{e}rsic index, concentration, and half-light radii with inclination. We develop novel inclination-independent galaxy structures by collapsing the light distribution in the near-infrared on to the major axis, yielding inclination-independent `linear' measures of size and concentration. With these new metrics we select a sample of Milky Way analogue galaxies with similar stellar masses, star formation rates, sizes and concentrations. Optical luminosities, light distributions, and spectral properties are all found to vary strongly with inclination: When inclining to edge-on, $r$-band luminosities dim by $>$1 magnitude, sizes decrease by a factor of 2, `dust-corrected' estimates of star formation rate drop threefold, metallicities decrease by 0.1 dex, and edge-on galaxies are half as likely to be classified as star forming. These systematic effects should be accounted for in analyses of galaxy properties.}, -archivePrefix = {arXiv}, -arxivId = {1702.06528}, -author = {Devour, Brian M. and Bell, Eric F.}, -doi = {10.1093/mnrasl/slx021}, -eprint = {1702.06528}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Devour, Bell - 2017 - Revealing strong bias in common measures of galaxy properties using new inclination-independent structures(2).pdf:pdf}, -issn = {1745-3925}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {dust,extinction,galaxies,general,photometric,techniques}, -number = {1}, -pages = {L31--L35}, -pmid = {18462818}, -title = {{Revealing strong bias in common measures of galaxy properties using new inclination-independent structures}}, -url = {http://arxiv.org/abs/1702.06528%0Ahttp://dx.doi.org/10.1093/mnrasl/slx021}, -volume = {468}, -year = {2017} -} -@article{Ma2014, -abstract = {Massive early-type galaxies represent the modern day remnants of the earliest major star formation episodes in the history of the universe. These galaxies are central to our understanding of the evolution of cosmic structure, stellar populations, and supermassive black holes, but the details of their complex formation histories remain uncertain. To address this situation, we have initiated the MASSIVE Survey, a volume-limited, multi-wavelength, integral-field spectroscopic (IFS) and photometric survey of the structure and dynamics of the ∼100 most massive early-type galaxies within a distance of 108 Mpc. This survey probes a stellar mass range M∗ ≳ 1011.5 M⊙ and diverse galaxy environments that have not been systematically studied to date. Our wide-field IFS data cover about two effective radii of individual galaxies, and for a subset of them, we are acquiring additional IFS observations on sub-arcsecond scales with adaptive optics. We are also acquiring deep K-band imaging to trace the extended halos of the galaxies and measure accurate total magnitudes. Dynamical orbit modeling of the combined data will allow us to simultaneously determine the stellar, black hole, and dark matter halo masses. The primary goals of the project are to constrain the black hole scaling relations at high masses, investigate systematically the stellar initial mass function and dark matter distribution in massive galaxies, and probe the late-time assembly of ellipticals through stellar population and kinematical gradients. In this paper, we describe the MASSIVE sample selection, discuss the distinct demographics and structural and environmental properties of the selected galaxies, and provide an overview of our basic observational program, science goals and early survey results.}, -archivePrefix = {arXiv}, -arxivId = {1407.1054}, -author = {Ma, Chung Pei and Greene, Jenny E and McConnell, Nicholas and Janish, Ryan and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/795/2/158}, -eprint = {1407.1054}, -isbn = {0000000000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content,galaxies: structure}, -number = {2}, -pages = {158}, -pmid = {28562576}, -title = {{The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...795..158M}, -volume = {795}, -year = {2014} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter (CDM) galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes possess a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a $\Lambda$CDM universe. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R and Eke, Vincent R and Frenk, Carlos S and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{2001er, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Tinker2016, -abstract = {We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen etal (2012) clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of Mgal for galaxies with logMgal{\textgreater}=11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma{\_}logM. Using this approach, we find sigma{\_}logM=0.18{\^{}}{\{}+0.01{\}}{\_}{\{}-0.02{\}}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L and Brownstein, Joel R and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {121}, -title = {{The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -volume = {839}, -year = {2017} -} -@article{Bower:2016aa, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of {\$\sim${}}1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -month = {jul}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Metcalf2018, -abstract = {Large scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100,000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. (abridged)}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R Benton and Meneghetti, M and Avestruz, Camille and Bellagamba, Fabio and Bom, Cl{\'{e}}cio R and Bertin, Emmanuel and Cabanac, R{\'{e}}mi and Courbin, F and Davies, Andrew and Decenci{\`{e}}re, Etienne and Flamary, R{\'{e}}mi and Gavazzi, Raphael and Geiger, Mario and Hartley, Philippa and Huertas-Company, Marc and Jackson, Neal and Jullo, Eric and Kneib, Jean-Paul and Koopmans, L{\'{e}}on V E and Lanusse, Fran{\c{c}}ois and Li, Chun-Liang and Ma, Quanbin and Makler, Martin and Li, Nan and Lightman, Matthew and Petrillo, Carlo Enrico and Serjeant, Stephen and Sch{\"{a}}fer, Christoph and Sonnenfeld, Alessandro and Tagore, Amit and Tortora, Crescenzo and Tuccillo, Diego and Valent{\'{i}}n, Manuel B and Velasco-Forero, Santiago and Kleijn, Gijs A Verdoes and Vernardos, Georgios}, -doi = {10.1051/0004-6361/201832797}, -eprint = {1802.03609}, -title = {{The Strong Gravitational Lens Finding Challenge}}, -url = {http://arxiv.org/abs/1802.03609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201832797}, -year = {2018} -} -@article{Mendez-Abreu2010a, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Shajib2022, -abstract = {The importance of alternative methods to measure the Hubble constant such as time-delay cosmography is highlighted by the recent Hubble tension. It is paramount to thoroughly investigate and rule out systematic biases in all measurement methods before we can accept new physics as the source of this tension. In this study, we perform a check for systematic biases in the lens modelling procedure of time-delay cosmography by comparing independent and blind time-delay predictions of the system WGD 2038$-$4008 from two teams using two different software programs: Glee and lenstronomy. The predicted time delays from both teams incorporate the stellar kinematics of the deflector and the external convergence from line-of-sight structures. The unblinded time-delay predictions from the two teams agree within $1.2\sigma$ implying that once the time delay is measured the inferred Hubble constant will also be mutually consistent. However, there is a $\sim$4$\sigma$ discrepancy between the power-law model slope and external shear, which is a significant discrepancy at the level of lens models before incorporating the stellar kinematics and the external convergence. We identify the difference in the reconstructed point spread function (PSF) to be the source of this discrepancy. If the same reconstructed PSF is used by both teams, then we achieve excellent agreement within $\sim$0.6$\sigma$, indicating that potential systematics stemming from source reconstruction algorithms and investigator choices are well under control. We recommend future studies to supersample the PSF as needed and marginalize over multiple algorithms/realizations for the PSF reconstruction to mitigate the systematic associated with the PSF. A future study will measure the time delays of the system WGD 2038$-$4008 and infer the Hubble constant based on our mass models.}, -archivePrefix = {arXiv}, -arxivId = {2202.11101}, -author = {Shajib, A. J. and Wong, K. C. and Birrer, S. and Suyu, S. H. and Treu, T. and Buckley-Geer, E. and Lin, H. and Rusu, C. E. and Poh, J. and Palmese, A. and Agnello, A. and Auger, M. W. and Galan, A. and Schuldt, S. and Sluse, D. and Courbin, F. and Frieman, J. and Millon, M.}, -eprint = {2202.11101}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Shajib2022SLComp.pdf:pdf}, -keywords = {cd,cosmology,data analysis,distance,elliptical and lenticular,galaxies,gravitational lensing,methods,strong}, -pages = {1--35}, -title = {{TDCOSMO. IX. Systematic comparison between lens modelling software programs: time delay prediction for WGD 2038$-$4008}}, -url = {http://arxiv.org/abs/2202.11101}, -year = {2022} -} -@article{Mendez-Abreu2010a, -abstract = {(Abridged) The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were analyzed to derive the intrinsic shape of their bulges. We developed a new method to derive the intrinsic shape of bulges based on the geometrical relationships between the apparent and intrinsic shapes of bulges and disks. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and galaxy inclination. We found that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them is characterized by an elliptical section (B/A{\textless}0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C{\textless}(A+B)/2). The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with Sersic index n{\textgreater}2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T{\textgreater}0.3. In particular, bulges with n{\$}\backslash{\$}leq2 and with B/T{\$}\backslash{\$}leq0.3 show a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n{\textgreater}2 and with B/T{\textgreater}0.3, respectively. According to predictions of the numerical simulations of bulge formation, bulges with n{\$}\backslash{\$}leq2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T{\$}\backslash{\$}leq0.3, could be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n{\textgreater}2 and B/T{\textgreater}0.3.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {Mendez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {8089}, -pages = {A71}, -title = {{Structural properties of disk galaxies. II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Birrer2018a, -abstract = {We present lenstronomy, a multi-purpose open-source gravitational lens modelling pythonpackage. lenstronomy is able to reconstruct the lens mass and surface brightness distributions of strong lensing systems using forward modelling. lenstronomy supports a wide range of analytic lens and light models in arbitrary combination. The software is also able to reconstruct complex extended sources (Birrer et. al 2015) as well as being able to model point sources. We designed lenstronomy to be stable, flexible and numerically accurate, with a clear user interface that could be deployed across different platforms. Throughout its development, we have actively used lenstronomy to make several measurements including deriving constraints on dark matter properties in strong lenses, measuring the expansion history of the universe with time-delay cosmography, measuring cosmic shear with Einstein rings and decomposing quasar and host galaxy light. The software is distributed under the MIT license. The documentation, starter guide, example notebooks, source code and installation guidelines can be found at https://lenstronomy.readthedocs.io.}, -archivePrefix = {arXiv}, -arxivId = {1803.09746}, -author = {Birrer, Simon and Amara, Adam}, -doi = {10.1016/j.dark.2018.11.002}, -eprint = {1803.09746}, -issn = {22126864}, -journal = {Physics of the Dark Universe}, -keywords = {Gravitational lensing,Image simulations,Software}, -pages = {189--201}, -title = {{lenstronomy: Multi-purpose gravitational lens modelling software package}}, -volume = {22}, -year = {2018} -} -@article{Seabroke2011, -abstract = {Gaia will only achieve its unprecedented measurement accuracy requirements with detailed calibration and correction for radiation damage. We present our Silvaco 3D engineering software model of the Gaia CCD pixel and two of its applications for Gaia: (1) physically interpreting supplementary buried channel (SBC) capacity measurements (pocket-pumping and first pixel response) in terms of e2v manufacturing doping alignment tolerances; and (2) deriving electron densities within a charge packet as a function of the number of constituent electrons and 3D position within the charge packet as input to microscopic models being developed to simulate radiation damage. {\textcopyright}EAS, EDP Sciences 2011.}, -archivePrefix = {arXiv}, -arxivId = {1009.2431}, -author = {Seabroke, G M and Prod'homme, T and Hopkinson, G and Burt, D and Robbins, M and Holland, A}, -doi = {10.1051/eas/1045077}, -eprint = {1009.2431}, -isbn = {9782759806089}, -issn = {16334760}, -journal = {EAS Publications Series}, -pages = {433--436}, -title = {{Modelling Gaia CCD pixels with silvaco 3D engineering software}}, -url = {http://www.eas-journal.org/10.1051/eas/1045077}, -volume = {45}, -year = {2011} -} -@article{Boylan2012, -abstract = {We use the Aquarius simulations to show that the most massive subhaloes in galaxy-mass dark matter (DM) haloes in $\Lambda$ cold dark matter ($\Lambda$CDM) are grossly inconsistent with the dynamics of the brightest Milky Way dwarf spheroidal galaxies. While the best-fitting hosts of the dwarf spheroidals all have, $\Lambda$CDM simulations predict at least 10 subhaloes with V max > 25kms -1. These subhaloes are also among the most massive at earlier times, and significantly exceed the reionization suppression mass back to z∼ 10. No $\Lambda$CDM-based model of the satellite population of the Milky Way explains this result. The problem lies in the satellites' densities: it is straightforward to match the observed Milky Way luminosity function, but doing so requires the dwarf spheroidals to have DM haloes that are a factor of ∼5 more massive than is observed. Independent of the difficulty in explaining the absence of these dense, massive subhaloes, there is a basic tension between the derived properties of the bright Milky Way dwarf spheroidals and $\Lambda$CDM expectations. The inferred infall masses of these galaxies are all approximately equal and are much lower than standard $\Lambda$CDM predictions for systems with their luminosities. Consequently, their implied star formation efficiencies span over two orders of magnitude, from 0.2 to 20 per cent of baryons converted into stars, in stark contrast with expectations gleaned from more massive galaxies. We explore possible solutions to these problems within the context of $\Lambda$CDM and find them to be unconvincing. In particular, we use controlled simulations to demonstrate that the small stellar masses of the bright dwarf spheroidals make supernova feedback an unlikely explanation for their low inferred densities. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1111.2048}, -author = {Boylan-Kolchin, Michael and Bullock, James S. and Kaplinghat, Manoj}, -doi = {10.1111/j.1365-2966.2012.20695.x}, -eprint = {1111.2048}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Local Group}, -number = {2}, -pages = {1203--1218}, -title = {{The Milky Way's bright satellites as an apparent failure of $\Lambda$CDM}}, -volume = {422}, -year = {2012} -} -@article{Pub---ae2019, -abstract = {Strong-gravitational lens systems with quadruply imaged quasars (quads) are unique probes to address several fundamental problems in cosmology and astrophysics. Although they are intrinsically very rare, ongoing and planned wide-field deep-sky surveys are set to discover thousands of such systems in the next decade. It is thus paramount to devise a general framework to model strong-lens systems to cope with this large influx without being limited by expert investigator time. We propose such a general modelling framework (implemented with the publicly available software lenstronomy) and apply it to uniformly model three-band Hubble Space Telescope Wide Field Camera 3 images of 13 quads. This is the largest uniformly modelled sample of quads to date and paves the way for a variety of studies. To illustrate the scientific content of the sample, we investigate the alignment between the mass and light distribution in the deflectors. The position angles of these distributions are well-aligned, except when there is strong external shear. However, we find no correlation between the ellipticity of the light and mass distributions. We also show that the observed flux-ratios between the images depart significantly from the predictions of simple smooth models. The departures are strongest in the bluest band, consistent with microlensing being the dominant cause in addition to millilensing. Future papers will exploit this rich data set in combination with ground-based spectroscopy and time delays to determine quantities such as the Hubble constant, the free streaming length of dark matter, and the normalization of the initial stellar mass function.}, -archivePrefix = {arXiv}, -arxivId = {1807.09278}, -author = {Shajib, A J and Birrer, S and Treu, T and Auger, M W and Agnello, A and Anguita, T and Buckley-Geer, E J and Chan, J H H and Collett, T E and Courbin, F and Fassnacht, C D and Frieman, J and Kayo, I and Lemon, C and Lin, H and Marshall, P J and McMahon, R and More, A and Morgan, N D and Motta, V and Oguri, M and Ostrovski, F and Rusu, C E and Schechter, P L and Shanks, T and Suyu, S H and Meylan, G and Abbott, T M C and Allam, S and Annis, J and Avila, S and Bertin, E and Brooks, D and {Carnero Rosell}, A and {Carrasco Kind}, M and Carretero, J and Cunha, C E and {Da Costa}, L N and {De Vicente}, J and Desai, S and Doel, P and Flaugher, B and Fosalba, P and Garc{\'{i}}a-Bellido, J and Gerdes, D W and Gruen, D and Gruendl, R A and Gutierrez, G and Hartley, W G and Hollowood, D L and Hoyle, B and James, D J and Kuehn, K and Kuropatkin, N and Lahav, O and Lima, M and Maia, M A G and March, M and Marshall, J L and Melchior, P and Menanteau, F and Miquel, R and Plazas, A A and Sanchez, E and Scarpine, V and Sevilla-Noarbe, I and Smith, M and Soares-Santos, M and Sobreira, F and Suchyta, E and Swanson, M E C and Tarle, G and Walker, A R}, -doi = {10.1093/mnras/sty3397}, -eprint = {1807.09278}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: structure,gravitational lensing: strong,methods: data analysis}, -number = {4}, -pages = {5649--5671}, -title = {{Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 13 quadruply+ imaged quasars}}, -volume = {483}, -year = {2019} -} -@article{Garvin2022, -abstract = {Context. The Hubble Space Telescope (HST) archives constitute a rich dataset of high-resolution images to mine for strong gravitational lenses. While many HST programmes specifically target strong lenses, they can also be present by coincidence in other HST observations. Aims. Our aim is to identify non-Targeted strong gravitational lenses, without any prior selection on the lens properties, in almost two decades of images from the ESA HST archive (eHST). Methods. We used crowdsourcing on the Hubble Asteroid Hunter (HAH) citizen science project to identify strong lenses, along with asteroid trails, in publicly available large field-of-view HST images. We visually inspected 2354 objects tagged by citizen scientists as strong lenses to clean the sample and identify the genuine lenses. Results. We report the detection of 252 strong gravitational lens candidates, which were not the primary targets of the HST observations. A total of 198 of them are new, not previously reported by other studies, consisting of 45 A grades, 74 B grades and 79 C grades. The majority are galaxy-galaxy configurations. The newly detected lenses are, on average, 1.3 magnitudes fainter than previous HST searches. This sample of strong lenses with high-resolution HST imaging is ideal to follow up with spectroscopy for lens modelling and scientific analyses. Conclusions. This paper presents the unbiased search of lenses that enabled us to find a wide variety of lens configurations, including exotic lenses. We demonstrate the power of crowdsourcing in visually identifying strong lenses and the benefits of exploring large archival datasets. This study shows the potential of using crowdsourcing in combination with artificial intelligence for the detection and validation of strong lenses in future large-scale surveys such as ESA's Euclid mission or in James Webb Space Telescope (JWST) archival images.}, -archivePrefix = {arXiv}, -arxivId = {2207.06997}, -author = {Garvin, Emily O. and Kruk, Sandor and Cornen, Claude and Bhatawdekar, Rachana and Ca{\~{n}}ameras, Raoul and Mer{\'{i}}n, Bruno}, -doi = {10.1051/0004-6361/202243745}, -eprint = {2207.06997}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Garvin2022HSTCrowdSource.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Catalogs,Galaxies: general,Gravitational lensing: strong}, -title = {{Hubble Asteroid Hunter: II. Identifying strong gravitational lenses in HST images with crowdsourcing}}, -volume = {667}, -year = {2022} -} -@article{Conselice2005, -abstract = {The evolution of rest-frame B-band luminosities, stellar masses, and number densities of field galaxies in the Hubble Deep Field North and South are studied as a function of rest-frame B-band morphological type out to redshifts z$\sim$3 using a sample of 1231 I < 27 galaxies with spectroscopic and photometric redshifts. We find that the co-moving number, and relative number, densities of ellipticals and spirals declines rapidly at z > 1, although examples exist at z > 2. The number and number fraction of peculiar galaxies consistent with undergoing major mergers rises consistently at redshifts z > 2. Through simulations we argue that this decline is robust at the 4 sigma level against morphological k-corrections and redshift effects. We trace the evolution of rest-frame B-band luminosity density as a function of morphology out to z$\sim$3 finding that the luminosity density is steadily dominated by peculiars at z > 1.5 with a peak fraction of 60-90% at z$\sim$3. By z$\sim$0.5 B-band luminosity fractions are similar to their local values. The stellar mass density follows a similar trend as the luminosity density, with some important exceptions. At high redshifts, z > 2, over 60-80% of stellar mass is attached to peculiars, while at z< 1, 80-95% of stellar mass is attached to ellipticals and spirals. In contrast to the luminosity density, the stellar mass density of ellipticals is greater than spirals at z < 1.5, and the stellar masses in both types grow together at z < 1, while number densities remain constant. (abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0405001}, -author = {Conselice, Christopher J. and Blackburne, Jeffrey A. and Papovich, Casey}, -doi = {10.1086/426102}, -eprint = {0405001}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Galaxies: Evolution,Galaxies: High-Redshift}, -month = {feb}, -number = {2}, -pages = {564--583}, -primaryClass = {astro-ph}, -title = {{ The Luminosity, Stellar Mass, and Number Density Evolution of Field Galaxies of Known Morphology from z = 0.5 to 3 }}, -url = {http://stacks.iop.org/0004-637X/620/i=2/a=564}, -volume = {620}, -year = {2005} -} -@article{Report2011, -abstract = {Modelling students' behaviour in relation to tuition fees is a complex task since students' 'talent' is not common knowledge. Students observe a private noisy signal of their abilities, while university receives noisy information based on the quantitative and qualitative data provided by university applicants. In this article, we add the heterogeneity of the population to this model: we assume that this heterogeneity means that the perception of skills among a part of the population is biased and underestimates the capabilities of its members to succeed in the higher education system. Our conclusions differ from those derived in the literature and show in particular that the optimal tuition fees for a given number of students are lower than those obtained for a homogeneous population. {\textcopyright}2013 Copyright Taylor and Francis Group, LLC.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Dolphin2009, -abstract = {Charge transfer loss on the Wide Field Planetary Camera 2 (WFPC2) onboard the Hubble Space Telescope is a primary source of uncertainty in stellar photometry obtained with this camera. This effect, discovered shortly after the camera was installed, has grown over time and can dim stars by several tenths of a magnitude (or even more, in particularly bad cases). The impact of CTE loss on WFPC2 stellar photometry was characterized by several studies between 1998 and 2000, but has received diminished attention since ACS became HST's primary imager. After the failure of ACS in January 2007, WFPC2 once again became the primary imaging instrument on board HST, restoring the importance of ensuring accurate CTE corrections. This paper reexamines the CTE loss of WFPC2, with three significant changes over previous studies. First, the present study considers calibration data obtained through 2007, thus increasing the confidence in the reliability of the CTE corrections when applied to recent observations. Second, the change in CTE loss during readout is accounted for analytically. Finally, a reanalysis of the CTE dependencies on counts, background, and observation date was made. The resulting correction is significantly more accurate than that provided in the WFPC2 Instrument Handbook (Dolphin 2002 and updates through 2004), resulting in photometry that can be enhanced by over 5% in certain circumstances.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.IM/0906.3557}, -author = {Dolphin, Andrew E.}, -doi = {10.1086/600028}, -eprint = {0906.3557}, -issn = {0004-6280}, -journal = {Publications of the Astronomical Society of the Pacific}, -keywords = {Data Analysis and Techniques}, -month = {jun}, -number = {880}, -pages = {655--667}, -primaryClass = {astro-ph.IM}, -title = {{A Revised Characterization of the WFPC2 CTE Loss}}, -url = {http://iopscience.iop.org/article/10.1086/600028}, -volume = {121}, -year = {2009} -} -@article{Fergus2014, -abstract = {High dynamic range imagers aim to block or eliminate light from a very bright primary star in order to make it possible to detect and measure far fainter companions; in real systems, a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronagraph. The model uses principal components analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles, but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of the order of a percent of the brightness of the speckles, or up to 10-7 times the brightness of the primary star. This outperforms existing methods by a factor of two to three and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W. and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Fergus et al. - 2014 - S4 A spatial-spectral model for speckle suppression.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Tian2017, -abstract = {We study themass discrepancy-acceleration relation (MDAR) of 57 elliptical galaxies by their Einstein rings from the Sloan Lens ACS Survey (SLACS). The mass discrepancy between the lensing mass and the baryonic mass derived from population synthesis is larger when the acceleration of the elliptical galaxy lenses is smaller. TheMDAR is also related to surface mass density discrepancy. At the Einstein ring, these lenses belong to high-surface-mass density galaxies. Similarly, we find that the discrepancy between the lensing and stellar surface mass density is small. It is consistent with the recent discovery of dynamical surface mass density discrepancy in disc galaxies where the discrepancy is smaller when surface density is larger. We also find relativistic modified Newtonian dynamics (MOND) can naturally explain the MDAR and surface mass density discrepancy in 57 Einstein rings. Moreover, the lensing mass, the dynamical mass and the stellar mass of these galaxies are consistent with each other in relativistic MOND.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1702.00183}, -author = {Tian, Yong and Ko, Chung Ming}, -doi = {10.1093/MNRAS/STX2056}, -eprint = {1702.00183}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tian, Ko - 2017 - Mass discrepancy-acceleration relation in Einstein rings.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: kinematics and dynamics,Dark matter,Galaxies: elliptical and lenticular,Gravitation,Gravitational lensing: strong}, -number = {1}, -pages = {765--771}, -title = {{Mass discrepancy-acceleration relation in Einstein rings}}, -url = {http://arxiv.org/abs/1702.00183}, -volume = {472}, -year = {2017} -} -@article{Greene2015, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 < $\sigma$∗ < 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E. and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J. and Blakeslee, John P. and Thomas, Jens and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2015 - the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies(3).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Marshall2007, -abstract = {We combine high-resolution images in four optical/infrared bands, obtained with the laser guide star adaptive optics (LGSAO) system on the Keck telescope and with the Hubble Space Telescope (HST), to study the gravitational lens system SDSS J0737+3216 (lens redshift 0.3223, source redshift 0.5812). We show that (under favorable observing conditions) ground-based images are comparable to those obtained with HST in terms of precision in the determination of the parameters of both the lens mass distribution and the background source. We also quantify the systematic errors associated with both the incomplete knowledge of the PSF and the uncertain process of lens galaxy light removal and find that similar accuracy can be achieved with Keck LGSAO as with HST We then exploit this well-calibrated combination of optical and gravitational telescopes to perform a multiwavelength study of the source galaxy at 0.01″ effective resolution. We find the S{\'{e}}rsic index to be indicative of a disklike object, but the measured half-light radius (re= 0.59 ± 0.007 stati ± 0.1 sys kpc) and stellar mass (M* = 2.0 ± 1.0 stat ± 0.8 sys × 109M⊙) place it more than 3 $\sigma$ away from the local disk size-mass relation. The SDSS J0737+3216 source has the characteristics of the most compact faint blue galaxies studied and comparable size and mass to dwarf early-type galaxies in the local universe. With the aid of gravitational telescopes to measure individual objects' brightness profiles to 10% accuracy, the study of the high-redshift size-mass relation may be extended by an order of magnitude or more beyond existing surveys at the low-mass end, thus providing a new observational test of galaxy formation models. {\textcopyright} 2007. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:0710.0637v1}, -author = {Marshall, Philip J. and Treu, Tommaso and Melbourne, Jason and Gavazzi, Raphael and Bundy, Kevin and Ammons, S. Mark and Bolton, Adam S. and Burles, Scott and Larkin, James E. and {Le Mignant}, David and Koo, David C. and Koopmans, Leon V. E. and Max, Claire E. and Moustakas, Leonidas A. and Steinbring, Eric and Wright, Shelley A.}, -doi = {10.1086/523091}, -eprint = {arXiv:0710.0637v1}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {1196--1211}, -title = {{ Superresolving Distant Galaxies with Gravitational Telescopes: Keck Laser Guide Star Adaptive Optics and Hubble Space Telescope Imaging of the Lens System SDSS J0737+3216 }}, -url = {http://stacks.iop.org/0004-637X/671/i=2/a=1196}, -volume = {671}, -year = {2007} -} -@article{Vieira2010, -abstract = {We report the results of an 87 deg2 point-source survey centered at R.A. 5h30m, decl. -55° taken with the South Pole Telescope at 1.4 and 2.0 mm wavelengths with arcminute resolution and milli-Jansky depth. Based on the ratio of flux in the two bands, we separate the detected sources into two populations, one consistent with synchrotron emission from active galactic nuclei and the other consistent with thermal emission from dust. We present source counts for each population from 11 to 640 mJy at 1.4 mm and from 4.4 to 800mJy at 2.0 mm. The 2.0 mm counts are dominated by synchrotron-dominated sources across our reported flux range; the 1.4 mm counts are dominated by synchrotron-dominated sources above ∼15 mJy and by dust-dominated sources below that flux level.We detect 141 synchrotron-dominated sources and 47 dust-dominated sources at signal-to-noise ratio S/N > 4.5 in at least one band. All of the most significantly detected members of the synchrotron-dominated population are associated with sources in previously published radio catalogs. Some of the dust-dominated sources are associated with nearby (z ≪ 1) galaxies whose dust emission is also detected by the Infrared Astronomy Satellite. However, most of the bright, dust-dominated sources have no counterparts in any existing catalogs.We argue that these sources represent the rarest and brightestmembers of the population commonly referred to as submillimeter galaxies (SMGs). Because these sources are selected at longer wavelengths than in typical SMG surveys, they are expected to have a higher mean redshift distribution and may provide a new window on galaxy formation in the early universe.}, -archivePrefix = {arXiv}, -arxivId = {0912.2338}, -author = {Vieira, J. D. and Crawford, T. M. and Switzer, E. R. and Ade, P. A.R. and Aird, K. A. and Ashby, M. L.N. and Benson, B. A. and Bleem, L. E. and Brodwin, M. and Carlstrom, J. E. and Chang, C. L. and Cho, H. M. and Crites, A. T. and {De Haan}, T. and Dobbs, M. A. and Everett, W. and George, E. M. and Gladders, M. and Hall, N. R. and Halverson, N. W. and High, F. W. and Holder, G. P. and Holzapfel, W. L. and Hrubes, J. D. and Joy, M. and Keisler, R. and Knox, L. and Lee, A. T. and Leitch, E. M. and Lueker, M. and Marrone, D. P. and McIntyre, V. and McMahon, J. J. and Mehl, J. and Meyer, S. S. and Mohr, J. J. and Montroy, T. E. and Padin, S. and Plagge, T. and Pryke, C. and Reichardt, C. L. and Ruhl, J. E. and Schaffer, K. K. and Shaw, L. and Shirokoff, E. and Spieler, H. G. and Stalder, B. and Staniszewski, Z. and Stark, A. A. and Vanderlinde, K. and Walsh, W. and Williamson, R. and Yang, Y. and Zahn, O. and Zenteno, A.}, -doi = {10.1088/0004-637X/719/1/763}, -eprint = {0912.2338}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Vieira2010MilimeterSL.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {Galaxies: High-redshift,Submillimeter: Galaxies,Surveys}, -number = {1}, -pages = {763--783}, -title = {{Extragalactic millimeter-wave sources in South Pole Telescope survey data: Source counts, catalog, and statistics for an 87 square-degree field}}, -volume = {719}, -year = {2010} -} -@article{Gaitskell2004, -abstract = {▪ Abstract This article reviews the astrophysics and cosmological evidence for nonbaryonic dark matter (DM). It covers historical, current, and future experiments that look for direct evidence of particle DM. In addition, it surveys the underlying particle theories that provide some guidance about expected event rates, and the future prospects for the discovery of DM. A number of recent theoretical papers, making calculations in SUSY-based frameworks, show a spread of many ({\textgreater}5) orders of magnitude in the possible interaction rates for models consistent with existing cosmological and accelerator bounds. Within this decade, it seems likely that DM searches will be successful, or at the very least rule out a broad class of the currently most favored DM models.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1410.0601v1}, -author = {Majumdar, Debasish}, -doi = {10.1201/b17323-11}, -eprint = {arXiv:1410.0601v1}, -isbn = {{\textless}null{\textgreater}}, -issn = {0163-8998}, -journal = {Dark Matter}, -keywords = {95.30.Cq,95.35.+d,98.62.Gq,SUSY,WIMPs,axions,cold dark matter,dark matter halo}, -month = {dec}, -number = {1}, -pages = {159--178}, -title = {{Direct Detection of Dark Matter}}, -url = {http://www.annualreviews.org/doi/10.1146/annurev.nucl.54.070103.181244}, -volume = {54}, -year = {2014} -} -@article{Refsdal1964, -abstract = {Abstract image available at: http://adsabs.harvard.edu/abs/1964MNRAS.128..307R}, -author = {Refsdal, S.}, -doi = {10.1093/mnras/128.4.307}, -isbn = {0301-620X (Print) 0301-620X (Linking)}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -number = {4}, -pages = {307--310}, -pmid = {23188894}, -title = {{On the Possibility of Determining Hubble's Parameter and the Masses of Galaxies from the Gravitational Lens Effect}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/128.4.307}, -volume = {128}, -year = {1964} -} -@article{Noll2009, -abstract = {Aims.Photometric data of galaxies covering the rest-frame wavelength range from far-UV to far-IR make it possible to derive galaxy properties with a high reliability by fitting the attenuated stellar emission and the related dust emission at the same time. Methods. For this purpose we wrote the code CIGALE (Code Investigating GALaxy Emission) that uses model spectra composed of the Maraston (or PEGASE) stellar population models, synthetic attenuation functions based on a modified Calzetti law, spectral line templates, the Dale & Helou dust emission models, and optional spectral templates of obscured AGN. Depending on the input redshifts, filter fluxes were computed for the model set and compared to the galaxy photometry by carrying out a Bayesian-like analysis. CIGALE was tested by analysing 39 nearby galaxies selected from SINGS. The reliability of the different model parameters was evaluated by studying the resulting expectation values and their standard deviations in relation to the input model grid. Moreover, the influence of the filter set and the quality of photometric data on the code results was estimated. Results.For up to 17 filters with effective wavelengths between 0.15 and 160 $\mu$m, we find robust results for the mass, star formation rate, effective age of the stellar population at 4000 {\AA}, bolometric luminosity, luminosity absorbed by dust, and attenuation in the far-UV. Details of the star formation history (excepting the burst fraction) and the shape of the attenuation curve are difficult to investigate with the available broad-band UV and optical photometric data. A study of the mutual relations between the reliable properties confirms the dependence of star formation activity on morphology in the local Universe and indicates a significant drop in this activity at about 1011 M towards higher total stellar masses. The dustiest galaxies in the SINGS sample are present in the same mass range. On the other hand, the far-UV attenuation of our sample galaxies does not appear to show a significant dependence on star formation activity. {\textcopyright} 2009 ESO.}, -author = {Noll, S. and Burgarella, D. and Giovannoli, E. and Buat, V. and Marcillac, D. and Mu{\~{n}}oz-Mateos, J. C.}, -doi = {10.1051/0004-6361/200912497}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Noll2009CIGALE.pdf:pdf}, -issn = {00046361}, -journal = {A\&A}, -keywords = {Galaxies: ISM,Galaxies: fundamental parameters,Galaxies: stellar content,Infrared: galaxies,Methods: data analysis,Ultraviolet: galaxies}, -number = {3}, -pages = {1793--1813}, -title = {{Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: Studying a SINGS test sample}}, -volume = {507}, -year = {2009} -} -@article{Pulsoni2017, -abstract = {Wolbachia is an intracellular endosymbiont that induces a variety of reproductive alterations in diverse arthropods. The almond moth, Cadra cautella, is double infected with two Wolbachia variants, wCauA and wCauB, and expresses complete cytoplasmic incompatibility (CI). The individual contribution of wCauA and wCauB to the expression of CI are unclear, however, because the two variants have not been separated in this host. The effect of wCauA is of particular interest because it induces male killing when transferred into the Mediterranean flour moth, Ephestia kuehniella. In the present study, we generated C. cautella infected with only wCauA by treating double-infected insects with tetracycline. Single-infected C. cautella exhibited strong CI, demonstrating that wCauA induces two distinct reproductive phenotypes in different hosts: CI in C. cautella and male killing in E. kuehniella. CI was also observed in the cross of double-infected males and single-infected females. Comparison of the single- and double-infected insects by real-time quantitative polymerase chain reaction suggested that the wCauA density is not affected much by the presence or absence of wCauB. {\textcopyright}2005 Nature Publishing Group All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {http://www.R-project.org}, -author = {Sasaki, T and Massaki, N and Kubo, T}, -doi = {10.1038/sj.hdy.6800737}, -eprint = {/www.R-project.org}, -isbn = {0018-067X}, -issn = {0018067X}, -journal = {Heredity}, -keywords = {Cadra cautella,Cytoplasmic incompatibility,Double infection,Male killing,Real-time quantitative PCR,Wolbachia}, -number = {5}, -pages = {389--393}, -pmid = {16106260}, -primaryClass = {http:}, -title = {{Wolbachia variant that induces two distinct reproductive phenotypes in different hosts}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/16106260}, -volume = {95}, -year = {2005} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M{\textless}inf{\textgreater}*{\textless}/inf{\textgreater} {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M{\textless}inf{\textgreater}⊙{\textless}/inf{\textgreater} galaxies at 1 {\textless} z {\textless} 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 {\textless} z {\textless} 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.5221}, -volume = {444}, -year = {2014} -} -@article{Hernquist1990, -abstract = {A potential-density pair which closely approximates the de Vaucouleurs R1/4 law for elliptical galaxies is presented. It is shown that the intrinsic properties and projected distributions of this model can be evaluated analytically. In particular, the distribution function, density of states, and projected surface brightness and velocity dispersion are expressible in terms of elementary functions.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {Hernquist, Lars}, -eprint = {arXiv:1011.1669v3}, -file = {:C\:/Users/Jammy/Documents/Papers/LightProFFits/Hernquist1990Nuker.pdf:pdf}, -isbn = {9788578110796}, -issn = {1098-6596}, -journal = {ApJ}, -keywords = {icle}, -number = {2}, -pages = {359--364}, -pmid = {25246403}, -title = {{An analytical model for spherical galaxies and buldges}}, -volume = {356}, -year = {1990} -} -@article{Croom2009, -abstract = {We present the quasi-stellar object (QSO) luminosity function (LF) of the completed 2dF-SDSS LRG and QSO (2SLAQ) survey, based on QSOs photometrically selected from Sloan Digital Sky Survey (SDSS) imaging data and then observed spectroscopically using the 2dF instrument on the Anglo-Australian Telescope. We analyse 10 637 QSOs in the redshift range 0.4 {\textless} z {\textless} 2.6 to a g-band flux limit of 21.85 (extinction-corrected) and an absolute continuum magnitude of Mg(z = 2) {\textless} -21.5. This sample covers an area of 191.9 deg 2. The binned QSO LF agrees with that of the brighter SDSS main QSO sample, but extends ∼2.5 mag fainter, clearly showing the flattening of the LF towards faint absolute magnitudes. 2SLAQ finds an excess of QSOs compared to the 2dF QSO Redshift Survey at g {\textgreater} 20.0, as found previously by Richards et al. The LF is consistent with other previous, much smaller, samples produced to the depth of 2SLAQ. By combining the 2SLAQ and SDSS QSO samples, we produce a QSO LF with an unprecedented combination of precision and dynamic range. With this we are able to accurately constrain both the bright and faint ends of the QSO LF. While the overall trends seen in the evolution of the QSO LF appear similar to pure luminosity evolution, the data show very significant departures from such a model. Most notably we see clear evidence that the number density of faint QSOs peaks at lower redshift than bright QSOs: QSOs with Mg {\textgreater} -23 have space densities which peak at z {\textless} 1, while QSOs at M g {\textless} -26 peak at z {\textgreater} 2. By fitting simple LF models in narrow Mg intervals, we find that this downsizing is significant at the 99.98 per cent level. We show that LF models which follow the pure luminosity evolution form [i.e. M*g ≡ M*g(z)], but with a redshift-dependent bright-end slope and an additional density evolution term, $\Phi$*≡ $\Phi$*(z), provide a much improved fit to the data. The bright-end slope, $\alpha$, steepens from $\alpha$ ≃ -3.0 at z ≃ 0.5 to $\alpha$ = -3.5 at z ≃ 2.5. This steepening is significant at the 99.9 per cent level. We find a decline in $\Phi$*from z ≃ 0.5 to 2.5 which is significant at the 94 per cent level. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0907.2727}, -author = {Croom, Scott M and Richards, Gordon T and Shanks, Tom and Boyle, Brian J and Strauss, Michael A and Myers, Adam D and Nichol, Robert C and Pimbblet, Kevin A and Ross, Nicholas P and Schneider, Donald P and Sharp, Robert G and Wake, David A}, -doi = {10.1111/j.1365-2966.2009.15398.x}, -eprint = {0907.2727}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Seyfert,Galaxies: active,Quasars: general}, -month = {nov}, -number = {4}, -pages = {1755--1772}, -title = {{The 2dF-SDSS LRG and QSO survey: The QSO luminosity function at 0.4 {\textless} z {\textless} 2.6}}, -volume = {399}, -year = {2009} -} -@article{RomanoDiaz2008, -abstract = {We study the central dark matter (DM) cusp evolution in cosmologically grown galactic halos. Numerical models with and without baryons (baryons+DM, hereafter BDM model, and pure DM, PDM model, respectively) are advanced from identical initial conditions, obtained using the Constrained Realization method. The DM cusp properties are contrasted by a direct comparison of pure DM and baryonic models. We find a divergent evolution between the PDM and BDM models within the inner few × 10 kpc region. The PDM model forms an R-1 cusp as expected, while the DM in the BDM model forms a larger isothermal cusp R-2 instead. The isothermal cusp is stable until z$\sim$1 when it gradually levels off. This leveling proceeds from inside out and the final density slope is shallower than -1 within the central 3 kpc (i.e., expected size of the R-1 cusp), tending to a flat core within $\sim$2 kpc. This effect cannot be explained by a finite resolution of our code which produces only a 5% difference between the gravitationally softened force and the exact Newtonian force of point masses at 1 kpc from the center. Neither is it related to the energy feedback from stellar evolution or angular momentum transfer from the bar. Instead it can be associated with the action of DM+baryon subhalos heating up the cusp region via dynamical friction and forcing the DM in the cusp to flow out and to ``cool'' down. The process described here is not limited to low z and can be efficient at intermediate and even high z.}, -archivePrefix = {arXiv}, -arxivId = {0808.0195}, -author = {Romano-D{\'{i}}az, Emilio and Shlosman, Isaac and Hoffman, Yehuda and Heller, Clayton}, -doi = {10.1086/592687}, -eprint = {0808.0195}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Evolution,Galaxies: Formation,Galaxies: Halos,Galaxies: Interactions,Galaxies: Kinematics and Dynamics}, -month = {oct}, -number = {2}, -pages = {L105--L108}, -title = {{Erasing Dark Matter Cusps in Cosmological Galactic Halos with Baryons}}, -url = {http://adsabs.harvard.edu/abs/2008ApJ...685L.105R}, -volume = {685}, -year = {2008} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright} 2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F.}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Steinmetz, Navarro - 2002 - The hierarchical origin of galaxy morphologies.pdf:pdf}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{He2022b, -abstract = {We rederive the number density of intervening line-of-sight haloes relative to lens subhaloes in galaxy-galaxy strong lensing observations, where these perturbers can generate detectable image fluctuations. Previous studies have calculated the detection limit of a line-of-sight small-mass dark halo by comparing the lensing deflection angles it would cause, to those caused by a subhalo within the lens. However, this overly simplifies the difference in observational consequences between a subhalo and a line-of-sight halo. Furthermore, it does not take into account degeneracies between an extra subhalo and the uncertain properties of the main lens. More in keeping with analyses of real-world observations, we regard a line-of-sight halo as detectable only if adding it to a smooth model generates a statistically significant improvement in the reconstructed image. We find that the number density of detectable line-of-sight perturbers has been overestimated by as much as a factor of two in the previous literature. For typical lensing geometries and configurations, very deep imaging is sensitive to twice as many line-of-sight perturbers as subhaloes, but moderate depth imaging is sensitive to only slightly more line-of-sight perturbers than subhaloes.}, -archivePrefix = {arXiv}, -arxivId = {2110.04512}, -author = {He, Qiuhan and Li, Ran and Frenk, Carlos S and Nightingale, James and Cole, Shaun and Amorisco, Nicola C and Massey, Richard and Robertson, Andrew and Etherington, Amy and Amvrosiadis, Aristeidis and Cao, Xiaoyue}, -doi = {10.1093/mnras/stac759}, -eprint = {2110.04512}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/He2021LoS.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {dark matter,gravitational lensing,strong}, -number = {4}, -pages = {5862--5873}, -title = {{Galaxy–galaxy strong lens perturbations: line-of-sight haloes versus lens subhaloes}}, -url = {http://arxiv.org/abs/2110.04512}, -volume = {512}, -year = {2022} -} -@article{Laporte:2013aa, -abstract = {We study the formation and evolution of brightest cluster galaxies starting from a z = 2 population of quiescent ellipticals and following them to z = 0. To this end, we use a suite of nine high-resolution dark matter only simulations of galaxy clusters in a $\lambda$ cold dark matter ($\lambda$CDM)universe.We develop a scheme inwhich simulation particles are weighted to generate realistic and dynamically stable stellar density profiles at z = 2. Our initial conditions assign a stellar mass to every identified dark halo as expected from abundance matching; assuming that there exists a one-to-one relation between the visible properties of galaxies and their host haloes. We setthe sizes of the luminous components according to the observed relations for z $\sim$ 2 massive quiescent galaxies. We study the evolution of the mass-sizerelation, the fate of satellite galaxies and the mass aggregation of the cluster central. From z = 2, these galaxies grow on average in size by a factor of 5 to 10 and in galaxy mass by 2 to 3. The stellar mass of our simulated BCGs grow by a factor of $\sim$2.1 in the range 0.3 < z < 1.0, consistent with observations, and by a factor of $\sim$1.4 in the range 0.0 < z<0.3. Furthermore, the non-central galaxies evolve on to the present-day mass-size relation by z = 0. Assuming passively evolving stellar populations, we present surface brightness profiles for our cluster centrals which resemble those observed for the cDs in similar mass clusters both at z = 0 and at z = 1. This demonstrates that the $\lambda$CDM cosmology does indeed predict minor and major mergers to occur in galaxy clusters with the frequency and mass ratio distribution required to explain the observed growth in size of passive galaxies since z = 2. Our experiment shows that brightest cluster galaxies could, inprinciple, form through dissipationless mergers of quiescent massive z = 2 galaxies, without substantial additional star formation. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1301.5319}, -author = {Laporte, Chervin F.P. and White, Simon D.M. and Naab, Thorsten and Gao, Liang}, -doi = {10.1093/mnras/stt912}, -eprint = {1301.5319}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Laporte et al. - 2013 - The growth in size and mass of cluster galaxies since z = 2(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Clusters: General,Galaxies,Galaxies: Elliptical and lenticular: cD,Galaxies: Evolution,Galaxies: Formation}, -month = {oct}, -number = {2}, -pages = {901--909}, -title = {{The growth in size and mass of cluster galaxies since z = 2}}, -volume = {435}, -year = {2013} -} -@article{Smith2019, -abstract = {The emergence of the first black holes during the first billion years of cosmic history marks a key event in cosmology. Their formation is part of the overall process of ending the cosmic dark ages, when the first stars appeared in low-mass dark matter haloes about a few 100 million years after the Big Bang. The first stars, galaxies, and black holes transformed the Universe from its simple initial state into one of ever increasing complexity. We review recent progress on our emerging theoretical picture of how the first black holes appeared on the cosmic scene, and how they impacted the subsequent history of the Universe. Our focus is on supermassive black holes, in particular assessing possible pathways to the formation of the billion-solar-mass black holes inferred to power the luminous quasars at high redshifts. We conclude with a discussion of upcoming empirical probes, such as the James Webb Space Telescope (JWST), and the Laser Interferometer Space Antenna (LISA), further ahead in time.}, -archivePrefix = {arXiv}, -arxivId = {2001.08420}, -author = {Smith, Aaron and Bromm, Volker}, -doi = {10.1080/00107514.2019.1615715}, -eprint = {2001.08420}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Smith, Bromm - 2019 - Supermassive black holes in the early universe.pdf:pdf}, -issn = {13665812}, -journal = {Contemporary Physics}, -keywords = {Black holes,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {2}, -pages = {111--126}, -title = {{Supermassive black holes in the early universe}}, -volume = {60}, -year = {2019} -} -@article{Lee2016, -abstract = {We study how properties of discrete dark matter haloes depend on halo environment, characterized by the mass density around the haloes on scales from 0.5 to 16 h−1 Mpc. We find that low-mass haloes (those less massive than the characteristic mass MC of haloes collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations and rounder shapes than haloes in median density environments. Haloes in median- and low-density environments have similar accretion rates and concentrations, but haloes in low-density environments have lower spins and are more elongated. Haloes of a given mass in high-density regions accrete material earlier than haloes of the same mass in lower density regions. All but the most massive haloes in high-density regions are losing mass (i.e. being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low-mass haloes in high-density regions at low redshifts z < 1, by preferentially removing higher angular momentum material from haloes. Haloes in low-density regions have lower than average spins because they lack nearby haloes whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an extreme value distribution, and that the density distribution becomes broader with cosmic time.}, -archivePrefix = {arXiv}, -arxivId = {1610.02108}, -author = {Lee, Christoph T. and Primack, Joel R. and Behroozi, Peter and Rodr{\'{i}}guez-Puebla, Aldo and Hellinger, Doug and Dekel, Avishai}, -doi = {10.1093/mnras/stw3348}, -eprint = {1610.02108}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lee et al. - 2017 - Properties of dark matter haloes as a function of local environment density.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Large-scale structure of Universe,Methods: numerical}, -number = {4}, -pages = {3834--3858}, -title = {{Properties of dark matter haloes as a function of local environment density}}, -url = {http://arxiv.org/abs/1610.02108%0Ahttp://dx.doi.org/10.1093/mnras/stw3348}, -volume = {466}, -year = {2017} -} -@article{Jullo2010, -abstract = {Current efforts in observational cosmology are focused on characterizing the mass-energy content of the universe. We present results from a geometric test based on strong lensing in galaxy clusters. Based on Hubble Space Telescope images and extensive ground-based spectroscopic follow-up of the massive galaxy cluster Abell 1689, we used a parametric model to simultaneously constrain the cluster mass distribution and dark energy equation of state. Combining our cosmological constraints with those from x-ray clusters and the Wilkinson Microwave Anisotropy Probe 5-year data gives $\Omega$m = 0.25 ±0.05 and Wx = -0.97 ±0.07, which are consistent with results from other methods. Inclusion of our method with all other available techniques brings down the current 2$\sigma$ contours on the dark energy equation-of-state parameter wx by ∼30%.}, -archivePrefix = {arXiv}, -arxivId = {1008.4802}, -author = {Jullo, Eric and Natarajan, Priyamvada and Kneib, Jean Paul and D'Aloisio, Anson and Limousin, Marceau and Richard, Johan and Schimd, Carlo}, -doi = {10.1126/science.1185759}, -eprint = {1008.4802}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Jullo et al. - 2010 - Cosmological constraints from strong gravitational lensing in clusters of galaxies.pdf:pdf}, -issn = {00368075}, -journal = {Science}, -number = {5994}, -pages = {924--927}, -title = {{Cosmological constraints from strong gravitational lensing in clusters of galaxies}}, -volume = {329}, -year = {2010} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. (2011) with the particle-tagging technique of Cooper et al. (2010) to predict galaxy surface brightness profiles in a representative sample of {\$\sim${}}1900 massive dark matter haloes (10{\^{}}12--10{\^{}}14 M{\_}sol) from the Millennium II Lambda-CDM N-body simulation. Here we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of Milky Way-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a Sersic profile, the radial scale and amplitude of which vary systematically with halo mass (M{\_}200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M{\_}200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M{\_}star and M{\_}200. To test our model we have derived average stellar mass surface density profiles for massive galaxies at z{\$\sim${}}0.08 by stacking SDSS images. Our model agrees well with these stacked profiles and with other data from the literature, and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S and White, Simon D M}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Talbot2018, -abstract = {We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for eight of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with two background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched $\sim$1.5 million spectra, of which 3065 contained multiple high signal-to-noise ratio background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius ≳ 1.7 arcsec, which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely.}, -archivePrefix = {arXiv}, -arxivId = {1803.03604}, -author = {Talbot, Michael S. and Brownstein, Joel R. and Bolton, Adam S. and Bundy, Kevin and Andrews, Brett H. and Cherinka, Brian and Collett, Thomas E. and More, Anupreeta and More, Surhud and Sonnenfeld, Alessandro and Vegetti, Simona and Wake, David A. and Weijmans, Anne Marie and Westfall, Kyle B.}, -doi = {10.1093/mnras/sty653}, -eprint = {1803.03604}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Talbot et al. - 2018 - SDSS-IV MaNGA The spectroscopic discovery of strongly lensed galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: General,Gravitational lensing: Strong}, -number = {1}, -pages = {195--209}, -title = {{SDSS-IV MaNGA: The spectroscopic discovery of strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1803.03604%0Ahttp://dx.doi.org/10.1093/mnras/sty653}, -volume = {477}, -year = {2018} -} -@article{Hopkins2009, -abstract = {Transformation of discs into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that the bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in haloes according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the overproduction of spheroids: low- and intermediate-mass galaxies are predicted to be bulge-dominated (B/T ∼ 0.5 at {\textless}10 10 M ⊙, with almost no 'bulgeless' systems), even if they have avoided major mergers. Including the different physical behaviour of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T ∼ 0.1 at {\textless}10 10 M ⊙, with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behaviour of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4111}, -author = {Hopkins, Philip F and Somerville, Rachel S and Cox, Thomas J and Hernquist, Lars and Jogee, Shardha and Kere{\v{s}}, Dusan and Ma, Chung Pei and Robertson, Brant and Stewart, Kyle}, -doi = {10.1111/j.1365-2966.2009.14983.x}, -eprint = {0901.4111}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Galaxies: spiral}, -number = {2}, -pages = {802--814}, -title = {{The effects of gas on morphological transformation in mergers: Implications for bulge and disc demographics}}, -volume = {397}, -year = {2009} -} -@article{Johnston2016, -abstract = {With the availability of large integral field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, howgalaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present bulge-disc decomposition of IFU data cubes (BUDDI), a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GALFITM, a modified form of GALFIT which can fit multiwaveband images simultaneously. The benefit of this technique over traditional multiwaveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the Sloan Digital Sky Survey-IV Mapping Nearby Galaxies atAPO(MaNGA)survey with redshifts z < 0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec full width at half-maximum and field of view of > 22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from theMaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data.}, -archivePrefix = {arXiv}, -arxivId = {1611.00609}, -author = {Johnston, Evelyn J. and H{\"{a}}u{\ss}ler, Boris and Arag{\'{o}}n-Salamanca, Alfonso and Merrifield, Michael R. and Bamford, Steven and Bershady, Matthew A. and Bundy, Kevin and Drory, Niv and Fu, Hai and Law, David and Nitschelm, Christian and Thomas, Daniel and Lopes, Alexandre Roman and Wake, David and Yan, Renbin}, -doi = {10.1093/mnras/stw2823}, -eprint = {1611.00609}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Johnston et al. - 2017 - SDSS-IV MaNGA Bulge-disc decomposition of IFU data cubes (BUDDI)(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content,Galaxies: structure}, -number = {2}, -pages = {2317--2341}, -title = {{SDSS-IV MaNGA: Bulge-disc decomposition of IFU data cubes (BUDDI)}}, -url = {http://arxiv.org/abs/1611.00609%0Ahttp://dx.doi.org/10.1093/mnras/stw2823}, -volume = {465}, -year = {2017} -} -@article{Greene2017b, -abstract = {The "kinematic" morphology-density relation for early-type galaxies posits that those galaxies with low angular momentum are preferentially found in the highest-density regions of the universe. We use a large sample of galaxy groups with halo masses 10{\^{}}12.5 {\textless} M{\_}halo {\textless} 10{\^{}}14.5 M{\_}sun/h observed with the Mapping Nearby Galaxies at APO (MaNGA) survey to examine whether there is a correlation between local environment and rotational support that is independent of stellar mass. We find no compelling evidence for a relationship between the angular momentum content of early-type galaxies and either local overdensity or radial position within the group at fixed stellar mass.}, -archivePrefix = {arXiv}, -arxivId = {1708.07843}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Goddard, D and Ge, J and Andrews, B H and Brinkman, J and Brownstein, J R and Greco, J and Law, D and Lin, Y.-T. and Masters, K L and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Yan, R and Drory, N}, -doi = {10.3847/2041-8213/aa8ace}, -eprint = {1708.07843}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L33}, -title = {{SDSS-IV MaNGA: Probing the Kinematic Morphology–Density Relation of Early-type Galaxies with MaNGA}}, -url = {http://arxiv.org/abs/1708.07843%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa8ace}, -volume = {851}, -year = {2017} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. with the particletagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of {\$\sim${}}1900 massive dark matter haloes (1012-1014M⊙) from the Millennium II $\lambda$ cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of MilkyWay-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a S{\`{e}}rsic profile, the radial scale and amplitude of which vary systematically with halo mass (M200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M* and M200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z ≈ 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S and White, Simon D M}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Seabroke2011, -abstract = {Gaia will only achieve its unprecedented measurement accuracy $\backslash$nrequirements with detailed calibration and correction for radiation$\backslash$ndamage. We present our Silvaco 3D engineering software model of the Gaia$\backslash$nCCD pixel and two of its applications for Gaia: (1) physically$\backslash$ninterpreting supplementary buried channel (SBC) capacity measurements$\backslash$n(pocket-pumping and first pixel response) in terms of e2v manufacturing$\backslash$ndoping alignment tolerances; and (2) deriving electron densities within$\backslash$na charge packet as a function of the number of constituent electrons and$\backslash$n3D position within the charge packet as input to microscopic models$\backslash$nbeing developed to simulate radiation damage.}, -archivePrefix = {arXiv}, -arxivId = {1009.2431}, -author = {Seabroke, G M and Prod'homme, T and Hopkinson, G and Burt, D and Robbins, M and Holland, A}, -doi = {10.1051/eas/1045077}, -eprint = {1009.2431}, -isbn = {1633-4760}, -issn = {1633-4760}, -journal = {EAS Publications Series}, -pages = {433--436}, -title = {{Modelling Gaia CCD pixels with Silvaco 3D engineering software}}, -url = {http://www.eas-journal.org/10.1051/eas/1045077}, -volume = {45}, -year = {2010} -} -@article{Dunne2003, -abstract = {Deep surveys in many wavebands have shown that the rate at which stars were forming was at least a factor of 10 higher at redshifts > 1 than today. Heavy elements ('metals') are produced by stars, and the star formation history deduced by these surveys implies that a significant fraction of all metals in the Universe today should already exist at z ∼ 2-3. However, only 10 per cent of the total metals expected to exist at this redshift have so far been accounted for (in damped Lyman $\alpha$ absorbers and the Lyman forest). In this paper, we use the results of submillimetre surveys of the local and high-redshift Universe to show that there was much more dust in galaxies in the past. We find that a large proportion of the missing metals are traced by this dust, bringing the metals implied from the star formation history and observations into agreement. We also show that the observed distribution of dust masses at high redshift can be reproduced remarkably well by a simple model for the evolution of dust in spheroids, suggesting that the descendants of the dusty galaxies found in deep submillimetre surveys are the relatively dust-free spiral bulges and ellipticals in the Universe today.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0210260}, -author = {Dunne, Loretta and Eales, Stephen A. and Edmunds, M. G.}, -doi = {10.1046/j.1365-8711.2003.06440.x}, -eprint = {0210260}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dust, extinction,Galaxies: Evolution,Galaxies: ISM,Galaxies: Luminosity function, Mass function,Submillimetre}, -number = {2}, -pages = {589--598}, -primaryClass = {arXiv:astro-ph}, -title = {{A census of metals at high and low redshift and the connection between submillimetre sources and spheroid formation}}, -volume = {341}, -year = {2003} -} -@article{2001eq, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Crain2015, -abstract = {We present results from 13 cosmological simulations that explore the parameter space of the 'Evolution and Assembly of GaLaxies and their Environments' (EAGLE) simulation project. Four of the simulations follow the evolution of a periodic cube L=50 cMpc on a side, and each employs a different subgrid model of the energetic feedback associated with star formation. The relevant parameters were adjusted so that the simulations each reproduce the observed galaxy stellar mass function at z = 0.1. Three of the simulations fail to form disc galaxies as extended as observed, and we show analytically that this is a consequence of numerical radiative losses that reduce the efficiency of stellar feedback in high-density gas. Such losses are greatly reduced in the fourth simulation - the EAGLE reference model - by injecting more energy in higher density gas. This model produces galaxies with the observed size distribution, and also reproduces many galaxy scaling relations. In the remaining nine simulations, a single parameter or process of the reference model was varied at a time. We find that the properties of galaxies with stellar mass ≲ M* (the 'knee' of the galaxy stellar mass function) are largely governed by feedback associated with star formation, while those of more massive galaxies are also controlled by feedback from accretion on to their central black holes. Both processes must be efficient in order to reproduce the observed galaxy population. In general, simulations that have been calibrated to reproduce the low-redshift galaxy stellar mass function will still not form realistic galaxies, but the additional requirement that galaxy sizes be acceptable leads to agreement with a large range of observables.}, -archivePrefix = {arXiv}, -arxivId = {1501.01311}, -author = {Crain, Robert A. and Schaye, Joop and Bower, Richard G. and Furlong, Michelle and Schaller, Matthieu and Theuns, Tom and Vecchia, Claudio Dalla and Frenk, Carlos S. and McCarthy, Ian G. and Helly, John C. and Jenkins, Adrian and Rosas-Guevara, Yetli M. and White, Simon D.M. and Trayford, James W.}, -doi = {10.1093/mnras/stv725}, -eprint = {1501.01311}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -month = {jun}, -number = {2}, -pages = {1937--1961}, -pmid = {22459768}, -title = {{The EAGLE simulations of galaxy formation: Calibration of subgrid physics and model variations}}, -volume = {450}, -year = {2015} -} -@article{Luis, -abstract = {This study departs from the reality of gender relations within the family institution which has to be dikhotomis, causing the pole inequality relations between men and women. Therefore, in this study wanted to dismantle the detail view of some theories, both social and feminist about gender relations in the family. Each of these theories (structural functional, conflict and feminist) has their own viewpoint about the pattern of gender relations in the family. However, simultaneously acknowledging that the social construction of culture remained significant influence on the division of roles are played by men (husbands) and women (wife) in the family institution. This means that the social construction of culture was instrumental in the creation of relations contribute between men and women equally or otherwise occurred inequality.}, -author = {Luis, Francisco and Moncayo, Gil}, -file = {:C\:/Users/Jammy/Documents/Papers/devaucoleurs1948.247D:247D}, -isbn = {9788490225370}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular it demands highly efficient machine learning and image analysis algorithms. But scalability is not the only challenge: Astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. We argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. In the following, we will present this exciting application area for data scientists. We will focus on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Kreckel2013, -abstract = {Dust has long been identified as a barrier to measuring inherent galaxy properties. However, the link between dust and attenuation is not straightforward and depends on both the amount of dust and its distribution. Herschel imaging of nearby galaxies undertaken as part of the KINGFISH project allows us to map the dust as seen in emission with unprecedented sensitivity and ∼1 kpc resolution. We present here new optical integral field unit spectroscopy for eight of these galaxies that provides complementary 100-200 pc scale maps of the dust attenuation through observation of the reddening in both the Balmer decrement and the stellar continuum. The stellar continuum reddening, which is systematically less than that observed in the Balmer decrement, shows no clear correlation with the dust, suggesting that the distribution of stellar reddening acts as a poor tracer of the overall dust content. The brightest H II regions are observed to be preferentially located in dusty regions, and we do find a correlation between the Balmer line reddening and the dust mass surface density for which we provide an empirical relation. Some of the high-inclination systems in our sample exhibit high extinction, but we also find evidence that unresolved variations in the dust distribution on scales smaller than 500 pc may contribute to the scatter in this relation. We caution against the use of integrated AV measures to infer global dust properties. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1305.2923}, -author = {Kreckel, Kathryn and Groves, Brent and Schinnerer, Eva and Johnson, Benjamin D. and Aniano, Gonzalo and Calzetti, Daniela and Croxall, Kevin V. and Draine, Bruce T. and Gordon, Karl D. and Crocker, Alison F. and Dale, Daniel A. and Hunt, Leslie K. and Kennicutt, Robert C. and Meidt, Sharon E. and Smith, J. D.T. and Tabatabaei, Fatemeh S.}, -doi = {10.1088/0004-637X/771/1/62}, -eprint = {1305.2923}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Kreckel2013Dust.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {dust,extinction,galaxies: ISM}, -number = {1}, -title = {{Mapping dust through emission and absorption in nearby galaxies}}, -volume = {771}, -year = {2013} -} -@article{Matplotlib2007, -abstract = {Matplotlib is a 2D graphics package used for Python for application development, interactive scripting, and publication-quality image generation across user interfaces and operating systems.}, -author = {Hunter, J D}, -doi = {10.1109/MCSE.2007.55}, -journal = {Comput Sci Eng}, -number = {3}, -pages = {90--95}, -publisher = {IEEE COMPUTER SOC}, -title = {{Matplotlib: A 2D graphics environment}}, -volume = {9}, -year = {2007} -} -@article{Riess1998, -abstract = {We present observations of 10 type Ia supernovae (SNe Ia) between 0.16 < z < 0.62. With previous data from our High-Z Supernova Search Team, this expanded set of 16 high-redshift supernovae and 34 nearby supernovae are used to place constraints on the Hubble constant (H_0), the mass density (Omega_M), the cosmological constant (Omega_Lambda), the deceleration parameter (q_0), and the dynamical age of the Universe (t_0). The distances of the high-redshift SNe Ia are, on average, 10% to 15% farther than expected in a low mass density (Omega_M=0.2) Universe without a cosmological constant. Different light curve fitting methods, SN Ia subsamples, and prior constraints unanimously favor eternally expanding models with positive cosmological constant (i.e., Omega_Lambda > 0) and a current acceleration of the expansion (i.e., q_0 < 0). With no prior constraint on mass density other than Omega_M > 0, the spectroscopically confirmed SNe Ia are consistent with q_0 <0 at the 2.8 sigma and 3.9 sigma confidence levels, and with Omega_Lambda >0 at the 3.0 sigma and 4.0 sigma confidence levels, for two fitting methods respectively. Fixing a ``minimal'' mass density, Omega_M=0.2, results in the weakest detection, Omega_Lambda>0 at the 3.0 sigma confidence level. For a flat-Universe prior (Omega_M+Omega_Lambda=1), the spectroscopically confirmed SNe Ia require Omega_Lambda >0 at 7 sigma and 9 sigma level for the two fitting methods. A Universe closed by ordinary matter (i.e., Omega_M=1) is ruled out at the 7 sigma to 8 sigma level. We estimate the size of systematic errors, including evolution, extinction, sample selection bias, local flows, gravitational lensing, and sample contamination. Presently, none of these effects reconciles the data with Omega_Lambda=0 and q_0 > 0.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9805201}, -author = {Riess, Adam G. and Filippenko, Alexei V. and Challis, Peter and Clocchiatti, Alejandro and Diercks, Alan and Garnavich, Peter M. and Gilliland, Ron L. and Hogan, Craig J. and Jha, Saurabh and Kirshner, Robert P. and Leibundgut, B. and Phillips, M. M. and Reiss, David and Schmidt, Brian P. and Schommer, Robert A. and Smith, R. Chris and Spyromilio, J. and Stubbs, Christopher and Suntzeff, Nicholas B. and Tonry, John}, -doi = {10.1086/300499}, -eprint = {9805201}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {cosmology,general,observations {\`{e}} supernovae}, -month = {sep}, -number = {3}, -pages = {1009--1038}, -pmid = {7684321}, -primaryClass = {astro-ph}, -title = {{Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant}}, -url = {http://arxiv.org/abs/astro-ph/9805201%0Ahttp://dx.doi.org/10.1086/300499}, -volume = {116}, -year = {1998} -} -@book{10.5555/1593511, -address = {Scotts Valley, CA}, -author = {{Van Rossum}, Guido and Drake, Fred L}, -isbn = {1441412697}, -publisher = {CreateSpace}, -title = {{Python 3 Reference Manual}}, -year = {2009} -} -@article{Massey2010c, -abstract = {We review progress in understanding dark matter by astrophysics, and particularly via the effect of gravitational lensing. Evidences from many different directions now all imply that five sixths of the material content of the Universe is in this mysterious form, separate from and beyond the ordinary 'baryonic' particles in the standard model of particle physics. Dark matter appears not to interact via the electromagnetic force, and therefore neither emits nor reflects light. However, it definitely does interact via gravity, and has played the most important role in shaping the Universe on large scales. The most successful technique with which to investigate it has so far been the effect of gravitational lensing. The curvature of space-time near any gravitating mass (including dark matter) deflects passing rays of light-observably shifting, distorting and magnifying the images of background galaxies. Measurements of such effects currently provide constraints on the mean density of dark matter, and its density relative to baryonic matter; the size and mass of individual dark matter particles and its cross-section under various fundamental forces. {\textcopyright} 2010 IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1001.1739}, -author = {Massey, Richard and Kitching, Thomas and Richard, Johan}, -doi = {10.1088/0034-4885/73/8/086901}, -eprint = {1001.1739}, -isbn = {0034-4885}, -issn = {00344885}, -journal = {Reports on Progress in Physics}, -month = {aug}, -number = {8}, -pages = {437--442}, -title = {{The dark matter of gravitational lensing}}, -volume = {73}, -year = {2010} -} -@article{Iwanus2017, -abstract = {We describe and test a novel dark matter annihilation feedback (DMAF) scheme that has been implemented into the well-known cosmological simulation code GADGET-2. In the models considered here, dark matter can undergo self-annihilation/decay into radiation and baryons. These products deposit energy into the surrounding gas particles and then the dark matter/baryon fluid is self-consistently evolved under gravity and hydrodynamics. We present tests of this new feedback implementation in the case of idealized dark matter haloes with gas components for a range of halomasses, concentrations and annihilation rates. For some darkmattermodels, DMAF's ability to evacuate gas is enhanced in lower mass, concentrated haloes where the injected energy is comparable to its gravitational binding energy. Therefore, we expect the strongest signs of darkmatter annihilation to imprint themselves on to the baryonic structure of concentrated dwarf galaxies through their baryonic fraction and star formation history. Finally, we present preliminary results of the first self-consistent DMAF cosmological box simulations showing that the small-scale substructure is washed out for large annihilation rates.}, -archivePrefix = {arXiv}, -arxivId = {1707.06770}, -author = {Iwanus, N. and Elahi, P. J. and Lewis, G. F.}, -doi = {10.1093/MNRAS/STX1974}, -eprint = {1707.06770}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Iwanus, Elahi, Lewis - 2017 - Dark matter annihilation feedback in cosmological simulations - I Code convergence and idealized haloes(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Large-scale structure of Universe}, -number = {1}, -pages = {1214--1225}, -title = {{Dark matter annihilation feedback in cosmological simulations - I: Code convergence and idealized haloes}}, -url = {http://arxiv.org/abs/1707.06770%0Ahttp://dx.doi.org/10.1093/mnras/stx1974}, -volume = {472}, -year = {2017} -} -@article{Agustsson2007a, -abstract = {We investigate the locations of the satellites of relatively isolated host galaxies in the Sloan Digital Sky Survey and the Millennium Run simulation. Provided we use two distinct prescriptions to embed luminous galaxies within the simulated dark matter halos (ellipticals share the shapes of their halos, while disks have angular momenta that are aligned with the net angular momenta of their halos), we find a fair agreement between observation and theory. Averaged over scales rp 500 kpc, the satellites of red, high-mass hosts with low star formation rates are found preferentially near the major axes of their hosts. In contrast, the satellites of blue, low-mass hosts with low star formation rates show little to no anisotropy when averaged over the same scale. The difference between the locations of the satellites of red and blue hosts cannot be explained by the effects of interlopers in the data. Instead, it is caused primarily by marked differences in the dependence of the mean satellite location, $\phi$, on the projected distance at which the satellites are found. We also find that the locations of red, high-mass satellites with low star formation rates show considerably more anisotropy than do the locations of blue, low-mass satellites with high star formation rates. There are two contributors to this result. First, the blue satellites have only recently arrived within their hosts' halos, while the red satellites arrived in the far distant past. Second, the sample of blue satellites is heavily contaminated by interlopers, which suppresses the measured anisotropy compared to the intrinsic anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {0704.3441}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1088/0004-637X/709/2/1321}, -eprint = {0704.3441}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: dwarf,Galaxies: fundamental parameters,Galaxies: halos,Galaxies: structure}, -number = {2}, -pages = {1321--1336}, -title = {{Anisotropic locations of satellite galaxies: Clues to the orientations of galaxies within their dark matter halos}}, -url = {http://arxiv.org/abs/0704.3441%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/0004-637X/709/2/1321}, -volume = {709}, -year = {2010} -} -@article{VandeSande2016, -abstract = {Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h3 ({\$\sim${}}skewness) and h4 ({\$\sim${}}kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using 2D integral field data from the SAMI Galaxy Survey. A proxy for the spin parameter ({\$}\backslashlambda{\_}{\{}R{\_}e{\}}{\$}) and ellipticity ({\$}\backslashepsilon{\_}e{\$}) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h3 versus {\$}V/\backslashsigma{\$} anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h3 and {\$}V/\backslashsigma{\$}. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h3 versus {\$}V/\backslashsigma{\$} signatures. We identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar {\$}\backslashlambda{\_}{\{}R{\_}e{\}}-\backslashepsilon{\_}e{\$} values can show distinctly different h3-{\$}V/\backslashsigma{\$} signatures. Class 5 objects are previously unidentified fast rotators that show a weak h3 versus {\$}V/\backslashsigma{\$} anti-correlation. These objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h3 versus {\$}V/\backslashsigma{\$} as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.}, -archivePrefix = {arXiv}, -arxivId = {1611.07039}, -author = {van de Sande, Jesse and Bland-Hawthorn, Joss and Fogarty, Lisa M R and Cortese, Luca and D'Eugenio, Francesco and Croom, Scott M and Scott, Nicholas and Allen, James T and Brough, Sarah and Bryant, Julia J and Cecil, Gerald and Colless, Matthew and Couch, Warrick J and Davies, Roger and Elahi, Pascal J and Foster, Caroline and Goldstein, Gregory and Goodwin, Michael and Groves, Brent and Ho, I-Ting and Jeong, Hyunjin and Jones, D Heath and Konstantopoulos, Iraklis S and Lawrence, Jon S and Leslie, Sarah K and L{\'{o}}pez-S{\'{a}}nchez, {\'{A}}ngel R and McDermid, Richard M and McElroy, Rebecca and Medling, Anne M and Oh, Sree and Owers, Matt S and Richards, Samuel N and Schaefer, Adam L and Sharp, Rob and Sweet, Sarah M and Taranu, Dan and Tonini, Chiara and Walcher, C Jakob and Yi, Sukyoung K}, -doi = {10.3847/1538-4357/835/1/104}, -eprint = {1611.07039}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cosmology,dynamics,evolution,formation,galaxies,kinematics and,observations,stellar content,structure}, -number = {1}, -pages = {104}, -title = {{the Sami Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics}}, -url = {http://arxiv.org/abs/1611.07039%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/835/1/104}, -volume = {835}, -year = {2017} -} -@article{Massey2010b, -abstract = {We update a physically motivated model of radiation damage in the Hubble Space Telescope Advanced Camera for Surveys/Wide Field Channel, using data up to mid-2010. We find that charge transfer inefficiency increased dramatically before shuttle Servicing Mission 4, with $\sim$1.3 charge traps now present per pixel. During detector readout, charge traps spuriously drag electrons behind all astronomical sources, degrading image quality in a way that affects object photometry, astrometry and morphology. Our detector readout model is robust to changes in operating temperature and background level, and can be used to iteratively remove the trailing by pushing electrons back to where they belong. The result is data taken in mid-2010 that recovers the quality of imaging obtained within the first six months of orbital operations. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1009.4335}, -author = {Massey, Richard}, -doi = {10.1111/j.1745-3933.2010.00959.x}, -eprint = {1009.4335}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Massey - 2010 - Charge transfer inefficiency in the Hubble Space Telescope since Servicing Mission 4(2).pdf:pdf}, -issn = {17453933}, -journal = {MNRAS Letters}, -keywords = {Instrumentation: detectors,Methods: data analysis,Space vehicles: instruments,Techniques: image processing}, -month = {nov}, -number = {1}, -pages = {L109--L113}, -title = {{Charge transfer inefficiency in the Hubble Space Telescope since Servicing Mission 4}}, -volume = {409}, -year = {2010} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, n=10[cm-3], results in strong expansion of the DM halo in galaxies with stellar masses in the range 107.5 ≤ Mstar ≤ 109.5 M⊙. We find that lower thresholds such as n = 0.1 (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e. ≤50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with n = 10 have gas fractions of ∼0.2 and variations of ∼0.1, while n = 0.1 simulations have order of magnitude lower gas fractions and hence do not expand the halo. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with n = 0.1 and n = 1, but in a reasonable agreement with n = 10. Star formation rates are more variable for higher n, lower galaxy masses, and when star formation is measured on shorter time-scales. For example, simulations with n = 10 have up to 0.4 dex higher scatter in specific star formation rates than simulations with n = 0.1. Thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625}, -author = {Dutton, Aaron A. and MacCi{\`{o}}, Andrea V. and Buck, Tobias and Dixon, Keri L. and Blank, Marvin and Obreja, Aura}, -doi = {10.1093/mnras/stz889}, -eprint = {1811.10625}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dutton et al. - 2019 - NIHAO XX The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure,methods: numerical}, -number = {1}, -pages = {655--671}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://arxiv.org/abs/1811.10625%0Ahttp://dx.doi.org/10.1093/mnras/stz889}, -volume = {486}, -year = {2019} -} -@article{Gonzalez2009, -abstract = {The huge size and uniformity of the Sloan Digital Sky Survey (SDSS) make possible an exacting test of current models of galaxy formation. We compare the predictions of the galform semi-analytical galaxy formation model for the luminosities, morphologies, colours and scalelengths of local galaxies. galform models the luminosity and size of the disc and bulge components of a galaxy, and so we can compute quantities which can be compared directly with SDSS observations, such as the Petrosian magnitude and the S{\'{e}}rsic index. We test the predictions of two published models set in the cold dark matter cosmology: the Baugh et al. model, which assumes a top-heavy initial mass function (IMF) in starbursts and superwind feedback, and the Bower et al. model, which uses active galactic nucleus feedback and a standard IMF. The Bower et al. model better reproduces the overall shape of the luminosity function, the morphology-luminosity relation and the colour bimodality observed in the SDSS data, but gives a poor match to the size-luminosity relation. The Baugh et al. model successfully predicts the size-luminosity relation for late-type galaxies. Both models fail to reproduce the sizes of bright early-type galaxies. These problems highlight the need to understand better both the role of feedback processes in determining galaxy sizes, in particular the treatment of the angular momentum of gas reheated by supernovae, and the sizes of the stellar spheroids formed by galaxy mergers and disc instabilities. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0812.4399}, -author = {Gonz{\'{a}}lez, Juan E. and Lacey, C. G. and Baugh, C. M. and Frenk, C. S. and Benson, A. J.}, -doi = {10.1111/j.1365-2966.2009.15057.x}, -eprint = {0812.4399}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {aug}, -number = {3}, -pages = {1254--1274}, -title = {{Testing model predictions of the cold dark matter cosmology for the sizes, colours, morphologies and luminosities of galaxies with the SDSS}}, -volume = {397}, -year = {2009} -} -@misc{Johannesen2007, -abstract = {As the field of autoimmune neurology develops, the role of the neurologist in the management of patients with systemic autoimmune disease is increasing. This chapter briefly reviews the neurologic manifestations, diagnostic approach, and treatment of neurosarcoidosis, IgG-4-related disease, Beh{\c{c}}et syndrome, Sj{\"{o}}gren syndrome, lupus, and rheumatoid arthritis. The neurologic manifestations of these conditions include parenchymal brain and brainstem disease, myelopathy, radiculopathy, myopathy, and all forms of peripheral neuropathy. Recognizing when a neurologic concern is related to immune-mediated or alternative mechanisms is a critical role for the neurologist as treatment decisions may be based on this assessment. Familiarity with the neurologic manifestations of systemic rheumatologic disease is therefore critical. The approach to treatment depends on the underlying mechanisms of disease and decisions should be made in consultation with other experts assisting in the clinical care of an individual patient.}, -author = {Bradshaw, Michael J. and Bhattacharyya, Shamik and Venna, Nagagopal and Cahill, Jonathan F.}, -booktitle = {Current Clinical Neurology}, -doi = {10.1007/978-3-030-24436-1_17}, -issn = {25244043}, -keywords = {Autoimmune neurology,Beh{\c{c}}et,IgG-4-related disease,Neuro-rheumatology,Neurologic complications,Neurosarcoidosis,Rheumatoid arthritis,Rheumatology,Sj{\"{o}}gren syndrome,Systemic lupus erythematosus}, -pages = {321--342}, -title = {{Neurologic Manifestations of Systemic Rheumatologic Diseases}}, -volume = {07/80}, -year = {2020} -} -@article{Devour2017, -abstract = {Accurate measurement of galaxy structures is a prerequisite for quantitative investigation of galaxy properties or evolution. Yet, the impact of galaxy inclination and dust on commonly used metrics of galaxy structure is poorly quantified. We use infrared data sets to select inclination-independent samples of disc and flattened elliptical galaxies. These samples show strong variation in S$\backslash$'{\{}e{\}}rsic index, concentration, and half-light radii with inclination. We develop novel inclination-independent galaxy structures by collapsing the light distribution in the near-infrared on to the major axis, yielding inclination-independent `linear' measures of size and concentration. With these new metrics we select a sample of Milky Way analogue galaxies with similar stellar masses, star formation rates, sizes and concentrations. Optical luminosities, light distributions, and spectral properties are all found to vary strongly with inclination: When inclining to edge-on, {\$}r{\$}-band luminosities dim by {\$}{\textgreater}{\$}1 magnitude, sizes decrease by a factor of 2, `dust-corrected' estimates of star formation rate drop threefold, metallicities decrease by 0.1 dex, and edge-on galaxies are half as likely to be classified as star forming. These systematic effects should be accounted for in analyses of galaxy properties.}, -archivePrefix = {arXiv}, -arxivId = {1702.06528}, -author = {Devour, Brian M and Bell, Eric F}, -doi = {10.1093/mnrasl/slx021}, -eprint = {1702.06528}, -issn = {1745-3925}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {dust,extinction,galaxies,general,photometric,techniques}, -number = {1}, -pages = {L31----L35}, -pmid = {18462818}, -title = {{Revealing strong bias in common measures of galaxy properties using new inclination-independent structures}}, -url = {http://arxiv.org/abs/1702.06528%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnrasl/slx021}, -volume = {468}, -year = {2017} -} -@article{Christensen2014, -abstract = {We present a detailed comparison between the photometric properties of the bulges of two simulated galaxies and those of a uniform sample of observed galaxies. This analysis shows that the simulated galaxies have bulges with realistic surface brightnesses for their sizes and magnitude. These two field disc galaxies have rotational velocities ̃100 km s-1 and were integrated to a redshift of zero in a fully cosmological $\delta$ cold dark matter context as part of high-resolution smoothed particle hydrodynamic simulations. We performed bulge- disc decompositions of the galaxies using artificial observations, in order to conduct a fair comparison to observations. We also dynamically decomposed the galaxies and compared the star formation histories of the bulges to those of the entire galaxies. These star formation histories showed that the bulges were primarily formed before z = 1 and during periods of rapid star formation. Both galaxies have large amounts of early star formation, which is likely related to the relatively high bulge-to-disc ratios also measured for them. Unlike almost all previous cosmological simulations, the realistically concentrated bulges of these galaxies do not lead to unphysically high rotational velocities, causing them to naturally lie along the observed Tully-Fisher relation. {\textcopyright}2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1402.2702}, -author = {Christensen, C R and Brooks, A M and Fisher, D B and Governato, F and McCleary, J and Quinn, T R and Shen, S and Wadsley, J}, -doi = {10.1093/mnrasl/slu020}, -eprint = {1402.2702}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Bulges,Formation,Galaxies,Methods,Numerical,Spiral,Structure}, -number = {1}, -pages = {1--6}, -title = {{Simulating disc galaxy bulges that are consistent with observed scaling relations}}, -volume = {440}, -year = {2014} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{More2012a, -abstract = {We present the Strong Lensing Legacy Survey-ARCS (SARCS) sample compiled from the final T0006 data release of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) covering a total non-overlapping area of 159deg2. We adopt a semi-automatic method to find gravitational arcs in the survey that makes use of an arc-finding algorithm. The candidate list is pruned by visual inspection and ranking to form the final SARCS sample. This list also includes some serendipitously discovered lens candidates which the automated algorithm did not detect. The SARCS sample consists of 127 lens candidates which span arc radii ∼2″-18″ within the unmasked area of ∼150deg 2. Within the sample, 54 systems are promising lenses among which, we find 12 giant arcs (length-to-width ratio ≥8). We also find two radial arc candidates in SL2SJ141447+544704. From our sample, we detect a systematic alignment of the giant arcs with the major axis of the baryonic component of the putative lens in concordance with previous studies. This alignment is also observed for all arcs in the sample and does not vary significantly with increasing arc radius. The mean values of the photometric redshift distributions of lenses corresponding to the giant arcs and all arcs sample are at z ∼ 0.6. Owing to the large area and depth of the CFHTLS, we find the largest sample of lenses probing mass scales that are intermediate to cluster and galaxy lenses for the first time. We compare the observed image separation distribution (ISD) of our arcs with theoretical models. A two-component density profile for the lenses which accounts for both the central galaxy and the dark matter component is required by the data to explain the observed ISD. Unfortunately, current levels of uncertainties anddegeneracies accommodate models both with and without adiabatic contraction. We also show the effects of changing parameters of the model that predict the ISD and that a larger lens sample might constrain relations such as the concentration-mass relation, mass-luminosity relation, and the faint-end slope of the luminosity function. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1109.1821}, -author = {More, A. and Cabanac, R. and More, S. and Alard, C. and Limousin, M. and Kneib, J. P. and Gavazzi, R. and Motta, V.}, -doi = {10.1088/0004-637X/749/1/38}, -eprint = {1109.1821}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/More2012SARCS.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {dark matter,gravitational lensing: strong,methods: data analysis,surveys}, -number = {1}, -title = {{The CFHTLS-strong Lensing Legacy Survey (SL2S): Investigating the group-scale lenses with the SARCS sample}}, -volume = {749}, -year = {2012} -} -@inproceedings{MartinNavarro2013, -author = {Mart$\backslash$'$\backslash$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Khochfar2011, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}R{\$}. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the {\$}\backslash{\$}atl survey, assuming that fast rotating ETGs have at least 10{\%} of their total stellar mass in a disc component. In agreement with {\$}\backslash{\$}atl observations we find that slow rotators are predominantly galaxies with {\$} M{\_}* {\textgreater}10{\^{}}{\{}10.5{\}}{\$} M{\$}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} contributing {\$}\backslashbackslashsim 20{\%}{\$} to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between {\$}\backslashbackslashsim 50{\%} -90{\%}{\$} of their stellar mass from satellites and their most massive progenitors have on average up to 3 major mergers during their evolution. Fast rotators in contrast, accrete less than 50{\%} and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stops, galaxies grow via infall from satellites. Frequent minor mergers thereby, destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}R{\$} into the slow rotator regime. Abridged...}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M and Cappellari, Michele and Davies, Roger L and Davis, Timothy A and de Zeeuw, P T and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: structure,cD}, -month = {oct}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3Dproject - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within {\$}\Lambda{\$}CDM}}, -volume = {417}, -year = {2011} -} -@article{Shi2015, -abstract = {We study how halo intrinsic dynamical properties are linked to their formation processes for halos in two mass ranges, 1012-1012.5 h-1M⊙ and ≥1013 h-1M⊙, and how both are correlated with the large-scale tidal field within which the halos reside at present. We identify infall halos that are about to merge with their hosts. We find that the tangential infall velocity increases significantly with the strength of the tidal field, but no strong correlation is found for the radial component. These results can be used to explain the environmental dependence of internal velocity anisotropy and spin of halos. The position vectors and velocities of infall halos are aligned with the principal axes of the tidal field, and the alignment depends on the strength of the tidal field. Opposite accretion patterns are found in weak and strong tidal fields, showing that in a weak field the accretion flow is dominated by radial motion within the local structure, while a large tangential component is present in a strong field. These findings can be used to understand the strong alignments we find between the principal axes of the internal velocity ellipsoids of halos and the tidal field, and their dependence on the strength of the tidal field. We further find that only in weak tidal fields does the spin-tidal field alignment follow the prediction of the tidal torque theory. We discuss how our results may be used to understand the spins of disk galaxies and velocity structures of elliptical galaxies and their correlations with large-scale structure.}, -archivePrefix = {arXiv}, -arxivId = {1501.07764}, -author = {Shi, Jingjing and Wang, Huiyuan and Mo, H. J.}, -doi = {10.1088/0004-637X/807/1/37}, -eprint = {1501.07764}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shi, Wang, Mo - 2015 - Flow Patterns Around Dark Matter Halos the Link Between Halo Dynamical Properties and Large-Scale Tidal Field(2).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: halos,large-scale structure of universe,methods: statistical}, -number = {1}, -title = {{Flow Patterns Around Dark Matter Halos: the Link Between Halo Dynamical Properties and Large-Scale Tidal Field}}, -volume = {807}, -year = {2015} -} -@article{Huang2018, -abstract = {We use {\$\sim${}}100 square deg of deep ({\textgreater}28.5 mag arcsec{\$}{\^{}}{\{}-2{\}}{\$} in i-band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach {\$\sim${}}4 magnitudes deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with {\$}\backslashbackslashlog M{\_}{\{}\backslashbackslashstar, 100\backslash\backslashbackslashmathrm{\{}\backslash{\{}{\}}kpc{\{}\backslash{\}}{\}}{\}}{\textgreater}11.6{\$} in more massive haloes at 0.3 {\textless}z {\textless}0.5 have shallower inner stellar mass density profiles (within {\$\sim${}}10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with {\$}\backslashbackslashlog M{\_}{\{}\backslashbackslashrm{\{}\backslash{\{}{\}}Halo{\{}\backslash{\}}{\}}{\}}{\textgreater}14.0{\$} are {\$\sim${}}20{\%} larger in {\$}R{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}50{\{}\backslash{\}}{\}}{\}}{\$} at fixed stellar mass. Such dependence is also reflected in the relationship between the stellar mass within 10 and 100 kpc. Comparing to the mass--size relation, the {\$}\backslashbackslashlog M{\_}{\{}\backslashbackslashstar, 100\backslash\backslashbackslashrm{\{}\backslash{\{}{\}}kpc{\{}\backslash{\}}{\}}{\}}{\$}-{\$}\backslashbackslashlog M{\_}{\{}\backslashbackslashstar, 10\backslash\backslashbackslashrm{\{}\backslash{\{}{\}}kpc{\{}\backslash{\}}{\}}{\}}{\$} relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287----a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{Wang2016, -abstract = {Astronomical observations are affected by several kinds of noise, each with its own causal source; there is photon noise, stochastic source variability, and residuals coming from imperfect calibration of the detector or telescope. The precision of NASA Kepler photometry for exoplanet science—the most precise photometric measurements of stars ever made—appears to be limited by unknown or untracked variations in spacecraft pointing and temperature, and unmodeled stellar variability. Here, we present the causal pixel model (CPM) for Kepler data, a data-driven model intended to capture variability but preserve transit signals. The CPM works at the pixel level so that it can capture very fine-grained information about the variation of the spacecraft. The CPM models the systematic effects in the time series of a pixel using the pixels of many other stars and the assumption that any shared signal in these causally disconnected light curves is caused by instrumental effects. In addition, we use the target star's future and past (autoregression). By appropriately separating, for each data point, the data into training and test sets, we ensure that information about any transit will be perfectly isolated from the model. The method has four tuning parameters—the number of predictor stars or pixels, the autoregressive window size, and two L2-regularization amplitudes for model components, which we set by cross-validation. We determine values for tuning parameters that works well for most of the stars and apply the method to a corresponding set of target stars. We find that CPM can consistently produce low-noise light curves. In this paper, we demonstrate that pixel-level de-trending is possible while retaining transit signals, and we think that methods like CPM are generally applicable and might be useful for K2, TESS, etc., where the data are not clean postage stamps like Kepler.}, -archivePrefix = {arXiv}, -arxivId = {1508.01853}, -author = {Wang, Dun and Hogg, David W. and Foreman-Mackey, Daniel and Sch{\"{o}}lkopf, Bernhard}, -doi = {10.1088/1538-3873/128/967/094503}, -eprint = {1508.01853}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2016 - A causal, data-driven approach to modeling the Kepler data(2).pdf:pdf}, -issn = {00046280}, -journal = {Publ. Astron. Soc. Pac.}, -keywords = {Methods: data analysis}, -number = {967}, -pages = {1--13}, -publisher = {IOP Publishing}, -title = {{A causal, data-driven approach to modeling the Kepler data}}, -url = {http://dx.doi.org/10.1088/1538-3873/128/967/094503}, -volume = {128}, -year = {2016} -} -@article{Hildebrandt2017, -abstract = {We present cosmological parameter constraints from a tomographic weak gravitational lensing analysis of $\sim$450 deg2 of imaging data from the Kilo Degree Survey (KiDS). For a flat $\lambda$CDM cosmology with a prior on H0 that encompasses the most recent direct measurements, we find S8 ≡ $\sigma$8 √$\omega$m/0.3 = 0.745±0.039. This result is in good agreement with other low redshift probes of large scale structure, including recent cosmic shear results, along with pre-Planck cosmic microwave background constraints. A 2.3-$\sigma$ tension in S8 and `substantial discordance' in the full parameter space is found with respect to the Planck 2015 results. We use shear measurements for nearly 15 million galaxies, determined with a new improved `self-calibrating' version of lens fit validated using an extensive suite of image simulations. Four-band ugri photometric redshifts are calibrated directly with deep spectroscopic surveys. The redshift calibration is confirmed using two independent tech- niques based on angular cross-correlations and the properties of the photometric redshift probability distributions. Our covariance matrix is determined using an analytical approach, verified numeri- cally with large mock galaxy catalogues. We account for uncertainties in the modelling of intrinsic galaxy alignments and the impact of baryon feedback on the shape of the non-linear matter power spectrum, in addition to the small residual uncertainties in the shear and redshift calibration. The cosmology analysis was performed blind. Our high-level data products, including shear correlation functions, covariance matrices, redshift distributions, and Monte Carlo Markov Chains.}, -archivePrefix = {arXiv}, -arxivId = {1606.05338}, -author = {Hildebrandt, H. and Viola, M. and Heymans, C. and Joudaki, S. and Kuijken, K. and Blake, C. and Erben, T. and Joachimi, B. and Klaes, D. and Miller, L. and Morrison, C. B. and Nakajima, R. and {Verdoes Kleijn}, G. and Amon, A. and Choi, A. and Covone, G. and de Jong, J. T.A. and Dvornik, A. and {Fenech Conti}, I. and Grado, A. and Harnois-D{\'{e}}raps, J. and Herbonnet, R. and Hoekstra, H. and K{\"{o}}hlinger, F. and McFarland, J. and Mead, A. and Merten, J. and Napolitano, N. and Peacock, J. A. and Radovich, M. and Schneider, P. and Simon, P. and Valentijn, E. A. and van den Busch, J. L. and van Uitert, E. and {Van Waerbeke}, L.}, -doi = {10.1093/mnras/stw2805}, -eprint = {1606.05338}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hildebrandt et al. - 2017 - KiDS-450 Cosmological parameter constraints from tomographic weak gravitational lensing.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmology,Observations - gravitational lensing,Weak - galaxies,pho-tometry - surveys}, -number = {2}, -pages = {1--50}, -title = {{KiDS-450: Cosmological parameter constraints from tomographic weak gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Sirianni2004, -abstract = {The Advanced Camera for Surveys (ACS), installed in the Hubble Space Telescope (HST) in March 2002, comprises three cameras: the Wide Field Camera (WFC), designed for deep near-IR survey imaging programs; the High Resolution Camera (HRC), a high angular resolution imager which fully samples the HST full spread function (PSF) in the visible; and the Solar Blind Camera (SBC), a far-UV imager. The WFC and HRC employ CCD detectors. Their performances are affected by the on-going damage due to the space radiation environment where they operate. We present an overview of the performance of the ACS CCD detectors, based on the first two years of flight science operations. We analyze the evolution with time of the basic detector performance that are subjected to degradation due to the on-going radiation damage. Comparison is made with ground testing prediction and with the amount of performance degradation seen in other CCD detectors on board of HST.}, -author = {Sirianni, Marco and Mutchler, Max and Clampin, Mark and Ford, Holland and Illingworth, Garth and Hartig, George and van Orsow, Doug and Wheeler, Thomas}, -doi = {10.1117/12.552584}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sirianni et al. - 2004 - Performance of the Advanced Camera for Surveys CCDs after two years on orbit.pdf:pdf}, -issn = {0277786X}, -journal = {Optical and Infrared Detectors for Astronomy}, -number = {January 2014}, -pages = {173}, -title = {{Performance of the Advanced Camera for Surveys CCDs after two years on orbit}}, -volume = {5499}, -year = {2004} -} -@article{Jaroszynski2012, -abstract = {We investigate strong lensing by non-singular finite isothermal ellipsoids taking into account the influence of the matter along the line of sight and in the close lens vicinity. We compare three descriptions of light propagation: the full approach taking into account all matter inhomogeneities along the rays; the single plane approach, where we take into account the influence of the strong lens neighbours but neglect the foreground and background objects; and the single lens approach. In each case, we simulate many strong lensing configurations placing a point source at the same redshift but in different locations inside the region surrounded by caustics. We further analyse configurations of four or five images. For every simulated strong lensing configuration, we attempt to fit a simplified lens model using a single isothermal ellipsoid or a single isothermal ellipsoid with external shear. The single lens fits to configurations obtained in the full approach are rejected in majority of cases with 95per cent significance. For configurations obtained in the single plane approach, the rejection rate is substantially lower. Also the inclusion of external shear in simplified modelling improves the chances of obtaining acceptable fits, but the problem is not solved completely. The quantitative estimates of the rates of rejection of simplified models depend on the required accuracy of the models, and we present few illustrative examples, which show that both matter close to the lens and matter along the rays do have important influence on lens modelling. We also estimate the typical value of the external shear and compare the fitted parameters of the simplified models with the parameters of the lenses used in the simulations. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1204.6223}, -author = {Jaroszynski, M and Kostrzewa-Rutkowska, Z}, -doi = {10.1111/j.1365-2966.2012.21197.x}, -eprint = {1204.6223}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: strong,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {1}, -pages = {325--332}, -title = {{Background, foreground and nearby matter influence on strong gravitational lenses}}, -volume = {424}, -year = {2012} -} -@article{Shi1999, -abstract = {We propose a new and unique dark matter candidate: ∼ 100 eV to ∼ 10 keV sterile neutrinos produced via lepton-number-driven resonant Mikheyev-Smirnov-Wolfenstein conversion of active neutrinos. The requisite lepton number asymmetries in any of the active neutrino flavors range from 10-3to 10-1of the photon number. The unique feature here is that the adiabaticity condition of the resonance strongly favors the production of lower energy sterile neutrinos. The resulting nonthermal (cold) energy spectrum can cause these sterile neutrinos to revert to nonrelativistic kinematics at an early epoch, so that free-streaming lengths at or below the dwarf galaxy scale are possible. Therefore, the main problem associated with light neutrino dark matter can be circumvented in our model. {\textcopyright} 1999 The American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9810076}, -author = {Shi, Xiangdong and Fuller, George M.}, -doi = {10.1103/PhysRevLett.82.2832}, -eprint = {9810076}, -isbn = {978-1-62410-071-0}, -issn = {10797114}, -journal = {Physical Review Letters}, -month = {apr}, -number = {14}, -pages = {2832--2835}, -pmid = {19482328}, -primaryClass = {astro-ph}, -title = {{New dark matter candidate: Nonthermal sterile neutrinos}}, -url = {http://link.aps.org/doi/10.1103/PhysRevLett.82.2832}, -volume = {82}, -year = {1999} -} -@article{Jimenez-Vicente2019, -abstract = {We present a new approach in the study of the Initial Mass function (IMF) in external galaxies based on quasar microlensing observations. We use measurements of quasar microlensing magnifications in 24 lensed quasars to estimate the average mass of the stellar population in the lens galaxies without any a priori assumption on the shape of the IMF. The estimated mean mass of the stars is {\$}\backslashlangle M \backslashrangle =0.16{\^{}}{\{}+0.05{\}}{\_}{\{}-0.08{\}} M{\_}\backslashodot{\$} (at 68$\backslash${\%} confidence level). We use this average mass to put constraints into two important parameters characterizing the IMF of lens galaxies: the low-mass slope, {\$}\backslashalpha{\_}2{\$}, and the low-mass cutoff, {\$}M{\_}{\{}low{\}}{\$}. Combining these constraints with prior information based on lensing, stellar dynamics, and absorption spectral feature analysis, we calculate the posterior probability distribution for the parameters {\$}M{\_}{\{}low{\}}{\$} and {\$}\backslashalpha{\_}2{\$}. We estimate values for the low-mass end slope of the IMF {\$}\backslashlangle \backslashalpha{\_}2\backslashrangle=-2.6\backslashpm 0.9{\$} (heavier than that of the Milky Way) and for the low-mass cutoff {\$}\backslashlangle M{\_}{\{}low{\}}\backslashrangle=0.13\backslashpm0.07{\$}. These results are in good agreement with previous studies on these parameters and remain stable against the choice of different suitable priors.}, -archivePrefix = {arXiv}, -arxivId = {1910.10509}, -author = {Jim{\'{e}}nez-Vicente, J and Mediavilla, E}, -doi = {10.3847/1538-4357/ab46b8}, -eprint = {1910.10509}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {75}, -title = {{The Initial Mass Function of Lens Galaxies from Quasar Microlensing}}, -url = {http://arxiv.org/abs/1910.10509%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/ab46b8}, -volume = {885}, -year = {2019} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{LSSTDarkEnergyScienceCollaboration2012, -abstract = {This white paper describes the LSST Dark Energy Science Collaboration (DESC), whose goal is the study of dark energy and related topics in fundamental physics with data from the Large Synoptic Survey Telescope (LSST). It provides an overview of dark energy science and describes the current and anticipated state of the field. It makes the case for the DESC by laying out a robust analytical framework for dark energy science that has been defined by its members and the comprehensive three-year work plan they have developed for implementing that framework. The analysis working groups cover five key probes of dark energy: weak lensing, large scale structure, galaxy clusters, Type Ia supernovae, and strong lensing. The computing working groups span cosmological simulations, galaxy catalogs, photon simulations and a systematic software and computational framework for LSST dark energy data analysis. The technical working groups make the connection between dark energy science and the LSST system. The working groups have close linkages, especially through the use of the photon simulations to study the impact of instrument design and survey strategy on analysis methodology and cosmological parameter estimation. The white paper describes several high priority tasks identified by each of the 16 working groups. Over the next three years these tasks will help prepare for LSST analysis, make synergistic connections with ongoing cosmological surveys and provide the dark energy community with state of the art analysis tools. Members of the community are invited to join the LSST DESC, according to the membership policies described in the white paper. Applications to sign up for associate membership may be made by submitting the Web form at http://www.slac.stanford.edu/exp/lsst/desc/signup.html with a short statement of the work they wish to pursue that is relevant to the LSST DESC.}, -archivePrefix = {arXiv}, -arxivId = {1211.0310}, -author = {{LSST Dark Energy Science Collaboration}}, -eprint = {1211.0310}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/LSST Dark Energy Science Collaboration - 2012 - Large Synoptic Survey Telescope Dark Energy Science Collaboration.pdf:pdf}, -journal = {arXiv preprint arXiv:1211.0310}, -keywords = {Astrophysics - Cosmology and Extragalactic Astroph,High Energy Physics - Experiment}, -pages = {133}, -title = {{Large Synoptic Survey Telescope: Dark Energy Science Collaboration}}, -url = {http://arxiv.org/abs/1211.0310}, -year = {2012} -} -@article{Governato2015, -abstract = {We use high resolution Hydro{\$}+{\$}N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass {\$\sim${}} 10{\$}{\^{}}{\{}6-7{\}}{\$} M{\$}\backslashbackslashodot{\{}\backslash{\$}{\}}, total mass 10{\$}{\^{}}{\{}10{\}}{\$} M{\$}\backslashbackslashodot{\{}\backslash{\$}{\}} in {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}} dominated CDM and 2keV WDM cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the DM model, but proportionally to the SF efficiency, gas outflows lower the central mass density through `dynamical heating', such that all realizations have circular velocities {\$}{\textless}{\$} 20kms at 500{\$}{\\sim{}}{\$}pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial color-magnitude diagrams and star formation histories in order to directly compare to available observations. The simulated galaxies formed most of their stars in many {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including `baryon physics' in simulations when 1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and 2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F and Weisz, D and Pontzen, A and Loebman, S and Reed, D and Brooks, A M and Behroozi, P and Christensen, C and Madau, P and Mayer, L and Shen, S and Walker, M and Quinn, T and Keller, B W and Wadsley, J}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Ikarashi2014, -abstract = {We report the source size distribution, as measured by ALMA millimetric continuum imaging, of a sample of 13 AzTEC-selected submillimeter galaxies (SMGs) at zphot ∼ 3-6. Their infrared luminosities and star formation rates (SFRs) are LIR∼ 2-6 × 1012 L⊙ and ∼200-600 M⊙ yr1, respectively. The sizes of these SMGs range from 0″ 10 to 0″ 38, with a median of 0″ 20 -0″05+0″03 (FWHM), corresponding to a median circularized effective radius (Rc,e) of 0.67-0.14+0.13 kpc, comparable to the typical size of the stellar component measured in compact quiescent galaxies at z ∼ 2 (cQGs)-Re ∼ 1 kpc. The median surface SFR density of our SMGs is 100-26+42 M yr1 kpc2, comparable to that seen in local merger-driven (U)LIRGs rather than in extended disk galaxies at low and high redshifts. The discovery of compact starbursts in z ≳ 3 SMGs strongly supports a massive galaxy formation scenario wherein z ∼ 3-6 SMGs evolve into the compact stellar components of z ∼ 2 cQGs. These cQGs are then thought to evolve into the most massive ellipticals in the local universe, mostly via dry mergers. Our results thus suggest that z ≳ 3 SMGs are the likely progenitors of massive local ellipticals, via cQGs, meaning that we can now trace the evolutionary path of the most massive galaxies over a period encompassing ∼90% of the age of the universe.}, -archivePrefix = {arXiv}, -arxivId = {1411.5038}, -author = {Ikarashi, Soh and Ivison, R. J. and Caputi, Karina I. and Aretxaga, Itziar and Dunlop, James S. and Hatsukade, Bunyo and Hughes, David H. and Iono, Daisuke and Izumi, Takuma and Kawabe, Ryohei and Kohno, Kotaro and Lagos, Claudia D.P. and Motohara, Kentaro and Nakanishi, Kouichiro and Ohta, Kouji and Tamura, Yoichi and Umehata, Hideki and Wilson, Grant W. and Yabe, Kiyoto and Yun, Min S.}, -doi = {10.1088/0004-637X/810/2/133}, -eprint = {1411.5038}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: high-redshift,submillimeter: galaxies}, -number = {2}, -pages = {133}, -title = {{Compact starbursts in z ∼ 3-6 submillimeter galaxies revealed by ALMA}}, -url = {http://stacks.iop.org/0004-637X/810/i=2/a=133?key=crossref.086f0a3643102b0606542cef2c0a73d3}, -volume = {810}, -year = {2015} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned r- and g-band images from a sample of 45 508 galaxies from Sloan Digital Sky Survey Data Release 9 in the redshift range 0.06≤z≤0.1 and in the mass range 1010.0M⊙ {\textless}M* {\textless} 1011.4M⊙.We derive surface brightness profiles to a depth of almost $\mu$r ̃ 32 mag arcsec-2. We find that the ellipticity of the stellar halo is a function of galaxy stellar mass and that the haloes of high-concentration galaxies are more elliptical than those of low-concentration galaxies. Where the g - r colour of the stellar halo can be measured, we find that the stellar light is always bluer than in the main galaxy. The colour of the stellar halo is redder for more massive galaxies. We further demonstrate that the full two-dimensional surface intensity distribution of our galaxy stacks can only be fit through multicomponent S{\'{e}}rsic models. Using the fraction of light in the outer component of the models as a proxy for the fraction of accreted stellar light, we show that this fraction is a function of stellar mass and galaxy type. The fraction of accreted stellar light rises from 30 to 70 per cent and from 2 to 25 per cent for high- and low-concentration galaxies, respectively, over the mass range 1010.0-1011.4M⊙. {\textcopyright}2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1404.2123}, -author = {D'Souza, Richard and Kauffman, Guinevere and Wang, Jing and Vegetti, Simona}, -doi = {10.1093/mnras/stu1194}, -eprint = {1404.2123}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: halo,Galaxy: structure}, -number = {2}, -pages = {1433--1450}, -title = {{Parametrizing the stellar haloes of galaxies}}, -volume = {443}, -year = {2014} -} -@article{Brewer2016, -abstract = {We introduce a Bayesian solution to the problem of inferring the density profile of strong gravitational lenses when the lens galaxy may contain multiple dark or faint substructures. The source and lens models are based on a superposition of an unknown number of non-negative basis functions (or 'blobs') whose form was chosen with speed as a primary criterion. The prior distribution for the blobs' properties is specified hierarchically, so the mass function of substructures is a natural output of the method. We use reversible jump Markov Chain Monte Carlo within Diffusive Nested Sampling to sample the posterior distribution and evaluate the marginal likelihood of the model, including the summation over the unknown number of blobs in the source and the lens. We demonstrate the method on two simulated data sets: one with a single substructure, and the other with 10. We also apply the method to the g-band image of the 'Cosmic Horseshoe' system, and find evidence for more than zero substructures. However, these have large spatial extent and probably only point to misspecifications in the model (such as the shape of the smooth lens component or the point-spread function), which are difficult to guard against in full generality.}, -archivePrefix = {arXiv}, -arxivId = {1508.00662}, -author = {Brewer, Brendon J. and Huijser, David and Lewis, Geraint F.}, -doi = {10.1093/mnras/stv2370}, -eprint = {1508.00662}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Gravitational lensing: strong,Methods: data analysis,Methods: statistical}, -month = {jan}, -number = {2}, -pages = {1819--1829}, -title = {{Trans-dimensional Bayesian inference for gravitational lens substructures}}, -url = {http://arxiv.org/abs/1508.00662}, -volume = {455}, -year = {2020} -} -@article{Sales2012, -abstract = {In the simplest scenario, disk galaxies form predominantly in halos with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly-rotating remnants of repeated merging events. We explore these assumptions using one hundred systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations GIMIC. At z=0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disk galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: disks form in halos with high and low net spin, and mergers play a negligible role in the formation of spheroid stars, most of which form in-situ. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly-accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Disks, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier-accreted material. Gas accretion from a hot corona thus favours disk formation, whereas gas that flows "cold", often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, most spheroids consist of superpositions of stellar components with distinct kinematics, age, and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology is imprinted early by the interplay of the tidal field and the shape of the material destined to form the galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {jun}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@techreport{Grogin2010, -author = {Grogin, N.$\sim$A. and Lucas, R and Golimowski, D and Biretta, J}, -booktitle = {Space Telescope WFPC2 Instrument Science Report}, -keywords = {HST,Hubble Space Telescope,Space Telescope Science Institute,WFPC 2,Wide Field Camera 2}, -month = {aug}, -title = {{WFPC2 CTE for Extended Sources: I. Photometric Correction}}, -year = {2010} -} -@article{Bentabol2016, -abstract = {We examine a sample of 1495 galaxies in the CANDELS fields to determine the evolution of two-component galaxies, including bulges and discs, within massive galaxies at the epoch 1 {\textless} z {\textless}3 when the Hubble sequence forms. We fit all of our galaxies' light profiles with a single S{\'{e}}rsic fit, as well as with a combination of exponential and S{\'{e}}rsic profiles. The latter is done in order to describe a galaxy with an inner and an outer component, or bulge and disc component. We develop and use three classification methods (visual, F-test and the residual flux fraction) to separate our sample into one-component galaxies (disc/spheroidslike galaxies) and two-component galaxies (galaxies formed by an 'inner part' or bulge and an 'outer part' or disc). We then compare the results from using these three different ways to classify our galaxies.We find that the fraction of galaxies selected as two-component galaxies increases on average 50 per cent from the lowest mass bin to the most massive galaxies, and decreases with redshift by a factor of 4 from z = 1 to 3. We find that single S{\'{e}}rsic 'disc-like' galaxies have the highest relative number densities at all redshifts, and that two-component galaxies have the greatest increase and become at par with S{\'{e}}rsic discs by z = 1. We also find that the systems we classify as two-component galaxies have an increase in the sizes of their outer components, or 'discs', by about a factor of 3 from z = 3 to 1.5, while the inner components or 'bulges' stay roughly the same size. This suggests that these systems are growing from the inside out, whilst the bulges or protobulges are in place early in the history of these galaxies. This is also seen to a lesser degree in the growth of single 'disc-like' galaxies versus 'spheroid-like' galaxies over the same epoch.}, -archivePrefix = {arXiv}, -arxivId = {1606.07405}, -author = {Margalef-Bentabol, Berta and Conselice, Christopher J and Mortlock, Alice and Hartley, Will and Duncan, Kenneth and Ferguson, Harry C and Dekel, Avishai and Primack, Joel R}, -doi = {10.1093/mnras/stw1451}, -eprint = {1606.07405}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure}, -number = {3}, -pages = {1--21}, -title = {{The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z {\textless} 3}}, -volume = {461}, -year = {2016} -} -@article{Hsu2018, -abstract = {We present a new framework to characterize the occurrence rates of planet candidates identified by Kepler based on hierarchical Bayesian modeling, Approximate Bayesian Computing (ABC), and sequential importance sampling. For this study we adopt a simple 2-D grid in planet radius and orbital period as our model and apply our algorithm to estimate occurrence rates for Q1-Q16 planet candidates orbiting around solar-type stars. We arrive at significantly increased planet occurrence rates for small planet candidates ({\$}R{\_}p{\textless}1.25 R{\_}{\{}\backslashoplus{\}}{\$}) at larger orbital periods ({\$}P{\textgreater}80{\$}d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is {\$}1.6{\^{}}{\{}+1.2{\}}{\_}{\{}-0.5{\}}{\$} per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2{\$}R{\_}{\{}\backslashoplus{\}}{\$} that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C and Ford, Eric B and Ragozzine, Darin and Morehead, Robert C}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -number = {5}, -pages = {205}, -title = {{ Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation }}, -url = {http://arxiv.org/abs/1803.10787%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -volume = {155}, -year = {2018} -} -@article{Tessore2016, -abstract = {Robust modelling of strong lensing systems is fundamental to exploit the information they contain about the distribution of matter in galaxies and clusters. In this work, we present lensed, a new code which performs forward parametric modelling of strong lenses. lensed takes advantage of a massively parallel ray-tracing kernel to perform the necessary calculations on a modern graphics processing unit (GPU). This makes the precise rendering of the background lensed sources much faster, and allows the simultaneous optimization of tens of parameters for the selected model. With a single run, the code is able to obtain the full posterior probability distribution for the lens light, the mass distribution and the background source at the same time. lensed is first tested on mock images which reproduce realistic space-based observations of lensing systems. In this way, we show that it is able to recover unbiased estimates of the lens parameters, even when the sources do not follow exactly the assumed model. Then, we apply it to a subsample of the Sloan Lens ACS Survey lenses, in order to demonstrate its use on real data. The results generally agree with the literature, and highlight the flexibility and robustness of the algorithm.}, -archivePrefix = {arXiv}, -arxivId = {1505.07674}, -author = {Tessore, Nicolas and Bellagamba, Fabio and Metcalf, R. Benton}, -doi = {10.1093/mnras/stw2212}, -eprint = {1505.07674}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tessore, Bellagamba, Metcalf - 2016 - LENSED A code for the forward reconstruction of lenses and sources from strong lensing observation.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Data analysis,Gravitational lensing: strong-methods,Methods: numerical,Methods: statistical,Techniques: image processing}, -number = {3}, -pages = {3115--3128}, -title = {{LENSED: A code for the forward reconstruction of lenses and sources from strong lensing observations}}, -volume = {463}, -year = {2016} -} -@article{VanDokkum2024, -abstract = {One of the surprising results from the Hubble Space Telescope was the discovery that many of the most massive galaxies at redshift z ≈ 2 are very compact, having a half-light radius of only 1−2 kpc. The interpretation is that massive galaxies formed inside out, with their cores largely in place by z ≈ 2 and approximately half of their present-day mass added later through minor mergers. Here we present a compact, massive, quiescent galaxy at a photometric redshift of zphot=1.94−0.17+0.13 with a complete Einstein ring. The ring was found in the James Webb Space Telescope COSMOS-Web survey and is produced by a background galaxy at zphot=2.98−0.47+0.42 . Its 1.54″ diameter provides a direct measurement of the mass of the ‘pristine' core of a massive galaxy, observed before the mixing and dilution of its stellar population during the 10 Gyr of galaxy evolution between z = 2 and z = 0. We find a mass for the lens Mlens=6.5−1.5+3.7×1011 M ⊙ within a radius of 6.6 kpc. The stellar mass within the same radius is Mstars=1.1−0.3+0.2×1011 M ⊙ for a Chabrier initial mass function and the fiducial dark matter mass is Mdm=2.6−0.7+1.6×1011 M ⊙. Additional mass appears to be needed to explain the lensing results, either in the form of a higher-than-expected dark matter density or a bottom-heavy initial mass function.}, -archivePrefix = {arXiv}, -arxivId = {2309.07969}, -author = {van Dokkum, Pieter and Brammer, Gabriel and Wang, Bingjie and Leja, Joel and Conroy, Charlie}, -doi = {10.1038/s41550-023-02103-9}, -eprint = {2309.07969}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/vandokkum2024full.pdf:pdf}, -isbn = {4155002302}, -issn = {23973366}, -journal = {Nature Astronomy}, -number = {1}, -pages = {119--125}, -publisher = {Springer US}, -title = {{A massive compact quiescent galaxy at z = 2 with a complete Einstein ring in JWST imaging}}, -volume = {8}, -year = {2024} -} -@article{VanDerWel2012, -abstract = {We present global structural parameter measurements of 109,533 unique, H{\_}F160W-selected objects from the CANDELS multi-cycle treasury program. Sersic model fits for these objects are produced with GALFIT in all available near-infrared filters (H{\_}F160W, J{\_}F125W and, for a subset, Y{\_}F105W). The parameters of the best-fitting Sersic models (total magnitude, half-light radius, Sersic index, axis ratio, and position angle) are made public, along with newly constructed point spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements -- to 10{\%} or better -- of all structural parameters can typically be obtained for galaxies with H{\_}F160W {\textless}23, with comparable fidelity for basic size and shape measurements for galaxies to H{\_}F160W {\$\sim${}} 24.5.}, -archivePrefix = {arXiv}, -arxivId = {1211.6954}, -author = {{Van Der Wel}, A and Bell, E F and H{\"{a}}ussler, B and McGrath, E J and Chang, Yu Yen and Guo, Yicheng and McIntosh, D H and Rix, H W and Barden, M and Cheung, E and Faber, S M and Ferguson, H C and Galametz, A and Grogin, N A and Hartley, W and Kartaltepe, J S and Kocevski, D D and Koekemoer, A M and Lotz, J and Mozena, M and Peth, M A and Peng, Chien Y}, -doi = {10.1088/0067-0049/203/2/24}, -eprint = {1211.6954}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: high-redshift,galaxies: statistics,galaxies: structure surveys}, -number = {2}, -title = {{Structural parameters of galaxies in candels}}, -volume = {203}, -year = {2012} -} -@article{Emsellem2007, -abstract = {Two-dimensional stellar kinematics of 48 representative elliptical (E) and lenticular (S0) galaxies obtained with the SAURON integral-field spectrograph reveal that early-type galaxies appear in two broad flavours, depending on whether they exhibit clear large-scale rotation or not. We define a new parameter, which involves luminosity-weighted averages over the full two-dimensional kinematic field as a proxy to quantify the observed projected stellar angular momentum per unit mass. We use it as a basis for a new kinematic classification: early-type galaxies are separated into slow and fast rotators, depending on whether they have $\lambda$R values within their effective radius Re below or above 0.1, respectively. Slow and fast rotators are shown to be physically distinct classes of galaxies, a result which cannot simply be the consequence of a biased viewing angle. Fast rotators tend to be relatively low-luminosity galaxies with MB ≳ -20.5. Slow rotators tend to be brighter and more massive galaxies, but are still spread over a wide range of absolute magnitude. Three slow rotators of our sample, among the most massive ones, are consistent with zero rotation. Remarkably, all other slow rotators (besides the atypical case of NGC 4550) contain a large kpc-scale kinematically decoupled core (KDC). All fast rotators (except one galaxy with well-known irregular shells) show well-aligned photometric and kinemetric axes, and small velocity twists, in contrast with most slow rotators which exhibit significant misalignments and velocity twists. These results are supported by a supplement of 18 additional early-type galaxies observed with SAURON. In a companion paper (Paper X), we also show that fast and slow rotators are distinct classes in terms of their orbital distribution. We suggest that gas is a key ingredient in the formation and evolution of fast rotators, and that the slowest rotators are the extreme evolutionary end point reached deep in gravitational potential wells where dissipationless mergers had a major role in the evolution, and for which most of the baryonic angular momentum was expelled outwards. Detailed numerical simulations in a cosmological context are required to understand how to form large-scale KDCs within slow rotators, and more generally to explain the distribution of $\lambda$R values within early-type galaxies and the distinction between fast and slow rotators. {\textcopyright} 2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0703531}, -author = {Emsellem, Eric and Cappellari, Michele and Krajnovi{\'{c}}, Davor and {Van De Ven}, Glenn and Bacon, R. and Bureau, M. and Davies, Roger L. and {De Zeeuw}, P. T. and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and Kuntschner, Harald and McDermid, Richard and Peletier, Reynier F. and Sarzi, Marc}, -doi = {10.1111/j.1365-2966.2007.11752.x}, -eprint = {0703531}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -month = {aug}, -number = {2}, -pages = {401--417}, -primaryClass = {astro-ph}, -title = {{The SAURON project - IX. A kinematic classification for early-type galaxies}}, -volume = {379}, -year = {2007} -} -@article{Mendez-Abreu2010a, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Treu2010, -abstract = {We determine an absolute calibration of the initial mass function (IMF) of early-type galaxies, by studying a sample of 56 gravitational lenses identified by the Sloan Lenses ACS Survey. Under the assumption of standard Navarro, Frenk, and White dark matter halos, a combination of lensing, dynamical, and stellar population synthesis models is used to disentangle the stellar and dark matter contribution for each lens. We define an “IMF mismatch” parameter $\alpha$ ≡M∗LDEin/M∗SPSEin as the ratio of stellar mass inferred by a joint lensing and dynamical model (M∗LDEin) to the current stellar mass inferred from stellar populations synthesis models (M∗SPSEin). We find that a Salpeter IMF provides stellar masses in agreement with those inferred by lensing and dynamical models (log $\alpha$ = −0.00 ± 0.03 ± 0.02), while a Chabrier IMF underestimates them (log $\alpha$ = 0.25 ± 0.03 ± 0.02). A tentative trend is found, in the sense that $\alpha$ appears to increase with galaxy velocity dispersion. Taken at face value, this result would imply a non-universal IMF, perhaps dependent on metallicity, age, or abundance ratios of the stellar populations. Alternatively, the observed trend may imply non-universal dark matter halos with inner density slope increasing with velocity dispersion. While the degeneracy between the two interpretations cannot be broken without additional information, the data imply that massive early-type galaxies cannot have both a universal IMF and universal dark matter halos.}, -archivePrefix = {arXiv}, -arxivId = {0911.3392v1}, -author = {Treu, Tommaso and Auger, Matthew W. and Koopmans, L{\'{e}}on V.E. and Gavazzi, Rapha{\"{e}}l and Marshall, Philip J. and Bolton, Adam S.}, -doi = {10.1088/0004-637X/709/2/1195}, -eprint = {0911.3392v1}, -isbn = {1097-0177 (Electronic)\r1058-8388 (Linking)}, -issn = {15384357}, -journal = {ApJ}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: structure,cD}, -number = {2}, -pages = {1195--1202}, -pmid = {24668528}, -title = {{The initial mass function of early-type galaxies}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1195?key=crossref.13584d69211f45adf93c3423b0b2ac61}, -volume = {709}, -year = {2010} -} -@article{Sanderson2009, -abstract = {We study the distribution of projected offsets between the cluster X-ray centroid and the brightest cluster galaxy (BCG) for 65 X-ray selected clusters from the Local Cluster Substructure Survey (LoCuSS), with a median redshift of z=0.23. We find a clear correlation between X-ray/BCG projected offset and the logarithmic slope of the cluster gas density profile at 0.04r500 (alpha), implying that more dynamically disturbed clusters have weaker cool cores. Furthermore, there is a close correspondence between the activity of the BCG, in terms of detected H{\_}alpha and radio emission, and the X-ray/BCG offset, with the line emitting galaxies all residing in clusters with X-ray/BCG offsets of {\textless}{\$\sim${}}15 kpc. Of the BCGs with alpha {\textless} -0.85 and an offset {\textless} 0.02r500, 96 per cent (23/24) have optical emission and 88 per cent (21/24) are radio active, while none has optical emission outside these criteria. We also study the cluster gas fraction (fgas) within r500 and find a significant correlation with X-ray/BCG projected offset. The mean fgas of the `small offset' clusters ({\textless} 0.02r500) is 0.106+/-0.005 (sigma=0.03) compared to 0.145+/-0.009 (sigma=0.04) for those with an offset {\textgreater} 0.02r500, indicating that the total mass may be systematically underestimated in clusters with larger X-ray/BCG offsets. Our results imply a link between cool core strength and cluster dynamical state consistent with the view that cluster mergers can significantly perturb cool cores, and set new constraints on models of the evolution of the intracluster medium.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:0906.1808v2}, -author = {Sanderson, Alastair J R and Edge, Alastair C and Smith, Graham P}, -doi = {10.1111/j.1365-2966.2009.15214.x}, -eprint = {arXiv:0906.1808v2}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: Clusters: general,Galaxies: Elliptical and lenticular,Galaxies: Evolution,X-rays: Galaxies: Clusters,cD}, -number = {4}, -pages = {1698--1705}, -title = {{LoCuSS: The connection between brightest cluster galaxy activity, gas cooling and dynamical disturbance of X-ray cluster cores}}, -volume = {398}, -year = {2009} -} -@inproceedings{Rhodes2006, -abstract = {The ability to accurately measure the shapes of faint objects in images taken with the Advanced Camera for Surveys(ACS) on the Hubble Space Telescope (HST) depends upon detailed knowledge of the Point Spread Function (PSF). We show that thermal fluctuations cause the PSF of the ACS Wide Field Camera (WFC) to vary over time. We describe a modified version of the TinyTim PSF modeling software to create artificial grids of stars across the ACS field of view at a range of telescope focus values. These models closely resemble the stars in real ACS images. Using $\sim$10 bright stars in a real image, we have been able to measure HST's apparent focus at the time of the exposure. TinyTim can then be used to model the PSF at any position on the ACS field of view. This obviates the need for images of dense stellar fields at different focus values, or interpolation between the few observed stars. We show that residual differences between our TinyTim models and real data are likely due to the effects of Charge Transfer Efficiency (CTE) degradation. Furthermore, we discuss stochastic noise that is added to the shape of point sources when distortion is removed, and we present Multidrizzle parameters that are optimal for weak lensing science. Specifically, we find that reducing the Multidrizzle output pixel scale and choosing a Gaussian kernel significantly stabilizes the resulting PSF after image combination, while still eliminating cosmic rays/bad pixels, and correcting the large geometric distortion in the ACS. We discuss future plans, which include more detailed study of the effects of CTE degradation on object shapes and releasing our TinyTim models to the astronomical community.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0512170}, -author = {Rhodes, Jason and Massey, Richard and Albert, Justin and Taylor, James E. and Koekemoer, Anton and Leauthaud, Alexie}, -booktitle = {The 2005 HST Calibration Workshop: Hubble After the Transition to Two-Gyro Mode}, -editor = {Koekemoer, A.$\sim$M. and Goudfrooij, P and Dressel, L.$\sim$L.}, -eprint = {0512170}, -month = {jan}, -pages = {21}, -primaryClass = {astro-ph}, -title = {{Modelling and Correcting the Time-Dependent ACS PSF}}, -url = {http://arxiv.org/abs/astro-ph/0512170}, -year = {2005} -} -@article{Version2018, -abstract = {We perform a systematic search for sub-parsec binary supermassive black holes (BHs) in normal broad-line quasars at z < 0.8, using multi-epoch Sloan Digital Sky Survey (SDSS) spectroscopy of the broad H$\beta$ line. Our working model is that (1) one and only one of the two BHs in the binary is active; (2) the active BH dynamically dominates its own broad-line region (BLR) in the binary system, so that the mean velocity of the BLR reflects the mean velocity of its host BH; (3) the inactive companion BH is orbiting at a distance of a few R BLR, where R BLR 0.01-0.1 pc is the BLR size. We search for the expected line-of-sight acceleration of the broad-line velocity from binary orbital motion by cross-correlating SDSS spectra from two epochs separated by up to several years in the quasar rest frame. Out of 00 pairs of spectra for which we have good measurements of the velocity shift between two epochs (1$\sigma$ error 0 km s-1), we detect 28 systems with significant velocity shifts in broad H$\beta$, among which 7 are the best candidates for the hypothesized binaries, 4 are most likely due to broad-line variability in single BHs, and the rest are ambiguous. Continued spectroscopic observations of these candidates will easily strengthen or disprove these claims. We use the distribution of the observed accelerations (mostly non-detections) to place constraints on the abundance of such binary systems among the general quasar population. Excess variance in the velocity shift is inferred for observations separated by longer than 0.4 yr (quasar rest frame). Attributing all the excess to binary motion would imply that most of the quasars in this sample must be in binaries, that the inactive BH must be on average more massive than the active one, and that the binary separation is at most a few times the size of the BLR. However, if this excess variance is partly or largely due to long-term broad-line variability, the requirement of a large population of close binaries is much weakened or even disfavored for massive companions. Future time-domain spectroscopic surveys of normal quasars can provide vital prior information on the structure function of stochastic velocity shifts induced by broad-line variability in single BHs. Such surveys with improved spectral quality, increased time baseline, and more epochs can greatly improve the statistical constraints of this method on the general binary population in broad-line quasars, further shrink the allowed binary parameter space, and detect true sub-parsec binaries. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1306.4330}, -author = {Shen, Yue and Liu, Xin and Loeb, Abraham and Tremaine, Scott}, -doi = {10.1088/0004-637X/775/1/49}, -eprint = {1306.4330}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shen et al. - 2013 - Constraining sub-parsec binary supermassive black holes in quasars with multi-epoch spectroscopy. I. the general qu.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {black hole physics,galaxies: active,line: profiles,quasars: general,surveys}, -number = {1}, -title = {{Constraining sub-parsec binary supermassive black holes in quasars with multi-epoch spectroscopy. I. the general quasar population}}, -volume = {775}, -year = {2013} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyse sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in 255 deg2 of the Kilo Degree Survey (KiDS), one of the currentgeneration optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii ≳1.4 arcsec, about twice the r-band seeing in KiDS. In a sample of 21 789 colour-magnitude selected luminous red galaxies (LRGs), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find {\$\sim${}}100 massive LRGgalaxy lenses at z ≲ 0.4 in KiDS when completed. In the most optimistic scenario, this number can grow considerably (to maximally {\$\sim${}}2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C E and Tortora, C and Chatterjee, S and Vernardos, G and Koopmans, L V E and Kleijn, G Verdoes and Napolitano, N R and Covone, G and Schneider, P and Grado, A and McFarland, J}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys,cD}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{Arcetri2018, -abstract = {We quantify the importance of mass accretion during active galactic nuclei (AGN) phases in the growth of supermassive black holes (BHs) by comparing the mass function of black holes in the Local Universe with that expected from AGN relics, which are black holes grown entirely with mass accretion during AGN phases. The local BH mass function (BHMF) is estimated by applying the well-known correlations between BH mass, bulge luminosity and stellar velocity dispersion to galaxy luminosity and velocity functions. We find that different correlations provide the same BHMF only if they have the same intrinsic dispersion. The density of supermassive black holes in the Local Universe that we estimate is $\rho$BH = 4.6-1.4+1.9h0.72 × 105 M⊙ Mpc-3. The relic BHMF is derived from the continuity equation with the only assumption that AGN activity is due to accretion on to massive BHs and that merging is not important. We find that the relic BHMF at z = 0 is generated mainly at z {\textless} 3 where the major part of the growth of a BH takes place. Moreover, BH growth is antihierarchical in the sense that smaller BHs (MBH {\textless} 10 7 M⊙) grow at lower redshifts (z {\textless} 1) with respect to more massive ones (z ∼ 1-3). Unlike previous work, we find that the BHMF of AGN relics is perfectly consistent with the local BHMF, indicating that local BHs were mainly grown during AGN activity. This agreement is obtained while satisfying, at the same time, the constraints imposed from the X-ray background (XRB). The comparison between the local and relic BHMFs also suggests that the merging process is not important in shaping the relic BHMF, at least at low redshifts (z {\textless} 3), and allows us to estimate the average radiative efficiency (e), the ratio between emitted and Eddington luminosity (A.) and the average lifetime of active BHs. Our analysis thus suggests the following scenario: local BHs grew during AGN phases in which accreting matter was converted into radiation with efficiencies $\epsilon$ = 0.04-0.16 and emitted at a fraction $\Lambda$ = 0.1-1.7 of the Eddington luminosity. The average total lifetime of these active phases ranges from ≃ 4.5 × 108 yr for MBH {\textless} 108 M⊙ to ≃ 1.5 × 108 yr for MBH {\textgreater} 109 M⊙, but can become as large as ∼109 yr for the lowest acceptable $\epsilon$ and $\lambda$values.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0311619}, -author = {Marconi, A and Risaliti, G and Gilli, R and Hunt, L K and Maiolino, R and Salvati, M}, -doi = {10.1111/j.1365-2966.2004.07765.x}, -eprint = {0311619}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cosmology: miscellaneous,Galaxies: active,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -pages = {169--185}, -primaryClass = {astro-ph}, -title = {{Local supermassive black holes, relics of active galactic nuclei and the X-ray background}}, -volume = {351}, -year = {2004} -} -@article{Lauer2005, -abstract = {We present observations of 77 early-type galaxies imaged with the{\$}\backslash{\$}nPC1 CCD of the Hubble Space Telescope (HST) WFPC2. ``Nuker-law''{\$}\backslash{\$}nparametric fits to the surface brightness profiles are used to classify{\$}\backslash{\$}nthe central structure into ``core'' or ``power-law'' forms. Core{\$}\backslash{\$}ngalaxies are typically rounder than power-law galaxies. Nearly all{\$}\backslash{\$}npower-law galaxies with central ellipticities ɛ{\textgreater}=0.3 have stellar{\$}\backslash{\$}ndisks, implying that disks are present in power-law galaxies with{\$}\backslash{\$}nɛ{\textless}0.3 but are not visible because of unfavorable geometry. A few{\$}\backslash{\$}nlow-luminosity flattened core galaxies also have disks; these may{\$}\backslash{\$}nbe transition forms from power-law galaxies to more luminous core{\$}\backslash{\$}ngalaxies, which lack disks. Several core galaxies have strong isophote{\$}\backslash{\$}ntwists interior to their break radii, although power-law galaxies{\$}\backslash{\$}nhave interior twists of similar physical significance when the photometric{\$}\backslash{\$}nperturbations implied by the twists are evaluated. Central color{\$}\backslash{\$}ngradients are typically consistent with the envelope gradients; core{\$}\backslash{\$}ngalaxies have somewhat weaker color gradients than power-law galaxies.{\$}\backslash{\$}nNuclei are found in 29{\%} of the core galaxies and 60{\%} of the power-law{\$}\backslash{\$}ngalaxies. Nuclei are typically bluer than the surrounding galaxy.{\$}\backslash{\$}nWhile some nuclei are associated with active galactic nuclei (AGNs),{\$}\backslash{\$}njust as many are not; conversely, not all galaxies known to have{\$}\backslash{\$}na low-level AGN exhibit detectable nuclei in the broadband filters.{\$}\backslash{\$}nNGC 4073 and 4382 are found to have central minima in their intrinsic{\$}\backslash{\$}nstarlight distributions; NGC 4382 resembles the double nucleus of{\$}\backslash{\$}nM31. In general, the peak brightness location is coincident with{\$}\backslash{\$}nthe photocenter of the core to a typical physical scale of {\textless}1 pc.{\$}\backslash{\$}nFive galaxies, however, have centers significantly displaced from{\$}\backslash{\$}ntheir surrounding cores; these may be unresolved asymmetric double{\$}\backslash{\$}nnuclei. Finally, as noted by previous authors, central dust is visible{\$}\backslash{\$}nin about half of the galaxies. The presence and strength of dust{\$}\backslash{\$}ncorrelates with nuclear emission; thus, dust may outline gas that{\$}\backslash{\$}nis falling into the central black hole. The prevalence of dust and{\$}\backslash{\$}nits morphology suggest that dust clouds form, settle to the center,{\$}\backslash{\$}nand disappear repeatedly on {\$\sim${}}108 yr timescales. We discuss the hypothesis{\$}\backslash{\$}nthat cores are created by the decay of a massive black hole binary{\$}\backslash{\$}nformed in a merger. Apart from their brightness profiles, there are{\$}\backslash{\$}nno strong differences between core galaxies and power-law galaxies{\$}\backslash{\$}nthat demand this scenario; however, the rounder shapes of core, their{\$}\backslash{\$}nlack of disks, and their reduced color gradients may be consistent{\$}\backslash{\$}nwith it. Based on observations made with the NASA/ESA Hubble Space{\$}\backslash{\$}nTelescope, obtained at the Space Telescope Science Institute, which{\$}\backslash{\$}nis operated by the Association of Universities for Research in Astronomy{\$}\backslash{\$}n(AURA), Inc., under NASA contract NAS 5-26555. These observations{\$}\backslash{\$}nare associated with GO and GTO proposals 5236, 5446, 5454, 5512,{\$}\backslash{\$}n5943, 5990, 5999, 6099, 6386, 6554, 6587, 6633, 7468, 8683, and 9107.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0412040}, -author = {Lauer, Tod R and Faber, S M and Gebhardt, Karl and Richstone, Douglas and Tremaine, Scott and Ajhar, Edward A and Aller, M C and Bender, Ralf and Dressler, Alan and Filippenko, Alexei V and Green, Richard and Grillmair, Carl J and Ho, Luis C and Kormendy, John and Magorrian, John and Pinkney, Jason and Siopis, Christos}, -doi = {10.1086/429565}, -eprint = {0412040}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2138--2185}, -primaryClass = {arXiv:astro-ph}, -title = {{The Centers of Early-Type Galaxies with {\textless}i{\textgreater}Hubble Space Telescope{\textless}/i{\textgreater}. V. New WFPC2 Photometry}}, -url = {http://stacks.iop.org/1538-3881/129/i=5/a=2138}, -volume = {129}, -year = {2005} -} -@article{Birrer2015, -abstract = {We present a strong lensing modeling technique based on versatile basis sets for the lens and source planes. Our method uses high performance Monte Carlo algorithms, allows for an adaptive build up of complexity, and bridges the gap between parametric and pixel based reconstruction methods. We apply our method to a Hubble Space Telescope image of the strong lens system RX J1131-1231 and show that our method finds a reliable solution and is able to detect substructure in the lens and source planes simultaneously. Using mock data, we show that our method is sensitive to sub-clumps with masses four orders of magnitude smaller than the main lens, which corresponds to about 108M⊙ , without prior knowledge of the position and mass of the sub-clump. The modeling approach is flexible and maximizes automation to facilitate the analysis of the large number of strong lensing systems expected in upcoming wide field surveys. The resulting search for dark sub-clumps in these systems, without mass-to-light priors, offers promise for probing physics beyond the standard model in the dark matter sector.}, -archivePrefix = {arXiv}, -arxivId = {1504.07629}, -author = {Birrer, Simon and Amara, Adam and Refregier, Alexandre}, -doi = {10.1088/0004-637X/813/2/102}, -eprint = {1504.07629}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmological parameters,distance scale,gravitational lensing: strong,methods: numerical}, -month = {nov}, -number = {2}, -pages = {102}, -title = {{GRAVITATIONAL LENS MODELING with BASIS SETS}}, -url = {http://stacks.iop.org/0004-637X/813/i=2/a=102?key=crossref.b6824f4280340fdc0fa018ab63d85879}, -volume = {813}, -year = {2015} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a $\Lambda$CDM concordance cosmology. To that extent we use a large N-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as a function of halo mass and galaxy colour. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by ∼40° (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the colour of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the colour of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion. {\textcopyright} 2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X. and {Van Den Bosch}, Frank C. and Yang, Xiaohu and Mao, Shude and Mo, H. J. and Li, Cheng and Jing, Y. P.}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kang et al. - 2007 - The alignment between satellites and central galaxies Theory versus observations.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@article{Merritt2006, -abstract = {A binary supermassive black hole leaves an imprint on a galactic nucleus in the form of a "mass deficit," a decrease in the mass of the nucleus due to ejection of stars by the binary. The magnitude of the mass deficit is in principle related to the galaxy's merger history, but the relation has never been quantified. Here high-accuracy N-body simulations are used to calibrate this relation. Mass deficits are shown to be Mdef ? 0.5M 12, with M12 the total mass of the binary; the coefficient in this relation is found to depend only weakly on M2/M1 or on the galaxy's preexisting nuclear density profile. Hence, after N mergers, Mdef ? 0.5NM?, with M? the final (current) black hole mass. When compared with observed mass deficits, this result implies 1 ? N ? 3, in accord with hierarchical structure formation models. Implications for binary stalling radii, the origin of hypervelocity stars, and the distribution of dark matter at the centers of galaxies are discussed. ? 2006. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0603439}, -author = {Merritt, David}, -doi = {10.1086/506139}, -eprint = {0603439}, -isbn = {0419-4217}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {astro-ph}, -month = {sep}, -number = {2}, -pages = {976--986}, -primaryClass = {arXiv:astro-ph}, -title = {{Mass Deficits, Stalling Radii, and the Merger Histories of Elliptical Galaxies}}, -url = {http://stacks.iop.org/0004-637X/648/i=2/a=976}, -volume = {648}, -year = {2006} -} -@article{YuSa2013, -abstract = {Charged Coupled Devices (CCDs) have been successfully used in several low energy X-ray astronomical satellites over the past two decades. Their high energy resolution and high spatial resolution make them a perfect tool for low energy astronomy, such as observing the formation of galaxy clusters and the environment around black holes. The Low Energy X-ray Telescope (LE) group is developing a Swept Charge Device (SCD) for the Hard X-ray Modulation Telescope (HXMT) satellite. A SCD is a special low energy X-ray CCD, which can be read out a thousand times faster than traditional CCDs, simultaneously keeping excellent energy resolution. A test method for measuring the charge transfer efficiency (CTE) of a prototype SCD has been set up. Studies of the charge transfer inefficiency (CTI) with a proton-irradiated SCD have been performed at a range of operating temperatures. The SCD is irradiated by 3 × 10 8cm-2 10 MeV protons. {\textcopyright}2014 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1308.1698}, -author = {Wang, Yu Sa and Yang, Yan Ji and Chen, Yong and Liu, Xiao Yan and Cui, Wei Wei and Xu, Yu Peng and Li, Cheng Kui and Li, Mao Shun and Han, Da Wei and Chen, Tian Xiang and Huo, Jia and Wang, Juan and Li, Wei and Hu, Wei and Zhang, Yi and Lu, Bo and Yin, Guo He and Zhu, Yue and Zhang, Zi Liang}, -doi = {10.1088/1674-1137/38/6/066001}, -eprint = {1308.1698}, -issn = {16741137}, -journal = {Chinese Physics C}, -keywords = {CCD,CTE,CTI,HXMT,LE,SCD,proton-irradiated}, -number = {6}, -pages = {1--5}, -title = {{Measurements of charge transfer efficiency in a proton-irradiated swept charge device}}, -url = {http://arxiv.org/abs/1308.1698}, -volume = {38}, -year = {2014} -} -@article{Leauthaud2017, -abstract = {We present high signal-to-noise galaxy-galaxy lensing measurements of the Baryon Oscillation Spectroscopic Survey constant mass (CMASS) sample using 250 deg2 of weak-lensing data from Canada-France-Hawaii Telescope Lensing Survey and Canada-France-Hawaii Telescope Stripe 82 Survey. We compare this signal with predictions from mock catalogues trained to match observables including the stellar mass function and the projected and twodimensional clustering of CMASS. We show that the clustering of CMASS, together with standard models of the galaxy-halo connection, robustly predicts a lensing signal that is 20-40 per cent larger than observed. Detailed tests show that our results are robust to a variety of systematic effects. Lowering the value of S8 = $\sigma$8 √ $\Omega$m/0.3 compared to Planck Collaboration XIII reconciles the lensing with clustering. However, given the scale of our measurement (r {\textless} 10 h-1 Mpc), other effects may also be at play and need to be taken into consideration. We explore the impact of baryon physics, assembly bias, massive neutrinos and modifications to general relativity on $\Delta$$\Sigma$ and show that several of these effects may be non-negligible given the precision of our measurement. Disentangling cosmological effects from the details of the galaxy-halo connection, the effect of baryons, and massive neutrinos, is the next challenge facing joint lensing and clustering analyses. This is especially true in the context of large galaxy samples from Baryon Acoustic Oscillation surveys with precise measurements but complex selection functions.}, -archivePrefix = {arXiv}, -arxivId = {1611.08606}, -author = {Leauthaud, Alexie and Saito, Shun and Hilbert, Stefan and Barreira, Alexandre and More, Surhud and White, Martin and Alam, Shadab and Behroozi, Peter and Bundy, Kevin and Coupon, Jean and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Mandelbaum, Rachel and Miller, Lance and Moraes, Bruno and Pereira, Maria E S and Rodr{\'{i}}guez-Torres, Sergio A and Schmidt, Fabian and Shan, Huan Yuan and Viel, Matteo and Villaescusa-Navarro, Francisco}, -doi = {10.1093/mnras/stx258}, -eprint = {1611.08606}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {3}, -pages = {3024--3047}, -title = {{Lensing is low: Cosmology, galaxy formation or new physics?}}, -volume = {467}, -year = {2017} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyze sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in {\$}255{\$} square degrees of the Kilo Degree Survey (KiDS), one of the current-generation optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii {\$}\backslashgtrsim 1.4{\$} arcsec, about twice the {\$}r{\$}-band seeing in KiDS. In a sample of {\$}21789{\$} colour-magnitude selected Luminous Red Galaxies (LRG), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find {\$}\backslashsim100{\$} massive LRG-galaxy lenses at {\$}z\backslashlsim 0.4{\$} in KiDS when completed. In the most optimistic scenario this number can grow considerably (to maximally {\$}\backslashsim{\$}2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C E and Tortora, C and Chatterjee, S and Vernardos, G and Koopmans, L V E and Kleijn, G Verdoes and Napolitano, N R and Covone, G and Schneider, P and Grado, A and McFarland, J}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys,cD}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{2001ev, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@inproceedings{MartinNavarro2013, -author = {Mart\$\backslash\$'\$\backslash\$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Sonnenfeld2023, -abstract = {Contact. Strong lenses are a biased subset of the general population of galaxies. Aims. The goal of this work is to quantify how lens galaxies and lensed sources differ from their parent distribution, namely the strong lensing bias. Methods. We first studied how the strong lensing cross-section varies as a function of lens and source properties. Then, we simulated strong lensing surveys with data similar to that expected for Euclid and measured the strong lensing bias in different scenarios. We focused particularly on two quantities: the stellar population synthesis mismatch parameter, $\alpha$sps, defined as the ratio between the true stellar mass of a galaxy and the stellar mass obtained from photometry, and the central dark matter mass at fixed stellar mass and size. Results. Strong lens galaxies are biased towards higher stellar masses, smaller half-mass radii, and higher dark matter masses. The amplitude of the bias depends on the intrinsic scatter in the mass-related parameters of the galaxy population and on the completeness in Einstein radius of the lens sample. For values of the scatter that are consistent with observed scaling relations and a minimum detectable Einstein radius of 0.5;, the strong lensing bias in $\alpha$sps is 10%, while that in the central dark matter mass is 5%. The bias has little dependence on the properties of the source population: samples of galaxy-galaxy lenses and galaxy-quasar lenses that probe the same Einstein radius distribution are biased in a very similar way. Conclusions. Given current uncertainties, strong lensing observations can be used directly to improve our current knowledge of the inner structure of galaxies, without the need to correct for selection effects. Time-delay measurements of H0 from lensed quasars can take advantage of prior information obtained from galaxy-galaxy lenses with similar Einstein radii.}, -author = {Sonnenfeld, Alessandro and Li, Shun Sheng and Despali, Giulia and Gavazzi, Raphael and Shajib, Anowar J. and Taylor, Edward N.}, -doi = {10.1051/0004-6361/202346026}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnenfeld2023SelectionEffects.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Gravitational lensing: strong}, -pages = {1--26}, -title = {{Strong lensing selection effects}}, -volume = {678}, -year = {2023} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of stellar parameters and abundances ("stellar labels") for hundreds of thousands of stars; this poses a formidable spectral modeling challenge. In many cases, there is a subset of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the "known" labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with and as the labels, and then applying it to the spectra of 55,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one-ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ness, M and Hogg, David W and Rix, H W and Ho, Anna Y Q and Zasowski, G}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{THE CANNON: A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION}}, -volume = {808}, -year = {2015} -} -@article{Gadotti2011, -abstract = {I present results from the modelling of stellar bars in nearly 300 barred galaxies in the local universe through parametric multicomponent multiband image fitting. The surface brightness radial profile of bars is described using a S{\'{e}}rsic function and parameters, such as the bar effective radius, ellipticity, boxiness, length and mass, and bar-to-total luminosity and mass ratios, are determined, which is unprecedented for a sample of this size. The properties of bars in galaxies with classical bulges and pseudo-bulges are compared. For a fixed bar-to-total mass ratio, pseudo-bulges are on average significantly less massive than classical bulges, indicating that, if pseudo-bulges are formed through bars, further processes are necessary to build a classical bulge. I find a correlation between bar ellipticity and boxiness, and define a new parameter as the product of these two quantities. I also find correlations between this product and the normalized bar size, between the sizes of bars and bulges, and between the normalized bar size and bulge-to-total ratio. Bars with different ellipticities follow parallel lines in the latter two correlations. These correlations can arise if, starting off with different normalized sizes and ellipticities, bars grow longer and stronger with dynamical age, as a result of angular momentum exchange between the inner and outer parts of galaxies, consistent with previous theoretical predictions. A plausible consequence is that bar pattern speeds should become lower with bar dynamical age and towards galaxies with more prominent bulges. {\textcopyright} 2011 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1003.1719}, -author = {Gadotti, Dimitri A.}, -doi = {10.1111/j.1365-2966.2011.18945.x}, -eprint = {1003.1719}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gadotti - 2011 - Secular evolution and structural properties of stellar bars in galaxies(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {3308--3318}, -title = {{Secular evolution and structural properties of stellar bars in galaxies}}, -volume = {415}, -year = {2011} -} -@article{Agustsson2007a, -abstract = {We investigate the locations of the satellites of relatively isolated host galaxies in the Sloan Digital Sky Survey and the Millennium Run simulation. Provided we use two distinct prescriptions to embed luminous galaxies within the simulated dark matter halos (ellipticals share the shapes of their halos, while disks have angular momenta that are aligned with the net angular momenta of their halos), we find a fair agreement between observation and theory. Averaged over scales r{\_}p {\$}\backslash{\$}le 500 kpc, the satellites of red, high-mass hosts with low star formation rates are found preferentially near the major axes of their hosts. In contrast, the satellites of blue, low-mass hosts with low star formation rates show little to no anisotropy when averaged over the same scale. The difference between the locations of the satellites of red and blue hosts cannot be explained by the effects of interlopers in the data. Instead, it is caused primarily by marked differences in the dependence of the mean satellite location, {\textless}{\$}\backslash{\$}phi{\textgreater}, on the projected distance at which the satellites are found. We also find that the locations of red, high-mass satellites with low star formation rates show considerably more anisotropy than do the locations of blue, low--mass satellites with high star formation rates. There are two contributors to this result. First, the blue satellites have only recently arrived within their hosts' halos, while the red satellites arrived in the far distant past. Second, the sample of blue satellites is heavily contaminated by interlopers, which suppresses the measured anisotropy compared to the intrinsic anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {0704.3441}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1088/0004-637X/709/2/1321}, -eprint = {0704.3441}, -issn = {0004-637X}, -journal = {arXiv}, -pages = {3441}, -title = {{Anisotropic Locations of Satellite Galaxies: Clues to the Orientations of Galaxies within their Dark Matter Halos}}, -url = {http://arxiv.org/abs/0704.3441%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/0004-637X/709/2/1321}, -volume = {0704}, -year = {2007} -} -@article{Handley2015, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W. J. and Hobson, M. P. and Lasenby, A. N.}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Handley, Hobson, Lasenby - 2015 - POLYCHORD Next-generation nested sampling(3).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Yan2016, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R{\$\sim${}}2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is {\$\sim${}}73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R and Bershady, Matthew A and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R and Thomas, Daniel and Wake, David A and Weijmans, Anne-Marie and Westfall, Kyle B and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A and Blanton, Michael R and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T and Goddard, Daniel and Gunn, James E and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R and Oravetz, Daniel and Pan, Kaike and Parejko, John K and Sanchez, Sebastian F and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -title = {{SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality}}, -url = {http://arxiv.org/abs/1607.08613%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {197}, -year = {2016} -} -@article{Hopkins2009, -abstract = {Transformation of discs into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that the bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in haloes according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the overproduction of spheroids: low- and intermediate-mass galaxies are predicted to be bulge-dominated (B/T ∼ 0.5 at {\textless}10 10 M ⊙, with almost no 'bulgeless' systems), even if they have avoided major mergers. Including the different physical behaviour of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T ∼ 0.1 at {\textless}10 10 M ⊙, with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behaviour of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4111}, -author = {Hopkins, Philip F and Somerville, Rachel S and Cox, Thomas J and Hernquist, Lars and Jogee, Shardha and Kere{\v{s}}, Dusan and Ma, Chung Pei and Robertson, Brant and Stewart, Kyle}, -doi = {10.1111/j.1365-2966.2009.14983.x}, -eprint = {0901.4111}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Galaxies: spiral}, -number = {2}, -pages = {802--814}, -title = {{The effects of gas on morphological transformation in mergers: Implications for bulge and disc demographics}}, -volume = {397}, -year = {2009} -} -@article{Cabanac2007, -abstract = {AIMS: We present data from the CFHTLS Strong Lensing Legacy Survey (SL2S). Due to the unsurpassed combined depth, area and image quality of the Canada-France-Hawaii Legacy Survey it is becoming possible to uncover a large, statistically well-defined sample of strong gravitational lenses which spans the dark halo mass spectrum predicted by the concordance model from galaxy to cluster haloes. METHODS: We describe the development of several automated procedures to find strong lenses of various mass regimes in CFHTLS images. RESULTS: The preliminary sample of about 40 strong lensing candidates discovered in the CFHTLS T0002 release, covering an effective field of view of 28 deg$^2$ is presented. These strong lensing systems were discovered using an automated search and consist mainly of gravitational arc systems with splitting angles between 2 and 15 arcsec. This sample shows for the first time that it is possible to uncover a large population of strong lenses from galaxy groups with typical halo masses of about $10^{13}h^{-1}M_\odot$. We discuss the future evolution of the SL2S project and its main scientific aims for the next 3 years, in particular our observational strategy to extract the hundreds of gravitational rings also present in these fields.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0610362}, -author = {Cabanac, R. A. and Alard, Christophe and Dantel-Fort, M. and Fort, B. and Gavazzi, R. and Gomez, P. and Kneib, J. P. and {Le F{\`{e}}vre}, O. and Mellier, Y. and Pello, R. and Soucail, G. and Sygnet, J. F. and Valls-Gabaud, D.}, -doi = {10.1051/0004-6361:20065810}, -eprint = {0610362}, -issn = {0004-6361}, -journal = {Astronomy and Astrophysics}, -keywords = {Astrophysics}, -number = {3}, -pages = {813--821}, -primaryClass = {astro-ph}, -title = {{The CFHTLS strong lensing legacy survey}}, -url = {http://www.aanda.org/10.1051/0004-6361:20065810}, -volume = {461}, -year = {2007} -} -@article{Ma2012, -abstract = {We present an analysis of the structures and dynamics of the merging cluster Abell1201, which has two sloshing cold fronts around a cooling core, and an offset gas core approximately 500kpc northwest of the center. New Chandra and XMM-Newton data reveal a region of enhanced brightness east of the offset core, with breaks in surface brightness along its boundary to the north and east. This is interpreted as a tail of gas stripped from the offset core. Gas in the offset core and the tail is distinguished from other gas at the same distance from the cluster center chiefly by having higher density, hence lower entropy. In addition, the offset core shows marginally lower temperature and metallicity than the surrounding area. The metallicity in the cool core is high and there is an abrupt drop in metallicity across the southern cold front. We interpret the observed properties of the system, including the placement of the cold fronts, the offset core, and its tail in terms of a simple merger scenario. The offset core is the remnant of a merging subcluster, which first passed pericenter southeast of the center of the primary cluster and is now close to its second pericenter passage, moving at ≃ 1000 km s-1. Sloshing excited by the merger gave rise to the two cold fronts and the disposition of the cold fronts reveals that we view the merger from close to the plane of the orbit of the offset core. {\textcopyright} 2012. The American Astronomical Society. All rights reserved..}, -author = {Ma, Cheng Jiun and Owers, Matt and Nulsen, Paul E.J. and McNamara, Brian R. and Murray, Stephen S. and Couch, Warrick J.}, -doi = {10.1088/0004-637X/752/2/139}, -file = {:C\:/Users/Jammy/Documents/Papers/Abell1201XRay.pdf:pdf}, -isbn = {0500760101}, -issn = {15384357}, -journal = {ApJ}, -keywords = {galaxies: clusters: general,galaxies: clusters: individual (A1201)}, -number = {2}, -pages = {139}, -title = {{Abell 1201: A minor merger at second core passage}}, -volume = {752}, -year = {2012} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in {\$\sim${}}10 dynamical times, or {\$\sim${}}0.5Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, {\$\sim${}}100 Msun/yr, and each clump converts into stars in {\$\sim${}}0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z{\$\sim${}}3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z{\$\sim${}}1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Li2008, -abstract = {We analyze properties of subhalos/substructures resolved in a dark matter simulation of a Milky Way-like halo in a $\Lambda$CDM cosmology. We explore possible links between subhalos and the Galactic satellites and find: 1) The infall patterns of subhalos are slightly elongated along the major axis of the galaxy halo and are clumpy on smaller scales. 2) The Great disk defined by MW satellites (Kroupa et al. 2005) is easily reproduced in our simulations without recurring to sophisticated galaxy formation recipes and is purely due to their highly centrally concentrated distribution around the Galaxy.}, -archivePrefix = {arXiv}, -arxivId = {0807.2780}, -author = {Li, Yang Shyang and Helmi, Amina}, -doi = {10.1007/978-1-4020-5573-7_53}, -eprint = {0807.2780}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Li, Helmi - 2007 - Infall of substructures onto a milky way-like dark halo.pdf:pdf}, -isbn = {0000000000000}, -issn = {15706605}, -journal = {Astrophysics and Space Science Proceedings}, -keywords = {Dark matter,Galaxies: Dwarf,Galaxies: Kinematics and dynamics,Galaxy: Formation,Methods: Numerical}, -number = {202409}, -pages = {311--314}, -title = {{Infall of substructures onto a milky way-like dark halo}}, -volume = {385}, -year = {2007} -} -@article{Xie2015, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{DiCintio2014, -abstract = {We use 31 simulated galaxies from the MaGICC project to investigate the effects of baryonic feedback on the density profiles of dark matter (DM) haloes. The sample covers a wide mass range: 9.4e999.9 per cent confidence), but that it can be described as the sum of two Gaussians, one of which is broad ($\sigma$ = 176 ± 15 km s-1), has a mean prograde velocity of 86 ± 30 km s-1, and contains ∼55 per cent of the satellites, while the other is slightly retrograde with a mean velocity of -21 ± 22 km s-1 and $\sigma$ = 74 ± 18 km s-1 and contains ∼45 per cent of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy, and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E.}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Herbert-Fort et al. - 2008 - The orbital distribution of satellite galaxies.pdf:pdf}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Greene2013, -abstract = {We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions $\sigma$* ≳ 150 km s-1. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼ 10 Gyr), relatively metal-poor ([Fe/H] ≈ -0.5), and $\alpha$-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z ≈ 1.5-2). {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1308.2682}, -author = {Greene, Jenny E and Murphy, Jeremy D and Graves, Genevieve J and Gunn, James E and Raskutti, Sudhir and Comerford, Julia M and Gebhardt, Karl}, -doi = {10.1088/0004-637X/776/2/64}, -eprint = {1308.2682}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: abundances,galaxies: elliptical and lenticular,galaxies: evolution}, -number = {2}, -title = {{The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius}}, -volume = {776}, -year = {2013} -} -@article{Diemand2004, -abstract = {We present a statistical study of substructure within a sample of $\lambda$cold dark matter ($\lambda$CDM) clusters and galaxies simulated with up to 25 × 106 particles. With thousands of subhaloes per object we can accurately measure their spatial clustering and velocity distribution functions and compare these with observational data. The substructure properties of galactic haloes closely resemble those of galaxy clusters with a small scatter in the mass and circular velocity functions. The velocity distribution function is non-Maxwellian and flat topped with a negative kurtosis of approximately -0.7. Within the virial radius the velocity bias b = $\sigma$sub/$\sigma$DM ∼ 1.12 ±0.04, increasing to b > 1.3 within the halo centres. Slow subhaloes are much less common, due to physical disruption by gravitational tides early in the merging history. This leads to a spatially antibiased subhalo distribution that is well fitted by a cored isothermal. Observations of cluster galaxies do not show such biases, which we interpret as a limitation of pure dark matter simulations - we estimate that we are missing half of the halo population, which has been destroyed by physical overmerging. High-resolution hydrodynamical simulations are required to study these issues further. If CDM is correct then the cluster galaxies must survive the tidal field, perhaps due to baryonic inflow during elliptical galaxy formation. Spirals can never exist near the cluster centres and the elliptical galaxies there will have little remaining dark matter. This implies that the morphology-density relation is set before the cluster forms, rather than a subsequent transformation of discs to S0s by virtue of the cluster environment.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402160}, -author = {Diemand, J{\"{u}}rg and Moore, Ben and Stadel, Joachim}, -doi = {10.1111/j.1365-2966.2004.07940.x}, -eprint = {0402160}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies,Galaxies: haloes,Methods: N-body simulations,Methods: numerical,clusters: general}, -number = {2}, -pages = {535--546}, -primaryClass = {astro-ph}, -title = {{Velocity and spatial biases in cold dark matter subhalo distributions}}, -volume = {352}, -year = {2004} -} -@article{Geometryek, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(10).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified $\sim$17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M <10^9 M*), low-metallicity (Z$\sim$1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He \ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A. and Erb, Dawn K. and Auger, Matthew W. and Pettini, Max and Brammer, Gabriel B.}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Berg et al. - 2018 - A Window on the Earliest Star Formation Extreme Photoionization Conditions of a High-ionization, Low-metallicity(2).pdf:pdf}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {164}, -title = {{ A Window on the Earliest Star Formation: Extreme Photoionization Conditions of a High-ionization, Low-metallicity Lensed Galaxy at z ∼ 2* }}, -url = {http://arxiv.org/abs/1803.02340}, -volume = {859}, -year = {2018} -} -@article{Emcee, -abstract = {We introduce a stable, well tested Python implementation of the affine-invariant ensemble sampler for Markov chain Monte Carlo (MCMC) proposed by Goodman {\&} Weare (2010). The code is open source and has already been used in several published projects in the astrophysics literature. The algorithm behind emcee has several advantages over traditional MCMC sampling methods and it has excellent performance as measured by the autocorrelation time (or function calls per independent sample). One major advantage of the algorithm is that it requires hand-tuning of only 1 or 2 parameters compared to {\$}\backslashsim N{\^{}}2{\$} for a traditional algorithm in an N-dimensional parameter space. In this document, we describe the algorithm and the details of our implementation and API. Exploiting the parallelism of the ensemble method, emcee permits any user to take advantage of multiple CPU cores without extra effort. The code is available online at http://dan.iel.fm/emcee under the MIT License.}, -archivePrefix = {arXiv}, -arxivId = {1202.3665}, -author = {Foreman-Mackey, Daniel and Hogg, David W and Lang, Dustin and Goodman, Jonathan}, -doi = {10.1086/670067}, -eprint = {1202.3665}, -issn = {00046280}, -journal = {Publications of the Astronomical Society of the Pacific}, -number = {925}, -pages = {306--312}, -title = {{emcee : The MCMC Hammer }}, -volume = {125}, -year = {2013} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and disks are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disk components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to CALIFA integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component, and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {elliptical and lenticular,galaxies,kinematics and dynamics}, -number = {2}, -pages = {2024--2033}, -title = {{Untangling galaxy components: full spectral bulge–disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {466}, -year = {2017} -} -@article{Eisenstein2001, -abstract = {We describe the target selection and resulting properties of a spectroscopic sample of luminous, red galaxies (LRG) from the imaging data of the Sloan Digital Sky Survey (SDSS). These galaxies are selected on the basis of color and magnitude to yield a sample of luminous, intrinsically red galaxies that extends fainter and further than the main flux-limited portion of the SDSS galaxy spectroscopic sample. The sample is designed to impose a passively-evolving luminosity and rest-frame color cut to a redshift of 0.38. Additional, yet more luminous, red galaxies are included to a redshift of 0.5. Approximately 12 of these galaxies per square degree are targeted for spectroscopy, so the sample will number over 100,000 with the full survey. SDSS commissioning data indicate that the algorithm efficiently selects luminous (M{\_}g=-21.4), red galaxies, that the spectroscopic success rate is very high, and that the resulting set of galaxies is approximately volume-limited out to z=0.38. When the SDSS is complete, the LRG spectroscopic sample will fill over 1h{\^{}}-3 Gpc{\^{}}3 with an approximately homogeneous population of galaxies and will therefore be well suited to studies of large-scale structure and clusters out to z=0.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108153}, -author = {Eisenstein, Daniel J and Annis, James and Gunn, James E and Szalay, Alexander S and Connolly, Andrew J and Nichol, R C and Bahcall, Neta A and Bernardi, Mariangela and Burles, Scott and Castander, Francisco J and Fukugita, Masataka and Hogg, David W and Ivezi{\'{c}}, {\v{Z}}eljko and Knapp, G R and Lupton, Robert H and Narayanan, Vijay and Postman, Marc and Reichart, Daniel E and Richmond, Michael and Schneider, Donald P and Schlegel, David J and Strauss, Michael A and SubbaRao, Mark and Tucker, Douglas L and {Vanden Berk}, Daniel and Vogeley, Michael S and Weinberg, David H and Yanny, Brian}, -doi = {10.1086/323717}, -eprint = {0108153}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2267--2280}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample}}, -url = {http://arxiv.org/abs/astro-ph/0108153%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/323717}, -volume = {122}, -year = {2001} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since z = 1.0. We find that lower mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher mass or lower redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single-aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys; we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1824--1848}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {469}, -year = {2017} -} -@article{Li2008, -abstract = {We analyze properties of subhalos/substructures resolved in a dark matter simulation of a Milky Way-like halo in a $\Lambda$CDM cosmology. We explore possible links between subhalos and the Galactic satellites and find: 1) The infall patterns of subhalos are slightly elongated along the major axis of the galaxy halo and are clumpy on smaller scales. 2) The Great disk defined by MW satellites (Kroupa et al. 2005) is easily reproduced in our simulations without recurring to sophisticated galaxy formation recipes and is purely due to their highly centrally concentrated distribution around the Galaxy.}, -archivePrefix = {arXiv}, -arxivId = {0807.2780}, -author = {Li, Yang Shyang and Helmi, Amina}, -doi = {10.1007/978-1-4020-5573-7_53}, -eprint = {0807.2780}, -isbn = {0000000000000}, -issn = {15706605}, -journal = {Astrophysics and Space Science Proceedings}, -keywords = {Dark matter,Galaxies: Dwarf,Galaxies: Kinematics and dynamics,Galaxy: Formation,Methods: Numerical}, -number = {202409}, -pages = {311--314}, -title = {{Infall of substructures onto a milky way-like dark halo}}, -volume = {385}, -year = {2007} -} -@article{Cohen2018, -abstract = {We present HST/ACS imaging of twenty-three very low surface brightness ({\$}\backslashmu{\_}{\{}e,V{\}}{\$}=25-27.5) galaxies detected in the fields of four nearby galaxy groups. These objects were selected from deep optical imaging obtained with the Dragonfly Telephoto Array. Seven are new discoveries, while most of the others had been identified previously in visual surveys of deep photographic plates and more recent surveys. Few have previously been studied in detail. From the ACS images, we measure distances to the galaxies using both the tip of the red giant branch method and the surface brightness fluctuations method. We demonstrate that the two methods are consistent with each other in the regime where both can be applied. The distances to 15 out of 20 galaxies with stable measurements are consistent with that of the targeted group within errors. This suggests that assuming group membership based solely on projected proximity is {\$\sim${}}75{\%} successful in this regime. The galaxies are nearly round, with a median axis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The objects have a range of sizes, from {\$}R{\_}e{\$}=0.4 kpc to {\$}R{\_}e{\$}=1.8 kpc, with a median of 1.0 kpc. They range in luminosity from {\$}M{\_}V{\$}=-11.4 to {\$}M{\_}V{\$}=-15.6, with a median of -12.4. Galaxies with {\$}R{\_}e{\$}{\$\sim${}}1 kpc and {\$}M{\_}V{\$}{\$\sim${}}-12 are fairly rare in the Local Group but we find many of them in this relatively small sample. Four of the objects fall in the class of ultra diffuse galaxies (UDGs), with {\$}R{\_}e{\$}{\textgreater}1.5 kpc and {\$}\backslashmu{\_}{\{}0,V{\}}{\$}{\textgreater}24 mag/arcsec{\^{}}2, including the recently identified dark matter deficient galaxy NGC1052-DF2.}, -archivePrefix = {arXiv}, -arxivId = {1807.06016}, -author = {Cohen, Yotam and van Dokkum, Pieter and Danieli, Shany and Romanowsky, Aaron J and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Mowla, Lamiya and Kruijssen, J M Diederik and Conroy, Charlie and Wasserman, Asher}, -doi = {10.3847/1538-4357/aae7c8}, -eprint = {1807.06016}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {Astrophysics,Astrophysics of Galaxies}, -number = {2}, -pages = {96}, -title = {{ The Dragonfly Nearby Galaxies Survey. V. HST /ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC 1052, NGC 1084, M96, and NGC 4258 }}, -url = {http://arxiv.org/abs/1807.06016%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aae7c8}, -volume = {868}, -year = {2018} -} -@article{Massey2004, -abstract = {We study the accuracy with which weak lensing measurements could be made from a future space-based survey, predicting the subsequent precisions of 3-dimensional dark matter maps, projected 2-dimensional dark matter maps, and mass-selected cluster catalogues. As a baseline, we use the instrumental specifications of the Supernova/Acceleration Probe (SNAP) satellite. We first compute its sensitivity to weak lensing shear as a function of survey depth. Our predictions are based on detailed image simulations created using `shapelets', a complete and orthogonal parameterization of galaxy morphologies. We incorporate a realistic redshift distribution of source galaxies, and calculate the average precision of photometric redshift recovery using the SNAP filter set to be Delta z=0.034. The high density of background galaxies resolved in a wide space-based survey allows projected dark matter maps with a rms sensitivity of 3% shear in 1 square arcminute cells. This will be further improved using a proposed deep space-based survey, which will be able to detect isolated clusters using a 3D lensing inversion techniques with a 1 sigma mass sensitivity of approximately 10^13 solar masses at z$\sim$0.25. Weak lensing measurements from space will thus be able to capture non-Gaussian features arising from gravitational instability and map out dark matter in the universe with unprecedented resolution.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0304418}, -author = {Massey, Richard and Rhodes, Jason and Refregier, Alexandre and Albert, Justin and Bacon, David and Bernstein, Gary and Ellis, Richard and Jain, Bhuvnesh and McKay, Tim and Perlmutter, Saul and Taylor, Andy}, -doi = {10.1086/420985}, -eprint = {0304418}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Gravitational Lensing,Cosmology: Large-Scale Structure of Universe,Space Vehicles: General}, -month = {jun}, -number = {6}, -pages = {3089--3101}, -primaryClass = {arXiv:astro-ph}, -title = {{Weak Lensing from Space. II. Dark Matter Mapping}}, -url = {http://stacks.iop.org/1538-3881/127/i=6/a=3089}, -volume = {127}, -year = {2004} -} -@article{Balm??s2013, -abstract = {Bayesian model selection methods provide a self-consistent probabilistic framework to test the validity of competing scenarios given a set of data. We present a case study application to strong gravitational lens parametric models. Our goal is to select a homogeneous lens subsample suitable for cosmological parameter inference. To this end we apply a Bayes factor analysis to a synthetic catalogue of 500 lenses with power-law potential and external shear. For simplicity, we focus on double-image lenses (the largest fraction of lens in the simulated sample) and select a subsample for which astrometry and time-delays provide strong evidence for a simple power-law model description. Through a likelihood analysis we recover the input value of the Hubble constant to within 3$\sigma$ statistical uncertainty. We apply this methodology to a sample of double-image-lensed quasars. In the case of B1600+434, SBS 1520+530 and SDSS J1650+4251 the Bayes' factor analysis favours a simple power-law model description with high statistical significance. Assuming a flat ̂ cold dark matter cosmology, the combined likelihood data analysis of such systems gives the Hubble constant H0 = 76+15-5 km s-1 Mpc-1 having marginalized over the lens model parameters, the cosmicmatter density and consistently propagated the observational errors on the angular position of the images. The next generation of cosmic structure surveys will provide larger lens data sets and the method described here can be particularly useful to select homogeneous lens subsamples adapted to perform unbiased cosmological parameter inference. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1206.5801v1}, -author = {Balm{\`{e}}s, I. and Corasaniti, P. S.}, -doi = {10.1093/mnras/stt260}, -eprint = {arXiv:1206.5801v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing,Observations-cosmology,Statistical-cosmology,Strong-methods,Theory}, -number = {2}, -pages = {1528--1540}, -title = {{Bayesian approach to gravitational lens model selection: Constraining H0 with a selected sample of strong lenses}}, -volume = {431}, -year = {2013} -} -@article{Rusin2000, -abstract = {The behaviour of the mineral matter in a fuel may crucially affect the availability of a boiler when the fuel is fired. The ash may cause severe problems in the flue gas channel in forms of fireside deposits on heat exchangers. These deposits lower the efficiency of the boiler and cause in the most severe cases an unscheduled shutdown. In this paper we report results from a study where the ash behaviour was monitored in a pulverized wood fired boiler. Short-term deposit sampling was combined with in situ fly ash and flue gas sampling as well as advanced fuel analyses. By combining these three tools we could track down a chain of events the ash went through from the point where it was introduced into the boiler with the fuel until the stage where it formed a deposit on a heat exchanger tube. Sub-micron sized ash particles found in the flue gas with a Berner-type low-pressure impactor were enriched in alkali, sulphur and chlorine. Similar particles were also found on the backside of the air-cooled deposit sampling probes, forming thin initial alkali, sulphur and chlorine-rich deposit layer. These elements were further found by advanced fuel analysis to be associated with the moisture or the organic phase of the fuel. Larger ash particles of the size of 1-10 ??m found in the flue gas with the low-pressure impactor were found to deposit on the front side of the sampling probe. These particles consisted mainly of calcium, most likely oxide or carbonate. With the advanced fuel analyses we could find these particles already as mineral particles in the wood fuel. We also saw some indication that peat could act as a cleaning fuel. In general the results show that a detailed well-performed fuel analysis is a key knowledge when ash behaviour predictions are to be made. ?? 2004 Elsevier Ltd. All rights reserved.}, -author = {Rusin, David and Ma, Chung-Pei}, -doi = {10.1086/319129}, -isbn = {0016-2361}, -issn = {0004637X}, -journal = {ApJ}, -number = {1}, -pages = {L33--L37}, -title = {{Constraints on the Inner Mass Profiles of Lensing Galaxies from Missing Odd Images}}, -url = {http://stacks.iop.org/1538-4357/549/i=1/a=L33}, -volume = {549}, -year = {2001} -} -@article{Auger2009, -abstract = {We use stellar masses, surface photometry, strong-lensing masses, and stellar velocity dispersions ($\sigma$e/2) to investigate empirical correlations for the definitive sample of 73 early-type galaxies (ETGs) that are strong gravitational lenses from the SLACS survey. The traditional correlations (fundamental plane (FP) and its projections) are consistent with those found for non-lens galaxies, supporting the thesis that SLACS lens galaxies are representative of massive ETGs (dimensional massMdim = 1011-1012 M⊙). The addition of high-precision stronglensing estimates of the total mass allows us to gain further insights into their internal structure: (1) the average slope of the total mass-density profile ($\rho$tot $\alpha$ r-$\gamma$') is ($\gamma$') = 2.078 ± 0.027 with an intrinsic scatter of 0.16 ± 0.02; (2) $\gamma$' correlates with effective radius (re) and central mass density, in the sense that denser galaxies have steeper profiles; (3) the dark matter (DM) fraction within r e/2 is a monotonically increasing function of galaxy mass and size (due to a mass-dependent central cold DM distribution or due to baryonic DM-stellar remnants or low-mass stars-if the initial mass function is non-universal and its normalization increases with mass); (4) the dimensional mass Mdim = 5re$\sigma$e/22/G is proportional to the total (lensing) mass Mre/2, and both increase more rapidly than stellar mass M* (M* $\alpha$ M0.8re/2); (5) the mass plane (MP), obtained by replacing surface brightness with surface mass density in the FP, is found to be tighter and closer to the virial relation than the FP and the M *.P, indicating that the scatter of those relations is dominated by stellar population effects; (6) we construct the fundamental hyper-plane by adding stellar masses to the MP and find the M* coefficient to be consistent with zero and no residual intrinsic scatter. Our results demonstrate that the dynamical structure of ETGs is not scale invariant and that it is fully specified by Mre/2, re, and $\sigma$e/2. Although the basic trends can be explained qualitatively in terms of varying star formation efficiency as a function of halo mass and as the result of dry and wet mergers, reproducing quantitatively the observed correlations and their tightness may be a significant challenge for galaxy formation models.}, -archivePrefix = {arXiv}, -arxivId = {1007.2880}, -author = {Auger, M. W. and Treu, T. and Bolton, A. S. and Gavazzi, R. and Koopmans, L. V.E. and Marshall, P. J. and Moustakas, L. A. and Burles, S.}, -doi = {10.1088/0004-637X/724/1/511}, -eprint = {1007.2880}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {CD,Dark matter,Galaxies: elliptical and lenticular,Galaxies: fundamental parameters,Galaxies: structure,Gravitational lensing: strong}, -number = {1}, -pages = {511--525}, -title = {{The sloan lens ACS survey. X. Stellar, dynamical, and total mass correlations of massive early-type galaxies}}, -url = {http://stacks.iop.org/0004-637X/724/i=1/a=511?key=crossref.2a8f66f24819ad7316941c9449a63c7f}, -volume = {724}, -year = {2010} -} -@article{Vieira2013, -abstract = {In the past decade, our understanding of galaxy evolution has been revolutionized by the discovery that luminous, dusty starburst galaxies were 1,000 times more abundant in the early Universe than at present. It has, however, been difficult to measure the complete redshift distribution of these objects, especially at the highest redshifts (z>4). Here we report a redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources. High-resolution imaging demonstrates that these sources are strongly gravitationally lensed by foreground galaxies. We detect spectral lines in 23 out of 26 sources and multiple lines in 12 of those 23 sources, from which we obtain robust, unambiguous redshifts. At least 10 of the sources are found to lie at z>4, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought. Models of lens geometries in the sample indicate that the background objects are ultra-luminous infrared galaxies, powered by extreme bursts of star formation. {\textcopyright} 2013 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1303.2723}, -author = {Vieira, J. D. and Marrone, D. P. and Chapman, S. C. and {De Breuck}, C. and Hezaveh, Y. D. and Wei, A. and Aguirre, J. E. and Aird, K. A. and Aravena, M. and Ashby, M. L.N. and Bayliss, M. and Benson, B. A. and Biggs, A. D. and Bleem, L. E. and Bock, J. J. and Bothwell, M. and Bradford, C. M. and Brodwin, M. and Carlstrom, J. E. and Chang, C. L. and Crawford, T. M. and Crites, A. T. and {De Haan}, T. and Dobbs, M. A. and Fomalont, E. B. and Fassnacht, C. D. and George, E. M. and Gladders, M. D. and Gonzalez, A. H. and Greve, T. R. and Gullberg, B. and Halverson, N. W. and High, F. W. and Holder, G. P. and Holzapfel, W. L. and Hoover, S. and Hrubes, J. D. and Hunter, T. R. and Keisler, R. and Lee, A. T. and Leitch, E. M. and Lueker, M. and Luong-Van, D. and Malkan, M. and McIntyre, V. and McMahon, J. J. and Mehl, J. and Menten, K. M. and Meyer, S. S. and Mocanu, L. M. and Murphy, E. J. and Natoli, T. and Padin, S. and Plagge, T. and Reichardt, C. L. and Rest, A. and Ruel, J. and Ruhl, J. E. and Sharon, K. and Schaffer, K. K. and Shaw, L. and Shirokoff, E. and Spilker, J. S. and Stalder, B. and Staniszewski, Z. and Stark, A. A. and Story, K. and Vanderlinde, K. and Welikala, N. and Williamson, R.}, -doi = {10.1038/nature12001}, -eprint = {1303.2723}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Viera2013DSFG.pdf:pdf}, -issn = {00280836}, -journal = {Nature}, -number = {7441}, -pages = {344--347}, -title = {{Dusty starburst galaxies in the early Universe as revealed by gravitational lensing}}, -volume = {495}, -year = {2013} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in SPH simulations. About half the gas shock heats to roughly the virial temperature of the galaxy potential well before cooling, condensing, and forming stars, but the other half radiates its acquired gravitational energy at much lower temperatures, typically T{\textless}10{\^{}}5 K, and the histogram of maximum gas temperatures is clearly bimodal. The "cold mode" of gas accretion dominates for low mass galaxies (M{\_}baryon {\textless} 10{\^{}}{\{}10.3{\}}Msun or M{\_}halo {\textless} 10{\^{}}{\{}11.4{\}}Msun), while the conventional "hot mode" dominates the growth of high mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasi-spherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with cold mode dominating at high redshift and in low density regions today, and hot mode dominating in group and cluster environments at low redshift. Star formation rates closely track accretion rates, and we discuss the physics behind the observed environment and redshift dependence of galactic scale star formation. If we allowed hot accretion to be suppressed by conduction or AGN feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colors of ellipticals and the cutoff of the galaxy luminosity function. The transition between cold and hot accretion at M{\_}h {\$\sim${}} 10{\^{}}{\{}11.4{\}}Msun is similar to that found by Birnboim {\&} Dekel (2003) using 1-d simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. (2003) find a marked shift in galaxy properties. We speculate on connections between these theoretical and observational transitions.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centers of typical {\$\sim${}}L* and lower-mass spheroids exhibit power law 'cusps' with {\$}\backslashSigma \backslashpropto R{\^{}}(-n){\$}, where 0.5{\textless}n{\textless}1 for radii {\$\sim${}}1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for or strongly modify the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m=1 lopsided/eccentric disk instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*({\textless}R){\textless}{\textless}M{\_}BH. When the stellar surface density profile is comparatively shallow with n{\textless}1/2, the modes cannot efficiently propagate to R=0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than n=1, the inwards propagation of eccentricity is strongly damped, suppressing inflow and bringing n down again. Together these results produce an equilibrium slope of 1/2 {\textless} n {\textless} 1 in the potential of the central black hole. These physical arguments are supported by nonlinear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Geometryej, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(9).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Postman2012, -abstract = {Hubble Space Telescope images of the galaxy cluster A2261, obtained as part of the Cluster Lensing And Supernova survey with Hubble, show that the brightest galaxy in the cluster, A2261-BCG, has the largest core yet detected in any galaxy. The cusp radius of A2261-BCG is 3.2kpc, twice as big as the next largest core known, and 3 × bigger than those typically seen in the most luminous brightest cluster galaxies. The morphology of the core in A2261-BCG is also unusual, having a completely flat interior surface brightness profile, rather than the typical shallow cusp rising into the center. This implies that the galaxy has a core with constant or even centrally decreasing stellar density. Interpretation of the core as an end product of the "scouring" action of a binary supermassive black hole implies a total black hole mass 1010 M from the extrapolation of most relationships between core structure and black hole mass. The core falls 1$\sigma$ above the cusp radius versus galaxy luminosity relation. Its large size in real terms, and the extremely large black hole mass required to generate it, raises the possibility that the core has been enlarged by additional processes, such as the ejection of the black holes that originally generated the core. The flat central stellar density profile is consistent with this hypothesis. The core is also displaced by 0.7kpc from the center of the surrounding envelope, consistent with a local dynamical perturbation of the core. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -author = {Postman, Marc and Lauer, Tod R. and Donahue, Megan and Graves, Genevieve and Coe, Dan and Moustakas, John and Koekemoer, Anton and Bradley, Larry and Ford, Holland C. and Grillo, Claudio and Zitrin, Adi and Lemze, Doron and Broadhurst, Tom and Moustakas, Leonidas and Ascaso, Bego{\~{n}}a and Medezinski, Elinor and Kelson, Daniel}, -doi = {10.1088/0004-637X/756/2/159}, -file = {:C\:/Users/Jammy/Documents/Papers/Postman2012Abell.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: nuclei,galaxies: photometry,galaxies: structure}, -number = {2}, -pages = {159}, -title = {{A brightest cluster galaxy with an extremely large flat core}}, -volume = {756}, -year = {2012} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of stellar parameters and abundances ("stellar labels") for hundreds of thousands of stars; this poses a formidable spectral modeling challenge. In many cases, there is a subset of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the "known" labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with and as the labels, and then applying it to the spectra of 55,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one-ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ness, M. and Hogg, David W. and Rix, H. W. and Ho, Anna Y.Q. and Zasowski, G.}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ness et al. - 2015 - THE CANNON A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{THE CANNON: A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION}}, -volume = {808}, -year = {2015} -} -@article{Vegetti2018, -abstract = {We use the observed amount of subhaloes and line-of-sight dark matter haloes in a sample of 11 gravitational lens systems from the Sloan Lens ACS Survey to constrain the free-streaming properties of the dark matter particles. In particular, we combine the detection of a small-mass dark matter halo by Vegetti et al. with the non-detections by Vegetti et al. and compare the derived subhalo and halo mass functions with expectations from cold dark matter (CDM) and resonantly produced sterile neutrino models. We constrain the half-mode mass, i.e. the mass scale at which the linear matter power spectrum is reduced by 50 per cent relatively to the CDM model, to be log Mhm[M⊙] < 12.0 (equivalent thermal relic mass mth > 0.3 keV) at the 2s level. This excludes sterile neutrino models with neutrino masses ms < 0.8 keV at any value of L6. Our constraints are weaker than currently provided by the number of MilkyWay satellites, observations of the 3.5 keV X-ray line, and the Lyman a forest. However, they are more robust than the former as they are less affected by baryonic processes. Moreover, unlike the latter, they are not affected by assumptions on the thermal histories for the intergalactic medium. Gravitational lens systems with higher data quality and higher source and lens redshift are required to obtain tighter constraints.}, -archivePrefix = {arXiv}, -arxivId = {1801.01505}, -author = {Vegetti, S. and Despali, G. and Lovell, M. R. and Enzi, W.}, -doi = {10.1093/mnras/sty2393}, -eprint = {1801.01505}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Vegetti et al. - 2018 - Constraining sterile neutrino cosmologies with strong gravitational lensing observations at redshift z $\sim$ 0.2.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {3}, -pages = {3661--3669}, -title = {{Constraining sterile neutrino cosmologies with strong gravitational lensing observations at redshift z $\sim$ 0.2}}, -volume = {481}, -year = {2018} -} -@article{Guo:2008aa, -abstract = {We use galaxy and dark halo data from the public database for the Millennium Simulation to study the growth of galaxies in the De Lucia et al. model for galaxy formation. Previous work has shown this model to reproduce many aspects of the systematic properties and the clustering of real galaxies, both in the nearby universe and at high redshift. It assumes the stellar masses of galaxies to increase through three processes, major mergers, the accretion of smaller satellite systems and star formation. We show the relative importance of these three modes to be a strong function of stellar mass and redshift. Galaxy growth through major mergers depends strongly on stellar mass, but only weakly on redshift. Except for massive systems, minor mergers contribute more to galaxy growth than major mergers at all redshifts and stellar masses. For galaxies significantly less massive than the Milky Way, star formation dominates the growth at all epochs. For galaxies significantly more massive than the Milky Way, growth through mergers is the dominant process at all epochs. At a stellar mass of 6 × 1010 M⊙, about that of the Milk Way, star formation dominates at z > 1 and mergers at later times. At every stellar mass, the growth rates through star formation increase rapidly with increasing redshift. Specific star formation rates are the decreasing function of stellar mass not only at z = 0 but also at all higher redshifts. For comparison, we carry out a similar analysis of the growth of dark matter haloes. In contrast to the galaxies, growth rates depend strongly on redshift, but only weakly on mass. They agree qualitatively with analytic predictions for halo growth. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0708.1814}, -author = {Guo, Q. and White, S. D.M.}, -doi = {10.1111/j.1365-2966.2007.12619.x}, -eprint = {0708.1814}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Guo, White - 2008 - Galaxy growth in the concordance $\Lambda$cDM cosmology.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution,Galaxies: formation,Galaxies: high-redshift,Galaxies: interactions}, -month = {feb}, -number = {1}, -pages = {2--10}, -title = {{Galaxy growth in the concordance $\Lambda$cDM cosmology}}, -url = {http://adsabs.harvard.edu/abs/2008MNRAS.384....2G}, -volume = {384}, -year = {2008} -} -@article{Sirianni2004, -abstract = {The Advanced Camera for Surveys (ACS), installed in the Hubble Space Telescope (HST) in March 2002, comprises three cameras: the Wide Field Camera (WFC), designed for deep near-IR survey imaging programs; the High Resolution Camera (HRC), a high angular resolution imager which fully samples the HST full spread function (PSF) in the visible; and the Solar Blind Camera (SBC), a far-UV imager. The WFC and HRC employ CCD detectors. Their performances are affected by the on-going damage due to the space radiation environment where they operate. We present an overview of the performance of the ACS CCD detectors, based on the first two years of flight science operations. We analyze the evolution with time of the basic detector performance that are subjected to degradation due to the on-going radiation damage. Comparison is made with ground testing prediction and with the amount of performance degradation seen in other CCD detectors on board of HST.}, -author = {Sirianni, Marco and Mutchler, Max and Clampin, Mark and Ford, Holland and Illingworth, Garth and Hartig, George and van Orsow, Doug and Wheeler, Thomas}, -doi = {10.1117/12.552584}, -issn = {0277786X}, -journal = {Optical and Infrared Detectors for Astronomy}, -number = {January 2014}, -pages = {173}, -title = {{Performance of the Advanced Camera for Surveys CCDs after two years on orbit}}, -volume = {5499}, -year = {2004} -} -@inproceedings{MartinNavarro2013, -abstract = {We have developed an innovative 'index scanning technique” to map the stellar kinematics of early-type galaxies by measuring for the first time the absorption line strength of the near-IR CaII triplet with the Red Tunable Filters of OSIRIS at GTC. Unlike classical spectroscopy, these filters allow us to perform a two-dimensional study, taking advantage of a 10.4 meter class telescope with a unvignetted field of view of 7.8 × 7.8 arcmin. We show the velocity fields obtained for two Virgo elliptical galaxies of very different masses and their globular cluster systems reaching galactocentric distances beyond 2 effective radii.}, -author = {Mart{\'{i}}n-Navarro, Ignacio and Vazdekis, Alexander and Bongiovanni, {\'{A}}ngel and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and Cepa, Jordi and Cenarro, Javier and S{\'{a}}nchez-Bl{\'{a}}zquez, Patricia}, -booktitle = {Proceedings of the 10th Scientific Meeting of the Spanish Astronomical Society - Highlights of Spanish Astrophysics VII, SEA 2012}, -editor = {Guirado, J.$\sim$C. and Lara, L.$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable filters at gtc: A novel approach}}, -year = {2020} -} -@article{Jaroszynski2012, -abstract = {We investigate strong lensing by non-singular finite isothermal ellipsoids taking into account the influence of the matter along the line of sight and in the close lens vicinity. We compare three descriptions of light propagation: the full approach taking into account all matter inhomogeneities along the rays, the single plane approach, where we take into account the influence of the strong lens neighbours but neglect the foreground and background objects, and the single lens approach. In each case we simulate many strong lensing configurations placing a point source at the same redshift but in different locations inside the region surrounded by caustics. We further analyze configurations of four or five images. For every simulated strong lensing configuration we attempt to fit a simplified lens model using a single isothermal ellipsoid or a single isothermal ellipsoid with external shear. The single lens fits to configurations obtained in the full approach are rejected in majority of cases with 95{\%} significance. For configurations obtained in the single plane approach the rejection rate is substantially lower. Also the inclusion of external shear in simplified modeling improves the chances of obtaining acceptable fits, but the problem is not solved completely. The quantitative estimates of the rates of rejection of simplified models depend on the required accuracy of the models, and we present few illustrative examples, which show that both matter close to the lens and matter along the rays do have important influence on lens modeling. We also estimate the typical value of the external shear and compare the fitted parameters of the simplified models with the parameters of the lenses used in the simulations.}, -archivePrefix = {arXiv}, -arxivId = {1204.6223}, -author = {Jaroszynski, M and Kostrzewa-Rutkowska, Z}, -doi = {10.1111/j.1365-2966.2012.21197.x}, -eprint = {1204.6223}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: strong,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {1}, -pages = {325--332}, -title = {{Background, foreground and nearby matter influence on strong gravitational lenses}}, -volume = {424}, -year = {2012} -} -@article{Xu2015, -abstract = {A power-law density model, i.e. $\rho$(r) ∝ r-$\gamma$', has been commonly employed in strong gravitational lensing studies, including the so-called time-delay technique used to infer the Hubble constant H0. However, since the radial scale at which strong lensing features are formed corresponds to the transition from the dominance of baryonic matter to dark matter, there is no known reason why galaxies should follow a power law in density. The assumption of a power law artificially breaks the mass-sheet degeneracy, a well-known invariance transformation in gravitational lensing which affects the product of Hubble constant and time delay and can therefore cause a bias in the determination of H0 from the time-delay technique. In this paper, we use the Illustris hydrodynamical simulations to estimate the amplitude of this bias, and to understand how it is related to observational properties of galaxies. Investigating a large sample of Illustris galaxies that have velocity dispersion $\sigma$SIE ≤ 160 km s-1 at redshifts below z = 1, we find that the bias on H0 introduced by the power-law assumption can reach 20-50 per cent, with a scatter of 10-30 per cent (rms). However, we find that by selecting galaxies with an inferred power-law model slope close to isothermal, it is possible to reduce the bias on H0 to ≲ 5 per cent and the scatter to ≲ 10 per cent. This could potentially be used to form less biased statistical samples for H0 measurements in the upcoming large survey era.}, -archivePrefix = {arXiv}, -arxivId = {1507.07937}, -author = {Xu, Dandan and Sluse, Dominique and Schneider, Peter and Springel, Volker and Vogelsberger, Mark and Nelson, Dylan and Hernquist, Lars}, -doi = {10.1093/mnras/stv2708}, -eprint = {1507.07937}, -isbn = {1466-2094}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {1}, -pages = {739--755}, -title = {{Lens galaxies in the illustris simulation: Power-law models and the bias of the Hubble constant from time delays}}, -volume = {456}, -year = {2016} -} -@article{Oh2016, -abstract = {We investigate two-dimensional image decomposition of nearby, morphologically selected early-type galaxies (ETGs). We are motivated by recent observational evidence of significant size growth of quiescent galaxies and theoretical development advocating a two-phase formation scenario for ETGs. We find that a significant fraction of nearby ETGs show changes in isophotal shape that require multi-component models. The characteristic sizes of the inner and outer component are $\sim 3$ and $\sim 15$ kpc. The inner component lies on the mass-size relation of ETGs at $z \sim 0.25-0.75$, while the outer component tends to be more elliptical and hints at a stochastic buildup process. We find real physical differences between the single- and double-component ETGs, with the double-component galaxies being younger and more metal-rich. The fraction of double component ETGs increases with increasing $\sigma$ and decreases in denser environments. We hypothesize that double-component systems were able to accrete gas and small galaxies until later times, boosting their central densities, building up their outer parts, and lowering their typical central ages. In contrast, the oldest galaxies, perhaps due to residing in richer environments, have no remaining hints of their last accretion episode.}, -archivePrefix = {arXiv}, -arxivId = {1612.06495}, -author = {Oh, Semyeong and Greene, Jenny E. and Lackner, Claire N.}, -doi = {10.3847/1538-4357/836/1/115}, -eprint = {1612.06495}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oh, Greene, Lackner - 2017 - Testing the Presence of Multiple Photometric Components in Nearby Early-type Galaxies Using SDSS(4).pdf:pdf}, -issn = {1538-4357}, -journal = {ApJ}, -keywords = {cD,cd,elliptical and lenticular,evolution,galaxies,galaxies: elliptical and lenticular,galaxies: evolution,machine-readable table,supporting material}, -number = {1}, -pages = {115}, -publisher = {IOP Publishing}, -title = {{Testing the Presence of Multiple Photometric Components in Nearby Early-type Galaxies Using SDSS}}, -url = {http://arxiv.org/abs/1612.06495%0Ahttp://dx.doi.org/10.3847/1538-4357/836/1/115}, -volume = {836}, -year = {2017} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo {\textgreater} 1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from {\$\sim${}}30° to 10° for M {\$\sim${}} 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles. {\textcopyright}2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z ? 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u - g color profiles for these galaxies and show that most z ? 2galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z ? 2galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: (?(u - g rest)/?(log r))median = -0.47, -0.33, and -0.46 for z ? 2, z ? 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z ? 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u - g colors, and lower S?rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch. ? 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J and {Van Dokkum}, Pieter G and Labb{\'{e}}, Ivo and Illingworth, Garth D and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Newman2012a, -abstract = {The presence of extremely compact galaxies at z{\$\sim${}}2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 host galaxies selected with 0.4{\textless}z{\textless}2.5 and stellar masses M* {\textgreater} 10{\^{}}10.7 Msol using optical and near-infrared photometry in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and we find that the mean size of these systems grows by a factor of 3.5 +- 0.3 over this redshift interval. The new data are sufficiently deep to enable us to identify companions to these hosts whose stellar masses are ten times smaller, while still yielding suitably accurate photometric redshifts to define a likely physical association. By searching for faint companions around 404 quiescent hosts within a projected physical annulus 10 {\textless} R {\textless} 30 kpc/h, we estimate the minor merger rate over the redshift range 0.4 {\textless} z {\textless} 2. After correcting for contamination from projected pairs, we find that 13-18{\%} of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6+-2{\%} per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model of merging motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers with mass ratios {\textgreater} 0.1 may explain most of the size evolution observed at z {\textgreater}{\$\sim${}} 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes.}, -archivePrefix = {arXiv}, -arxivId = {1110.1637}, -author = {Newman, Andrew B and Ellis, Richard S and Bundy, Kevin and Treu, Tommaso}, -doi = {10.1088/0004-637X/746/2/162}, -eprint = {1110.1637}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: structure}, -number = {2}, -title = {{Can minor merging account for the size growth of quiescent galaxies? New results from the CANDELS survey}}, -volume = {746}, -year = {2012} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Naab2007, -abstract = {We describe high-resolution smoothed particle hydrodynamics (SPH) simulations of three approximately M* field galaxies starting from $\Lambda$CDM initial conditions. The simulations are made intentionally simple, and include photoionization, cooling of the intergalactic medium, and star formation, but not feedback from AGNs or supernovae. All of the galaxies undergo an initial burst of star formation at z{\$\sim${}}5, accompanied by the formation of a bubble of heated gas. Two out of three galaxies show early-type properties at present, whereas only one of them experienced a major merger. Heating from shocks and PdV work dominates over cooling so that for most of the gas the temperature is an increasing function of time. By z{\$\sim${}}1 a significant fraction of the final stellar system is in place and the spectral energy distribution resembles those of observed massive red galaxies. The galaxies have grown from z=1--{\textgreater}0 on average by 25{\%} in mass and in size by gas-poor (dry) stellar mergers. By the present day the simulated galaxies are old ({\$\sim${}}10 Gyr), kinematically hot stellar systems surrounded by hot gaseous haloes. Stars dominate the mass of the galaxies up to {\$\sim${}}4 effective radii ({\$\sim${}}10 kpc). Kinematic and most photometric properties are in good agreement with those of observed elliptical galaxies. The galaxy with a major merger develops a counter-rotating core. Our simulations show that realistic intermediate-mass giant elliptical galaxies with plausible formation histories can be formed from $\Lambda$CDM initial conditions even without requiring recent major mergers or feedback from supernovae or AGNs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0512235}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P and Efstathiou, George}, -doi = {10.1086/510841}, -eprint = {0512235}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {710--720}, -primaryClass = {astro-ph}, -title = {{Formation of Early‐Type Galaxies from Cosmological Initial Conditions}}, -url = {http://stacks.iop.org/0004-637X/658/i=2/a=710}, -volume = {658}, -year = {2007} -} -@article{Bellstedt2018, -abstract = {We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 1010 {\textless} M*/M⊙ {\textless} 1011.6 that cover a large radial range of 0.1-4.0 effective radii.We combine SLUGGS and ATLAS3D data sets to model the total-mass profiles of a sample of 21 fast-rotator galaxies, utilizing a hyperparameter method to combine the two independent data sets. The total-mass density profile slope values derived for these galaxies are consistent with those measured in the inner regions of galaxies by other studies. Furthermore, the total-mass density slopes ($\gamma$tot) appear to be universal over this broad stellar mass range, with an average value of $\gamma$tot= -2.24± 0.05, i.e. slightly steeper than isothermal. We compare our results to model galaxies from the Magneticum and EAGLE cosmological hydrodynamic simulations, in order to probe the mechanisms that are responsible for varying total-mass density profile slopes. The simulated-galaxy slopes are shallower than the observed values by {\$\sim${}}0.3-0.5, indicating that the physical processes shaping the mass distributions of galaxies in cosmological simulations are still incomplete. For galaxies with M* {\textgreater} 1010.7M⊙ in the Magneticum simulations, we identify a significant anticorrelation between total-mass density profile slopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas this anticorrelation is weaker for lower stellar masses, implying that the measured total-mass density slopes for low-mass galaxies are less likely to be determined by merger activity.}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A and Romanowsky, Aaron J and Remus, Rhea Silvia and Stevens, Adam R H and Brodie, Jean P and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to {\$\sim${}}4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Geometryef, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Etherington2022, -abstract = {The distribution of dark and luminous matter can be mapped around galaxies that gravitationally lens background objects into arcs or Einstein rings. New surveys will soon observe hundreds of thousands of galaxy lenses, and current, labour-intensive analysis methods will not scale up to this challenge. We develop an automatic, Bayesian method which we use to fit a sample of 59 lenses imaged by the Hubble Space Telescope. We set out to leave no lens behind and focus on ways in which automated fits fail in a small handful of lenses, describing adjustments to the pipeline that ultimately allows us to infer accurate lens models for all 59 lenses. A high success rate is key to avoid catastrophic outliers that would bias large samples with small statistical errors. We establish the two most difficult steps to be subtracting foreground lens light and initialising a first, approximate lens model. After that, increasing model complexity is straightforward. We put forward a likelihood cap method to avoid the underestimation of errors due to pixel discretization noise inherent to pixel-based methods. With this new approach to error estimation, we find a mean $\sim 1{{\%}}$ fractional uncertainty on the Einstein radius measurement which does not degrade with redshift up to at least z = 0.7. This is in stark contrast to measurables from other techniques, like stellar dynamics, and demonstrates the power of lensing for studies of galaxy evolution. Our PyAutoLens software is open source, and is installed in the Science Data Centres of the ESA Euclid mission.}, -archivePrefix = {arXiv}, -arxivId = {2202.09201}, -author = {Etherington, Amy and Nightingale, James W and Massey, Richard and Cao, XiaoYue and Robertson, Andrew and Amorisco, Nicola C and Amvrosiadis, Aristeidis and Cole, Shaun and Frenk, Carlos S and He, Qiuhan and Li, Ran and Tam, Sut-Ieng}, -doi = {10.1093/mnras/stac2639}, -eprint = {2202.09201}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Etherington2022SLaM.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {Etherington2022,dark matter,data analysis,fundamental parameters,galaxies,gravitational lensing,software,strong}, -mendeley-tags = {Etherington2022}, -number = {3}, -pages = {3275}, -title = {{Automated galaxy-galaxy strong lens modelling: No lens left behind}}, -url = {http://arxiv.org/abs/2202.09201}, -volume = {517}, -year = {2022} -} -@article{Peng2002, -abstract = {We present a two-dimensional (2-D) fitting algorithm (GALFIT) designed to extract structural components from galaxy images, with emphasis on closely modeling light profiles of spatially well-resolved, nearby galaxies observed with the Hubble Space Telescope. Our algorithm improves on previous techniques in two areas, by being able to simultaneously fit a galaxy with an arbitrary number of components, and with optimization in computation speed, suited for working on large galaxy images. We use 2-D models such as the ``Nuker'' law, the Sersic (de Vaucouleurs) profile, an exponential disk, and Gaussian or Moffat functions. The azimuthal shapes are generalized ellipses that can fit disky and boxy components. Many galaxies with complex isophotes, ellipticity changes, and position-angle twists can be modeled accurately in 2-D. When examined in detail, we find that even simple-looking galaxies generally require at least three components to be modeled accurately, rather than the one or two components more often employed. We illustrate this by way of 7 case studies, which include regular and barred spiral galaxies, highly disky lenticular galaxies, and elliptical galaxies displaying various levels of complexities. A useful extension of this algorithm is to accurately extract nuclear point sources in galaxies. We compare 2-D and 1-D extraction techniques on simulated images of galaxies having nuclear slopes with different degrees of cuspiness, and we then illustrate the application of the program to several examples of nearby galaxies with weak nuclei.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0204182}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans-Walter}, -doi = {10.1086/340952}, -eprint = {0204182}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {1}, -pages = {266--293}, -primaryClass = {astro-ph}, -title = {{Detailed Structural Decomposition of Galaxy Images}}, -url = {http://arxiv.org/abs/astro-ph/0204182%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/340952}, -volume = {124}, -year = {2002} -} -@article{Shao2016, -abstract = {The spatial distribution of the satellite populations of the Milky Way and Andromeda are puzzling in that they are nearly perpendicular to the discs of their central galaxies. To understand the origin of such configurations we study the alignment of the central galaxy, satellite system and dark matter halo in the largest of the 'Evolution and Assembly of GaLaxies and their Environments' (eagle) simulation. We find that centrals and their satellite systems tend to be well aligned with their haloes, with a median misalignment angle of 33° in both cases. While the centrals are better aligned with the inner 10 kpc halo, the satellite systems are better aligned with the entire halo indicating that satellites preferentially trace the outer halo. The central-satellite alignment is weak (median misalignment angle of 52°) and we find that around 20 per cent of systems have a misalignment angle larger than 78°, which is the value for the Milky Way. The central-satellite alignment is a consequence of the tendency of both components to align with the dark matter halo. As a consequence, when the central is parallel to the satellite system, it also tends to be parallel to the halo. In contrast, if the central is perpendicular to the satellite system, as in the case of the Milky Way and Andromeda, then the central-halo alignment is much weaker. Dispersion-dominated (spheroidal) centrals have a stronger alignment with both their halo and their satellites than rotation-dominated (disc) centrals. We also found that the halo, the central galaxy and the satellite system tend to be aligned with the surrounding large-scale distribution of matter, with the halo being the better aligned of the three.}, -archivePrefix = {arXiv}, -arxivId = {1605.01728}, -author = {Shao, Shi and Cautun, Marius and Frenk, Carlos S and Gao, Liang and Crain, Robert A and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw1247}, -eprint = {1605.01728}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3772--3783}, -title = {{Alignments between galaxies, satellite systems and haloes}}, -volume = {460}, -year = {2016} -} -@article{Bluck2015, -abstract = {We derive the dependence of the fraction of passive central galaxies on the mass of their supermassive black holes for a sample of over 400,000 SDSS galaxies at z < 0.2. Our large sample contains galaxies in a wide range of environments, with stellar masses 8 < log(M*/Msun) < 12, spanning the entire morphological spectrum from pure disks to spheroids. We derive estimates for the black hole masses from measured central velocity dispersions and bulge masses, using a variety of published empirical relationships. We find a very strong dependence of the passive fraction on black hole mass, which is largely unaffected by the details of the black hole mass estimate. Moreover, the passive fraction relationship with black hole mass remains strong and tight even at fixed values of galaxy stellar mass (M*), dark matter halo mass (Mhalo), and bulge-to-total stellar mass ratio (B/T). Whereas, the passive fraction dependence on M*, Mhalo and B/T is weak at fixed MBH. These observations show that, for central galaxies, MBH is the strongest correlator with the passive fraction, consistent with quenching from AGN feedback.}, -archivePrefix = {arXiv}, -arxivId = {1412.3862}, -author = {Bluck, Asa F. L. and Ellison, Sara L. and Patton, David R. and Simard, Luc and Mendel, J. Trevor and Teimoorinia, Hossein and Moreno, Jorge and Starkenburg, Else and Road, Finnerty and Columbia, British and Bluck, Asa F. L. and Ellison, Sara L. and Patton, David R. and Simard, Luc and Mendel, J. Trevor and Teimoorinia, Hossein and Moreno, Jorge and Starkenburg, Else}, -eprint = {1412.3862}, -journal = {MNRAS}, -keywords = {agn,black holes,evolution,formation,galaxies,morphology,star formation}, -number = {December 2014}, -pages = {6}, -title = {{Why do galaxies stop forming stars? I. The passive fraction - black hole mass relation for central galaxies}}, -url = {http://arxiv.org/abs/1412.3862}, -volume = {000}, -year = {2014} -} -@article{Vehtari2020, -abstract = {A common divide-and-conquer approach for Bayesian computation with big data is to partition the data, perform local inference for each piece separately, and combine the results to obtain a global posterior approximation. While being conceptually and computationally appealing, this method involves the problematic need to also split the prior for the local inferences; these weakened priors may not provide enough regularization for each separate computation, thus eliminating one of the key advantages of Bayesian methods. To resolve this dilemma while still retaining the generalizability of the underlying local inference method, we apply the idea of expectation propagation (EP) as a framework for distributed Bayesian inference. The central idea is to iteratively update approximations to the local likelihoods given the state of the other approximations and the prior. The present paper has two roles: we review the steps that are needed to keep EP algorithms numerically stable, and we suggest a general approach, inspired by EP, for approaching data partitioning problems in a way that achieves the computational benefits of parallelism while allowing each local update to make use of relevant information from the other sites. In addition, we demonstrate how the method can be applied in a hierarchical context to make use of partitioning of both data and parameters. The paper describes a general algorithmic framework, rather than a specific algorithm, and presents an example implementation for it.}, -archivePrefix = {arXiv}, -arxivId = {1412.4869}, -author = {Vehtari, Aki and Gelman, Andrew and Sivula, Tuomas and Jyl{\"{a}}nki, Pasi and Tran, Dustin and Sahai, Swupnil and Blomstedt, Paul and Cunningham, John P. and Schiminovich, David and Robert, Christian P.}, -eprint = {1412.4869}, -file = {:C\:/Users/Jammy/Documents/Papers/Stats/Vehtair2020EP.pdf:pdf}, -issn = {15337928}, -journal = {Journal of Machine Learning Research}, -keywords = {Bayesian computation,Data partitioning,Expectation propagation,Hierarchical models,Statistical computing}, -pages = {1--53}, -title = {{Expectation propagation as a way of life: A framework for Bayesian inference on partitioned data}}, -volume = {21}, -year = {2020} -} -@article{Rizzo2020, -abstract = {The extreme astrophysical processes and conditions that characterize the early Universe are expected to result in young galaxies that are dynamically different from those observed today1–5. This is because the strong effects associated with galaxy mergers and supernova explosions would lead to most young star-forming galaxies being dynamically hot, chaotic and strongly unstable1,2. Here we report the presence of a dynamically cold, but highly star-forming, rotating disk in a galaxy at redshift6z = 4.2, when the Universe was just 1.4 billion years old. Galaxy SPT–S J041839–4751.9 is strongly gravitationally lensed by a foreground galaxy at z = 0.263, and it is a typical dusty starburst, with global star-forming7 and dust properties8 that are in agreement with current numerical simulations9 and observations10. Interferometric imaging at a spatial resolution of about 60 parsecs reveals a ratio of rotational to random motions of 9.7 ± 0.4, which is at least four times larger than that expected from any galaxy evolution model at this epoch1–5 but similar to the ratios of spiral galaxies in the local Universe11. We derive a rotation curve with the typical shape of nearby massive spiral galaxies, which demonstrates that at least some young galaxies are dynamically akin to those observed in the local Universe, and only weakly affected by extreme physical processes.}, -archivePrefix = {arXiv}, -arxivId = {2009.01251}, -author = {Rizzo, F. and Vegetti, S. and Powell, D. and Fraternali, F. and McKean, J. P. and Stacey, H. R. and White, S. D.M.}, -doi = {10.1038/s41586-020-2572-6}, -eprint = {2009.01251}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Rizzo2020DSFGNature.pdf:pdf}, -issn = {14764687}, -journal = {Nature}, -number = {7820}, -pages = {201--204}, -pmid = {32788739}, -title = {{A dynamically cold disk galaxy in the early Universe}}, -volume = {584}, -year = {2020} -} -@article{Hezaveh2013b, -abstract = {We present Atacama Large Millimeter/submillimeter Array (ALMA) 860 $\mu$m imaging of four high-redshift (z = 2.8-5.7) dusty sources that were detected using the South Pole Telescope (SPT) at 1.4 mm and are not seen in existing radio to far-infrared catalogs. At 1.″5 resolution, the ALMA data reveal multiple images of each submillimeter source, separated by 1″-3″, consistent with strong lensing by intervening galaxies visible in near-IR imaging of these sources. We describe a gravitational lens modeling procedure that operates on the measured visibilities and incorporates self-calibration- like antenna phase corrections as part of the model optimization, which we use to interpret the source structure. Lens models indicate that SPT0346-52, located at z = 5.7, is one of the most luminous and intensely star-forming sources in the universe with a lensing corrected FIR luminosity of 3.7 × 10 13 L and star formation surface density of 4200 M⊙yr -1 kpc-2. We find magnification factors of 5 to 22, with lens Einstein radii of 1.″1-2.″0 and Einstein enclosed masses of 1.6-7.2 × 1011 M⊙. These observations confirm the lensing origin of these objects, allow us to measure their intrinsic sizes and luminosities, and demonstrate the important role that ALMA will play in the interpretation of lensed submillimeter sources. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1303.2722}, -author = {Hezaveh, Y. D. and Marrone, D. P. and Fassnacht, C. D. and Spilker, J. S. and Vieira, J. D. and Aguirre, J. E. and Aird, K. A. and Aravena, M. and Ashby, M. L.N. and Bayliss, M. and Benson, B. A. and Bleem, L. E. and Bothwell, M. and Brodwin, M. and Carlstrom, J. E. and Chang, C. L. and Chapman, S. C. and Crawford, T. M. and Crites, A. T. and {De Breuck}, C. and {De Haan}, T. and Dobbs, M. A. and Fomalont, E. B. and George, E. M. and Gladders, M. D. and Gonzalez, A. H. and Greve, T. R. and Halverson, N. W. and High, F. W. and Holder, G. P. and Holzapfel, W. L. and Hoover, S. and Hrubes, J. D. and Husband, K. and Hunter, T. R. and Keisler, R. and Lee, A. T. and Leitch, E. M. and Lueker, M. and Luong-Van, D. and Malkan, M. and McIntyre, V. and McMahon, J. J. and Mehl, J. and Menten, K. M. and Meyer, S. S. and Mocanu, L. M. and Murphy, E. J. and Natoli, T. and Padin, S. and Plagge, T. and Reichardt, C. L. and Rest, A. and Ruel, J. and Ruhl, J. E. and Sharon, K. and Schaffer, K. K. and Shaw, L. and Shirokoff, E. and Stalder, B. and Staniszewski, Z. and Stark, A. A. and Story, K. and Vanderlinde, K. and Wei{\ss}, A. and Welikala, N. and Williamson, R.}, -doi = {10.1088/0004-637X/767/2/132}, -eprint = {1303.2722}, -issn = {15384357}, -journal = {ApJ}, -keywords = {galaxies: high-redshift,galaxies: starburst,gravitational lensing: strong,techniques: interferometric}, -month = {apr}, -number = {2}, -pages = {132}, -pmid = {20052985}, -title = {{Alma observations of spt-discovered, strongly lensed, dusty, star-forming galaxies}}, -url = {http://stacks.iop.org/0004-637X/767/i=2/a=132?key=crossref.b61d251fa2ccc38744f6e3bbdb7c5879}, -volume = {767}, -year = {2013} -} -@article{OrbandeXivry2008, -abstract = {Wide-field optical imaging surveys will contain tens of thousands of new strong gravitational lenses. Some of these will have new and unusual image configurations, and so will enable new applications: for example, systems with high image multiplicity will allow more detailed study of galaxy and group mass distributions, while high magnification is needed to super-resolve the faintest objects in the high-redshift universe. Inspired by a set of six unusual lens systems [including five selected from the Sloan Lens ACS survey (SLACS) and Strong Lens Legacy Survey (SL2S), plus the cluster Abell 1703], we consider several types of multi-component, physically motivated lens potentials, and use the ray-tracing code glamroc to predict exotic image configurations. We also investigate the effects of galaxy source profile and size, and use realistic sources to predict observable magnifications and estimate very approximate relative cross-sections. We find that lens galaxies with misaligned discs and bulges produce swallowtail and butterfly catastrophes, observable as 'broken' Einstein rings. Binary or merging galaxies show elliptic umbilic catastrophes, leading to an unusual Y-shaped configuration of four merging images. While not the maximum magnification configuration possible, it offers the possibility of mapping the local small-scale mass distribution. We estimate the approximate abundance of each of these exotic galaxy-scale lenses to be ∼1 per all-sky survey. In higher mass systems, a wide range of caustic structures are expected, as already seen in many cluster lens systems. We interpret the central ring and its counter-image in Abell 1703 as a 'hyperbolic umbilic' configuration, with total magnification ∼100 (depending on source size). The abundance of such configurations is also estimated to be ∼1 per all-sky survey {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0904.1454}, -author = {{Orban De Xivry}, Gilles and Marshall, Phil}, -doi = {10.1111/j.1365-2966.2009.14925.x}, -eprint = {0904.1454}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Orban De Xivry, Marshall - 2009 - An atlas of predicted exotic gravitational lenses(2).pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Gravitational lensing,Surveys}, -number = {1}, -pages = {2--20}, -title = {{An atlas of predicted exotic gravitational lenses}}, -volume = {399}, -year = {2009} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of stellar parameters and abundances ("stellar labels") for hundreds of thousands of stars; this poses a formidable spectral modeling challenge. In many cases, there is a subset of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the "known" labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with and as the labels, and then applying it to the spectra of 55,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one-ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ness, M and Hogg, David W and Rix, H W and Ho, Anna Y Q and Zasowski, G}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{THE CANNON: A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION}}, -volume = {808}, -year = {2015} -} -@inproceedings{Goudfrooij2003, -author = {Goudfrooij, P and Kimble, R.$\sim$A.}, -booktitle = {HST Calibration Workshop : Hubble after the Installation of the ACS and the NICMOS Cooling System}, -editor = {Arribas, S and Koekemoer, A and Whitmore, B}, -pages = {105}, -title = {{Correcting STIS CCD Photometry for CTE Loss}}, -year = {2003} -} -@article{Xie:2015aa, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P. and Frenk, Carlos S. and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xie et al. - 2015 - The size evolution of elliptical galaxies(3).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -month = {feb}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Sonnenfeld2012, -abstract = {Stars and dark matter account for most of the mass of early-type galaxies, but uncertainties in the stellar population and the dark matter profile make it challenging to distinguish between the two components. Nevertheless, precise observations of stellar and dark matter are extremely valuable for testing the many models of structure formation and evolution. We present a measurement of the stellar mass and inner slope of the dark matter halo of a massive early-type galaxy at z = 0.222. The galaxy is the foreground deflector of the double Einstein ring gravitational lens system SDSSJ0946+1006, also known as the "Jackpot." By combining the tools of lensing and dynamics we first constrain the mean slope of the total mass density profile () within the radius of the outer ring to be $\gamma$′ = 1.98 ± 0.02 ± 0.01. Then we obtain a bulge-halo decomposition, assuming a power-law form for the dark matter halo. Our analysis yields $\gamma$DM = 1.7 ± 0.2 for the inner slope of the dark matter profile, in agreement with theoretical findings on the distribution of dark matter in ellipticals, and a stellar mass from lensing and dynamics M LD* = 5.5-1.3+0.4 × 1011 M. By comparing this measurement with stellar masses inferred from stellar population synthesis fitting we find that a Salpeter initial mass function (IMF) provides a good description of the stellar population of the lens while the probability of the IMF being heavier than Chabrier is 95%. Our data suggest that growth by accretion of small systems from a compact red nugget is a plausible formation scenario for this object. {\textcopyright} 2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1111.4215}, -author = {Sonnenfeld, A. and Treu, T. and Gavazzi, R. and Marshall, P. J. and Auger, M. W. and Suyu, S. H. and Koopmans, L. V.E. and Bolton, A. S.}, -doi = {10.1088/0004-637X/752/2/163}, -eprint = {1111.4215}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: structure,gravitational lensing: strong}, -number = {2}, -pages = {163}, -title = {{Evidence for dark matter contraction and a salpeter initial mass function in a massive early-type galaxy}}, -url = {http://stacks.iop.org/0004-637X/752/i=2/a=163?key=crossref.201aa76030fad6de9fcb9bcdea5b05d1}, -volume = {752}, -year = {2012} -} -@article{Kennicutt, -abstract = {We review progress over the past decade in observations of large-scale star formation, with a focus on the interface between extragalactic and Galactic studies. Methods of measuring gas contents and star formation rates are discussed, and updated prescriptions for calculating star formation rates are provided. We review relations between star formation and gas on scales ranging from entire galaxies to individual molecular clouds.}, -archivePrefix = {arXiv}, -arxivId = {1204.3552}, -author = {Kennicutt, Robert C and Evans, Neal J}, -doi = {10.1146/annurev-astro-081811-125610}, -eprint = {1204.3552}, -issn = {0066-4146}, -journal = {Annual Review of Astronomy and Astrophysics}, -number = {1}, -pages = {531--608}, -title = {{Star Formation in the Milky Way and Nearby Galaxies}}, -url = {http://arxiv.org/abs/1204.3552%7B%5C%25%7D0Ahttp://dx.doi.org/10.1146/annurev-astro-081811-125610}, -volume = {50}, -year = {2012} -} -@article{Cole:2000aa, -abstract = {We describe the GALFORM semi-analytic model for calculating the formation and evolution of galaxies in hierarchical models. It improves upon, and extends, the Cole et al 1994 model. The model employs a new Monte-Carlo algorithm to follow the merging evolution of dark matter halos with arbitrary mass resolution. It incorporates realistic descriptions of the density profiles of dark matter halos and their gas content; follows the chemical evolution of gas and stars, and the associated production of dust; and includes a detailed calculation of the sizes of disks and spheroids. Wherever possible, our prescriptions for modelling individual physical processes are based on results of numerical simulations. We apply our methods to the LCDM cosmology (Omega{\_}0=0.3, Lambda{\_}0=0.7), and find good agreement with a wide range of properties of the local galaxy population: the B-band and K-band luminosity functions, the distribution of colours for the population as a whole, the ratio of ellipticals to spirals, the distribution of disk sizes, and the current cold gas content of disks. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0007281}, -author = {Cole, Shaun and Lacey, Cedric G and Baugh, Carlton M and Frenk, Carlos S}, -doi = {10.1046/j.1365-8711.2000.03879.x}, -eprint = {0007281}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -month = {nov}, -number = {1}, -pages = {168--204}, -primaryClass = {astro-ph}, -title = {{Hierarchical galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0007281%7B%5C%25%7D0Ahttp://dx.doi.org/10.1046/j.1365-8711.2000.03879.x}, -volume = {319}, -year = {2002} -} -@article{Sonnenfeld2015, -abstract = {We investigate the cosmic evolution of the internal structure of massive early-type galaxies over half of the age of the universe. We perform a joint lensing and stellar dynamics analysis of a sample of 81 strong lenses from the Strong Lensing Legacy Survey and Sloan ACS Lens Survey and combine the results with a hierarchical Bayesian inference method to measure the distribution of dark matter mass and stellar initial mass function (IMF) across the population of massive early-type galaxies. Lensing selection effects are taken into account. We find that the dark matter mass projected within the inner 5 kpc increases for increasing redshift, decreases for increasing stellar mass density, but is roughly constant along the evolutionary tracks of early-type galaxies. The average dark matter slope is consistent with that of a Navarro-Frenk-White profile, but is not well constrained. The stellar IMF normalization is close to a Salpeter IMF at log M ∗ = 11.5 and scales strongly with increasing stellar mass. No dependence of the IMF on redshift or stellar mass density is detected. The anti-correlation between dark matter mass and stellar mass density supports the idea of mergers being more frequent in more massive dark matter halos.}, -archivePrefix = {arXiv}, -arxivId = {1410.1881}, -author = {Sonnenfeld, Alessandro and Treu, Tommaso and Marshall, Philip J. and Suyu, Sherry H. and Gavazzi, Rapha{\"{e}}l and Auger, Matthew W. and Nipoti, Carlo}, -doi = {10.1088/0004-637X/800/2/94}, -eprint = {1410.1881}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,gravitational lensing: strong}, -number = {2}, -pages = {94}, -title = {{The sl2s galaxy-scale lens sample. V. Dark matter halos and stellar imf of massive early-type galaxies out to redshift 0.8}}, -url = {http://arxiv.org/abs/1410.1881}, -volume = {800}, -year = {2015} -} -@article{Tian2017, -abstract = {We study the Mass Discrepancy-Acceleration Relation (MDAR) of 57 elliptical galaxies by their Einstein rings from the Sloan Lens ACS Survey (SLACS). This is the first time that the MDAR is discussed with data from gravitational lensing, a relativistic effect. The mass discrepancy between the lensing mass and the baryonic mass derived from population synthesis is larger when the acceleration of the elliptical galaxy lenses is smaller. The MDAR is also related to surface mass density discrepancy. At the Einstein ring, these lenses belong to high-surface-mass density galaxies. Similarly, we find that the discrepancy between the lensing and stellar surface mass density is small. It is consistent with the recent discovery of dynamical surface mass density discrepancy in disk galaxies where the discrepancy is smaller when surface density is larger. We also find relativistic modified Newtonian dynamics (MOND) can naturally explain the MDAR and surface mass density discrepancy in 57 Einstein rings. Moreover, the lensing mass, the dynamical mass and the stellar mass of these galaxies are consistent with each other in relativistic MOND.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1702.00183}, -author = {Tian, Yong and Ko, Chung Ming}, -doi = {10.1093/MNRAS/STX2056}, -eprint = {1702.00183}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: kinematics and dynamics,Dark matter,Galaxies: elliptical and lenticular,Gravitation,Gravitational lensing: strong}, -number = {1}, -pages = {765--771}, -title = {{Mass discrepancy-acceleration relation in Einstein rings}}, -url = {http://arxiv.org/abs/1702.00183}, -volume = {472}, -year = {2017} -} -@article{Rhodes2007, -abstract = {We examine the spatial and temporal stability of the Hubble Space Telescope's Advanced Camera for Surveys (ACS) Wide Field Camera (WFC) point-spread function (PSF) using the 2 deg2 COSMOS survey. This is important for studies of weak gravitational lensing, where the ability to deconvolve the PSF from galaxy shapes is of paramount importance. We show that stochastic aliasing of the PSF necessarily occurs during ``drizzling.'' This aliasing is maximal if the output-pixel scale is equal to the input-pixel scale. This source of PSF variation can be significantly reduced by choosing a Gaussian drizzle kernel with a size of 0.8 input pixels and by reducing the output-pixel scale. We show that the PSF is temporally unstable, resulting in an overall slow periodic focus change in the COSMOS images. Using a modified version of the Tiny Tim PSF modeling software, we create grids of undistorted stars over a range of telescope focus values. We then use the approximately 10 well-measured stars in each COSMOS field to pick the best-fit focus value for each field. The Tiny Tim model stars can then be used to perform PSF corrections for weak lensing. We derive a parametric correction for the effect of charge transfer efficiency (CTE) degradation on the shapes of objects in the COSMOS field as a function of observation date, position within the ACS WFC field, and object flux. Finally, we discuss future plans to improve the CTE correction. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555 also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0702140}, -author = {Rhodes, Jason D. and Massey, Richard J. and Albert, Justin and Collins, Nicholas and Ellis, Richard S. and Heymans, Catherine and Gardner, Jonathan P. and Kneib, Jean‐Paul and Koekemoer, Anton and Leauthaud, Alexie and Mellier, Yannick and Refregier, Alexander and Taylor, James E. and {Van Waerbeke}, Ludovic}, -doi = {10.1086/516592}, -eprint = {0702140}, -issn = {0067-0049}, -journal = {The Astrophysical Journal Supplement Series}, -keywords = {Instrumentation: Detectors,Surveys,Techniques: Image Processing}, -month = {sep}, -number = {1}, -pages = {203--218}, -primaryClass = {astro-ph}, -title = {{ The Stability of the Point‐Spread Function of the Advanced Camera for Surveys on the Hubble Space Telescope and Implications for Weak Gravitational Lensing }}, -url = {http://stacks.iop.org/0067-0049/172/i=1/a=203}, -volume = {172}, -year = {2007} -} -@article{Cautun2015, -abstract = {The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model ($\Lambda$ cold dark matter - $\Lambda$CDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of theMWand M31 planes in $\Lambda$CDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high-resolution cosmological simulations. We find that planar structures are very common, and that $\sim$10 per cent of $\Lambda$CDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small-scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and $\Lambda$CDM predictions. In fact, $\sim$10 per cent of $\Lambda$CDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1506.04151}, -author = {Cautun, Marius and Bose, Sownak and Frenk, Carlos S. and Guo, Qi and Han, Jiaxin and Hellwing, Wojciech A. and Sawala, Till and Wang, Wenting}, -doi = {10.1093/mnras/stv1557}, -eprint = {1506.04151}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cautun et al. - 2015 - Planes of satellite galaxies When exceptions are the rule(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {4}, -pages = {3838--3852}, -title = {{Planes of satellite galaxies: When exceptions are the rule}}, -volume = {452}, -year = {2015} -} -@article{Kochanek2004b, -abstract = {The flux anomalies in four-image gravitational lenses can be interpreted as evidence for the dark matter substructure predicted by cold dark matter (CDM) halo models. In principle, these flux anomalies could arise from alternate sources, such as absorption, scattering, or scintillation by the interstellar medium (ISM) of the lens galaxy, problems in the ellipsoidal macro models used to fit lens systems, or stellar microlensing. We apply several tests to the data that appear to rule out these alternate explanations. First, the radio flux anomalies show no significant dependence on wavelength, as would be expected for almost any propagation effect in the ISM or microlensing by the stars. Second, the flux anomaly distributions show the characteristic demagnifications of the brightest saddle point relative to the other images expected for low optical depth substructure, which cannot be mimicked by either the ISM or problems in the macro models. Microlensing by stars also cannot reproduce the suppression of the bright saddle points if the radio source sizes are consistent with the Compton limit for their angular sizes. Third, while it is possible to change the smooth lens models to fit the flux anomalies in some systems, we can rule out the necessary changes in all systems where we have additional lens constraints to check the models. Moreover, the parameters of these models are inconsistent with our present observations and expectations for the structure of galaxies. We conclude that low-mass halos remain the best explanation of the phenomenon.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0302036}, -author = {Kochanek, C. S. and Dalal, N.}, -doi = {10.1086/421436}, -eprint = {0302036}, -isbn = {3134843099}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Gravitational Lensing,Galaxies: Halos}, -month = {jul}, -number = {1}, -pages = {69--79}, -primaryClass = {astro-ph}, -title = {{Tests for Substructure in Gravitational Lenses}}, -url = {http://stacks.iop.org/0004-637X/610/i=1/a=69}, -volume = {610}, -year = {2004} -} -@article{Algorry2016, -abstract = {We examine the properties of barred disc galaxies in a LCDM cosmological hydrodynamical simulation from the EAGLE project. Our study follows the formation of 269 discs identified at z = 0 in the stellar mass range 10.6 {\textless}log Mstr /M {\textless}11. These discs show a wide range of bar strengths, from unbarred discs to weak bars to strongly barred systems (= 20{\%}). Bars in these systems develop after redshift = 1.3, on timescales that depend sen- sitively on the strength of the pattern. Strong bars develop relatively quickly (in a few Gyr, = 10 disc rotation periods) in systems that are disc dominated, gas poor, and have declining rotation curves. Weak bars develop more slowly in systems where the disc is less gravitation- ally important, and are still growing at z = 0. Unbarred galaxies are comparatively gas-rich discs whose rotation speeds do not exceed the maximum circular velocity of the halos they inhabit. Bar lengths compare favourably with observations, ranging from 0.2 to 0.8 times the radius containing 90{\%} of the stars. Bars slow down remarkably quickly as they grow, causing the inner regions of the surrounding dark halo to expand. At z = 0 strong bars have corota- tion radii roughly ten times the bar length. Such slow bars are inconsistent with the few cases where pattern speeds have been measured or inferred observationally, a discrepancy that, if confirmed, might prove a challenge for disc galaxy formation in LCDM.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1609.05909}, -author = {Algorry, David G and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Vecchia, Claudio Dalla and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx1008}, -eprint = {1609.05909}, -keywords = {disc,formation,galaxies,galaxy,kinematics and dynamics}, -number = {September}, -pages = {1--11}, -title = {{Barred galaxies in the EAGLE cosmological hydrodynamical simulation}}, -url = {http://arxiv.org/abs/1609.05909%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1008}, -volume = {11}, -year = {2016} -} -@article{Hopkins2011b, -abstract = {Feedback from massive stars is believed to play a critical role in shaping the galaxy mass function, the structure of the interstellar medium (ISM) and the low efficiency of star formation, but the exact form of the feedback is uncertain. In this paper, the first in a series, we present and test a novel numerical implementation of stellar feedback resulting from momentum imparted to the ISM by radiation, supernovae and stellar winds. We employ a realistic cooling function, and find that a large fraction of the gas cools to ≲100K, so that the ISM becomes highly inhomogeneous. Despite this, our simulated galaxies reach an approximate steady state, in which gas gravitationally collapses to form giant 'molecular' clouds (GMCs), dense clumps and stars; subsequently, stellar feedback disperses the GMCs, repopulating the diffuse ISM. This collapse and dispersal cycle is seen in models of Small Magellanic Cloud (SMC)-like dwarfs, the Milky Way and z{\$\sim${}} 2 clumpy disc analogues. The simulated global star formation efficiencies are consistent with the observed Kennicutt-Schmidt relation. Moreover, the star formation rates are nearly independent of the numerically imposed high-density star formation efficiency, density threshold and density scaling. This is a consequence of the fact that, in our simulations, star formation is regulated by stellar feedback limiting the amount of very dense gas available for forming stars. In contrast, in simulations without stellar feedback, i.e. under the action of only gravity and gravitationally induced turbulence, the ISM experiences runaway collapse to very high densities. In these simulations without feedback, the global star formation rates exceed observed galactic star formation rates by 1-2 orders of magnitude, demonstrating that stellar feedback is crucial to the regulation of star formation in galaxies. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1101.4940}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2011.19306.x}, -eprint = {1101.4940}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation}, -number = {2}, -pages = {950--973}, -title = {{Self-regulated star formation in galaxies via momentum input from massive stars}}, -volume = {417}, -year = {2011} -} -@article{Jin2017, -abstract = {We report the results from a recent 133 ks XMM-Newton observation of a highly super-Eddington narrow-line Type-1 QSO RX J0439.6-5311. This source has one of the steepest AGN hard X-ray slopes, in addition to a prominent and smooth soft X-ray excess. Strong variations are found throughout the 0.3 to 10 keV energy range on all time-scales covered by the observation, with the soft excess mainly showing low frequency variations below 0.1 mHz while the hard X-rays show stronger variability at higher frequencies. We perform a full set of spectral-timing analysis on the X-ray data, including a simultaneous modelling of the time-average spectra, frequency-dependent RMS and covariance spectra, lag-frequency and lag-energy spectra. Especially, we find a significant time-lag signal in the low frequency band, which indicates that the soft X-rays lead the hard by {\$}\backslashsim{\$}4 ks, with a broad continuum-like profile in the lag spectrum. Our analysis strongly supports the model where the soft X-ray excess is dominated by a separate low temperature, optically thick Comptonisation component rather than relativistic reflection or a jet. This soft X-ray emitting region is several tens or hundreds of {\$}R{\_}{\{}g{\}}{\$} away from the hot corona emitting hard X-rays, and is probably associated with a geometrically thick (`puffed-up') inner disc region.}, -archivePrefix = {arXiv}, -arxivId = {1703.07118}, -author = {Jin, Chichuan and Done, Chris and Ward, Martin}, -doi = {10.1093/mnras/stx718}, -eprint = {1703.07118}, -issn = {0035-8711}, -keywords = {accretion,accretion discs - galaxies,active - galaxies,nuclei}, -number = {June}, -pages = {1--17}, -title = {{Super-Eddington QSO RX J0439.6-5311. I. Origin of the Soft X-ray Excess and Structure of the Inner Accretion Flow}}, -url = {http://arxiv.org/abs/1703.07118%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx718}, -volume = {17}, -year = {2017} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ {\textgreater} 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright}2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{Bullock2005a, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past {\$\sim${}}12 Gyr. We model this process using a hybrid semianalytic plus N-body approach that distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our accreted stellar halos have density profiles that typically drop off with radius faster than the dark matter and follow power laws at r{\textgreater}{\$\sim${}}30 kpc with {\$}\rho{\$}{\$\sim${}}r-{\$}\alpha{\$}, {\$}\alpha{\$}{\$\sim${}}=3-4. They are well fit by Hernquist profiles over the full radial range. We find that stellar halos are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the {\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase-space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print){\$}\backslash{\$}r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://stacks.iop.org/0004-637X/635/i=2/a=931}, -volume = {635}, -year = {2005} -} -@article{Oh2011, -abstract = {We make a direct comparison of the derived dark matter (DM) distributions between hydrodynamical simulations of dwarf galaxies assuming a $\Lambda$CDM cosmology and the observed dwarf galaxies sample from the THINGS survey in terms of (1) the rotation curve shape and (2) the logarithmic inner density slope $\alpha$ of mass density profiles. The simulations, which include the effect of baryonic feedback processes, such as gas cooling, star formation, cosmic UV background heating, and most importantly, physically motivated gas outflows driven by supernovae, form bulgeless galaxies with DM cores. We show that the stellar and baryonic mass is similar to that inferred from photometric and kinematic methods for galaxies of similar circular velocity. Analyzing the simulations in exactly the same way as the observational sample allows us to address directly the so-called cusp/core problem in the $\Lambda$CDM model. We show that the rotation curves of the simulated dwarf galaxies rise less steeply than cold dark matter rotation curves and are consistent with those of the THINGS dwarf galaxies. The mean value of the logarithmic inner density slopes $\alpha$ of the simulated galaxies' DM density profiles is ∼-0.4 ± 0.1, which shows good agreement with $\alpha$ = -0.29 ± 0.07 of the THINGS dwarf galaxies. The effect of non-circular motions is not significant enough to affect the results. This confirms that the baryonic feedback processes included in the simulations are efficiently able to make the initial cusps with $\alpha$ ∼ -1.0 to -1.5 predicted by DM-only simulations shallower and induce DM halos with a central mass distribution similar to that observed in nearby dwarf galaxies. {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1011.2777}, -author = {Oh, Se Heon and Brook, Chris and Governato, Fabio and Brinks, Elias and Mayer, Lucio and {De Blok}, W. J.G. and Brooks, Alyson and Walter, Fabian}, -doi = {10.1088/0004-6256/142/1/24}, -eprint = {1011.2777}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {dark matter,galaxies: dwarf,galaxies: halos,galaxies: kinematics and dynamics}, -month = {jul}, -number = {1}, -pages = {24}, -title = {{The central slope of dark matter cores in dwarf galaxies: Simulations versus things}}, -url = {http://stacks.iop.org/1538-3881/142/i=1/a=24?key=crossref.7392fede3277be6798bcdb117e463ba0}, -volume = {142}, -year = {2011} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, $\sigma$(R), for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude MK {\textless} -25.3mag, or stellar mass M* ≳ 4 × 1011M⊙, within 108 Mpc. Our wide-field 107 arcsec × 107 arcsec IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes $\gamma$ inner and $\gamma$ outer of s(R). While $\gamma$ inner is mostly negative, of the 56 galaxies with sufficient radial coverage to determine $\gamma$ outer we find 36 per cent to have rising outer dispersion profiles, 30 per cent to be flat within the uncertainties and 34 per cent to be falling. The fraction of galaxies with rising outer profiles increases with M* and in denser galaxy environment, with 10 of the 11 most massive galaxies in our sample having flat or rising dispersion profiles. The strongest environmental correlations are with local density and halo mass, but a weaker correlation with large-scale density also exists. The average $\gamma$ outer is similar for brightest group galaxies, satellites and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis h4. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{DeLucia2005, -abstract = {We take advantage of the largest high-resolution simulation of cosmic structure growth ever carried out - the Millennium Simulation of the concordance $\Lambda$ cold dark matter (CDM) cosmogony - to study how the star formation histories, ages and metallicities of elliptical galaxies depend on environment and on stellar mass. We concentrate on a galaxy formation model which is tuned to fit the joint luminositycolourmorphology distribution of low-redshift galaxies. Massive ellipticals in this model have higher metal abundances, older luminosity-weighted ages and shorter star formation time-scales, but lower assembly redshifts, than less massive systems. Within clusters the typical masses, ages and metal abundances of ellipticals are predicted to decrease, on average, with increasing distance from the cluster centre. We also quantify the effective number of progenitors of ellipticals as a function of present stellar mass, finding typical numbers below two for , rising to approximately five for the most massive systems. These findings are consistent with recent observational results that suggest 'down-sizing' or 'antihierarchical' behaviour for the star formation history of the elliptical galaxy population, despite the fact that our model includes all the standard elements of hierarchical galaxy formation and is implemented on the standard, $\Lambda$CDM cosmogony. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0509725}, -author = {{De Lucia}, Gabriella and Springel, Volker and White, Simon D.M. and Croton, Darren and Kauffmann, Guinevere}, -doi = {10.1111/j.1365-2966.2005.09879.x}, -eprint = {0509725}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/De Lucia et al. - 2006 - The formation history of elliptical galaxies.pdf:pdf}, -isbn = {1535-4970}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content}, -number = {2}, -pages = {499--509}, -pmid = {19910610}, -primaryClass = {astro-ph}, -title = {{The formation history of elliptical galaxies}}, -url = {http://arxiv.org/abs/astro-ph/0509725%0Ahttp://dx.doi.org/10.1111/j.1365-2966.2005.09879.x}, -volume = {366}, -year = {2006} -} -@article{Wood2014, -abstract = {The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D and Hall, D J and Murray, N J and Gow, J P D and Holland, A and Turner, P and Burt, D}, -doi = {10.1088/1748-0221/9/12/C12028}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv,visible and ir photons (s}, -number = {12}, -pages = {C12028--------C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{Sonnenfeld2018, -abstract = {The initial mass function (IMF) for massive galaxies can be constrained by combining stellar dynamics with strong gravitational lensing. However, this method is limited by degeneracies between the density profile of dark matter and the stellar mass-to-light ratio (M/L). In this work, we reduce this degeneracy by combining weak lensing together with strong lensing and stellar kinematics. Our analysis is based on two galaxy samples: 45 strong lenses from the SLACS survey and 1700 massive quiescent galaxies from the Sloan Digital Sky Survey main spectroscopic sample with weak lensing measurements from the Hyper Suprime-Cam survey. We use a Bayesian hierarchical approach to jointly model all three observables. We fit the data with models of varying complexity and show that a model with a radial gradient in the stellar M/L is required to simultaneously describe both galaxy samples. This result is driven by a subset of strong lenses with very steep total density profile that cannot be fitted by models with no gradient. Our measurements are unable to determine whether M*/L gradients are due to variations in stellar population parameters at fixed IMF, or to gradients in the IMF itself. The inclusion of M*/L gradients decreases dramatically the inferred IMF normalization, compared to previous lensing-based studies, with the exact value depending on the assumed dark matter profile. The main effect of strong lensing selection is to shift the stellar mass distribution towards the high-mass end, while the halo mass and stellar IMF distribution at fixed stellar mass are not significantly affected.}, -archivePrefix = {arXiv}, -arxivId = {1801.01883}, -author = {Sonnenfeld, Alessandro and Leauthaud, Alexie and Auger, Matthew W. and Gavazzi, Raphael and Treu, Tommaso and More, Surhud and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty2262}, -eprint = {1801.01883}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sonnenfeld et al. - 2018 - Evidence for radial variations in the stellar mass-to-light ratio of massive galaxies from weak and strong(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {CD- gravitational lensing: strong,Galaxies: elliptical and lenticular,Gravitational lensing: weak}, -number = {1}, -pages = {164--184}, -title = {{Evidence for radial variations in the stellar mass-to-light ratio of massive galaxies from weak and strong lensing}}, -volume = {481}, -year = {2018} -} -@article{Ferreras2019, -abstract = {We study the internal radial gradients of the stellar populations in a sample comprising 522 early-type galaxies (ETGs) from the SAMI (Sydney-AAO Multi-object Integral field spectrograph) Galaxy Survey. We stack the spectra of individual spaxels in radial bins, and derive basic stellar population properties: total metallicity ([Z/H]), [Mg/Fe], [C/Fe] and age. The radial gradient (∇) and central value of the fits (evaluated at Re/4) are compared against a set of six observables that may act as drivers of the trends. We find that velocity dispersion ($\sigma$) - or, equivalently gravitational potential - is the dominant driver of the chemical composition gradients. Surface mass density is also correlated with the trends, especially with stellar age. The decrease of ∇[Mg/Fe] with increasing $\sigma$ is contrasted by a rather shallow dependence of ∇[Z/H] with $\sigma$ (although this radial gradient is overall rather steep). This result, along with a shallow age slope at the massive end, imposes a substantial constraint on the progenitors of the populations that contribute to the formation of the outer envelopes of ETGs. The SAMI sample is split, by design, between 'field' and cluster galaxies. Only weak environment-related differences are found, most notably a stronger dependence of central total metallicity ([Z/H]e4) with $\sigma$, along with a marginal trend of ∇[Z/H] to steepen in cluster galaxies, a result that is not followed by [Mg/Fe]. The results presented here serve as stringent constraints on numerical models of the formation and evolution of ETGs.}, -archivePrefix = {arXiv}, -arxivId = {1905.03257}, -author = {Ferreras, Ignacio and Scott, Nicholas and la Barbera, Francesco and Croom, Scott and van de Sande, Jesse and Hopkins, Andrew and Colless, Matthew and Barone, Tania M. and D'Eugenio, Francesco and Bland-Hawthorn, Joss and Brough, Sarah and Bryant, Julia J. and Konstantopoulos, Iraklis S. and Lagos, Claudia and Lawrence, Jon S. and L{\'{o}}pez-S{\'{a}}nchez, Angel and Medling, Anne M. and Owers, Matt S. and Richards, Samuel N.}, -doi = {10.1093/mnras/stz2095}, -eprint = {1905.03257}, -file = {:C\:/Users/Jammy/Documents/Papers/Ferraras2019SAMIRadialGradientETG.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content}, -number = {1}, -pages = {608--622}, -title = {{The SAMI galaxy survey: Stellar population radial gradients in early-type galaxies}}, -volume = {489}, -year = {2019} -} -@article{Chirivi2017, -abstract = {Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we aim to present the first attempt at modelling line-of-sight (LOS) mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We have focussed on the Hubble Frontier Field cluster MACS J0416.1-2403, and our multi-plane model reproduces the observed image positions with a rms offset of $\sim$0.′′53. Starting from this best-fitting model, we simulated a mock cluster that resembles MACS J0416.1-2403 in order to explore the effects of LOS structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms $\sim$0.′′3); accounting for LOS galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factor of the lensed multiple images are recovered within $\sim$10% for $\sim$95% of them, those $\sim$5% that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models. In addition, LOS galaxies cannot explain the apparent discrepancy in the properties of massive sub-halos between MACS J0416.1-2403 and N-body simulated clusters. Since our model of MACS J0416.1-2403 with LOS galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities would be needed in future models of MACS J0416.1-2403.}, -archivePrefix = {arXiv}, -arxivId = {1706.07815}, -author = {Chiriv{\`{i}}, G. and Suyu, S. H. and Grillo, C. and Halkola, A. and Balestra, I. and Caminha, G. B. and Mercurio, A. and Rosati, P.}, -doi = {10.1051/0004-6361/201731433}, -eprint = {1706.07815}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Chiriv{\`{i}} et al. - 2018 - MACS J0416.1-2403 Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy cluster.pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Dark matter,Galaxies: clusters: general,Galaxies: clusters: individual: MACS J0416.1-2403,Gravitational lensing: strong}, -pages = {1--29}, -title = {{MACS J0416.1-2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters}}, -url = {http://arxiv.org/abs/1706.07815%0Ahttp://dx.doi.org/10.1051/0004-6361/201731433}, -volume = {614}, -year = {2018} -} -@article{Crowley2016, -abstract = {Since the launch of ESA's Gaia satellite in December 2013, the 106 large-format scientific CCDs onboard have been operating at L2. Due to a combination of the high-precision measurement requirements of the mission and the predicted proton environment at L2, the effect of non-ionizing radiation damage on the detectors was early identified pre-launch as potentially imposing a major limitation on the scientific value of the data. In this paper we compare pre-flight radiation-induced Charge Transfer Inefficiency (CTI) predictions against in-flight measurements, focusing especially on charge injection diagnostics, as well as correlating these CTI diagnostic results with solar proton event data. We show that L2-directed solar activity has been relatively low since launch, and radiation damage (so far) is less than originally expected. Despite this, there are clear cases of correlation between earth-directed solar coronal mass ejection events and abrupt changes in CTI diagnostics over time. These sudden jumps are lying on top of a rather constant increase in CTI which we show is primarily due to the continuous bombardment of the devices by high-energy Galactic Cosmic Rays. We examine the possible reasons for the lower than expected levels of CTI as well as examining the effect of controlled payload heating events on the CTI diagnostics. Radiation-induced CTI in the CCD serial registers and effects of ionizing radiation are also correspondingly lower than expected, however these topics are not examined here in detail.}, -archivePrefix = {arXiv}, -arxivId = {1608.01476}, -author = {Crowley, Cian and Abreu, Asier and Kohley, Ralf and Prod'homme, Thibaut and Beaufort, Thierry}, -doi = {10.1117/12.2232078}, -eprint = {1608.01476}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Crowley et al. - 2016 - Radiation effects on the Gaia CCDs after 30 months at L2.pdf:pdf}, -isbn = {9781510602090}, -issn = {0277-786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -number = {July 2016}, -pages = {99150K}, -title = {{Radiation effects on the Gaia CCDs after 30 months at L2}}, -volume = {9915}, -year = {2016} -} -@article{Huang2018, -abstract = {We use {\$\sim${}}100 deg2 of deep ({\textgreater} 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach {\$\sim${}}4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) {\textgreater} 11.6 in more massive haloes at 0.3 {\textless} z {\textless} 0.5 have shallower inner stellar mass density profiles (within {\$\sim${}}10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) {\textgreater} 14.0 are {\$\sim${}}20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{2001et, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Lin2018, -abstract = {A Python non-uniform fast Fourier transform (PyNUFFT) package has been developed to accelerate multidimensional non-Cartesian image reconstruction on heterogeneous platforms. Since scientific computing with Python encompasses a mature and integrated environment, the time efficiency of the NUFFT algorithm has been a major obstacle to real-time non-Cartesian image reconstruction with Python. The current PyNUFFT software enables multi-dimensional NUFFT accelerated on a heterogeneous platform, which yields an efficient solution to many non-Cartesian imaging problems. The PyNUFFT also provides several solvers, including the conjugate gradient method, 1 total variation regularized ordinary least square (L1TV-OLS), and 1 total variation regularized least absolute deviation (L1TV-LAD). Metaprogramming libraries have been employed to accelerate PyNUFFT. The PyNUFFT package has been tested on multi-core central processing units (CPUs) and graphic processing units (GPUs), with acceleration factors of 6.3–9.5× on a 32-thread CPU platform and 5.4–13× on a GPU.}, -author = {Lin, Jyh Miin}, -doi = {10.3390/jimaging4030051}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lin - 2018 - Python non-uniform fast fourier transform (PyNUFFT) An accelerated non-cartesian MRI package on a heterogeneous platform (C.pdf:pdf}, -issn = {2313433X}, -journal = {Journal of Imaging}, -keywords = {Graphic processing unit (GPU),Heterogeneous system architecture (HSA),Magnetic resonance imaging (MRI),Multi-core system,Total variation (TV)}, -number = {3}, -pages = {1--22}, -title = {{Python non-uniform fast fourier transform (PyNUFFT): An accelerated non-cartesian MRI package on a heterogeneous platform (CPU/GPU)}}, -volume = {4}, -year = {2018} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{PASJEditionalOffice2015, -abstract = {We present the results from the Suzaku satellite of the surrounding region of a galaxy clus-ter, A2744, at z = 0.3. To search for oxygen emission lines from the warm-hot intergalactic medium (WHIM), we analyzed X-ray spectra from two northeast regions 2.2–3.3 and 3.3– 4.4 Mpc from the center of the cluster, which offers the first test on the presence of a WHIM near the typical accretion shock radius (∼ 2r 200) predicted by hydrodynamical simulations. For the 2.2–3.3 Mpc region, the spectral fit significantly (99.2% significance) improved when we include O VII and O VIII lines in the spectral model. A comparable WHIM surface bright-ness was obtained in the 3.3–4.4 Mpc region and the redshift of O VIII line is consistent with z = 0.3 within errors. The present results support that the observed soft X-ray emission orig-inated from the WHIM. However, considering both statistical and systematic uncertainties, O VIII detection in the northeast regions was marginal. The surface brightness of the O VIII line in 10 −7 photons cm −2 s −1 arcmin −2 was measured to be 2.7 ± 1.0, 2.1 ± 1.2 for the 2.2–3.3, 3.3– 4.4 Mpc regions, giving the upper limit on the baryon overdensity of $\delta$ = 319(< 443), 283(< 446), respectively. This is comparable with previous observations of cluster outskirts and their the-oretical predictions. The future prospect for WHIM detection using the Athena X-IFU micro-calorimeter is briefly discussed here. In addition, we also derived the ICM temperature distri-bution of A2744 to detect a clear discontinuity at the location of the radio relic. This suggests that the cluster has undergone strong shock heating by mass accretion along the filament.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1702.02157v1}, -author = {Hattori, Shiho and Ota, Naomi and Zhang, Yu-Ying and Akamatsu, Hiroki and Finoguenov, Alexis}, -doi = {10.1093/pasj/xxx000}, -eprint = {arXiv:1702.02157v1}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hattori et al. - 2014 - arXiv1702.02157v1 astro-ph.HE 7 Feb 2017.pdf:pdf}, -journal = {Publ. Astron. Soc. Japan}, -keywords = {clusters,cosmology,galaxies,individual (Abell 2744) — X-rays}, -number = {0}, -pages = {1--9}, -title = {{arXiv:1702.02157v1 [astro-ph.HE] 7 Feb 2017}}, -volume = {00}, -year = {2014} -} -@article{Hsu2018, -abstract = {We present a new framework to characterize the occurrence rates of planet candidates identified by Kepler based on hierarchical Bayesian modeling, Approximate Bayesian Computing (ABC), and sequential importance sampling. For this study we adopt a simple 2-D grid in planet radius and orbital period as our model and apply our algorithm to estimate occurrence rates for Q1-Q16 planet candidates orbiting around solar-type stars. We arrive at significantly increased planet occurrence rates for small planet candidates ({\$}R{\_}p{\textless}1.25 R{\_}{\{}\backslashbackslashoplus{\{}\backslash{\}}{\}}{\$}) at larger orbital periods ({\$}P{\textgreater}80{\$}d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is {\$}1.6{\^{}}{\{}+1.2{\}}{\_}{\{}-0.5{\}}{\$} per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2{\$}R{\_}{\{}\backslashbackslashoplus{\{}\backslash{\}}{\}}{\$} that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C and Ford, Eric B and Ragozzine, Darin and Morehead, Robert C}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -issn = {0004-6256}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -title = {{Improving the Accuracy of Planet Occurrence Rates from Kepler using Approximate Bayesian Computation}}, -url = {http://arxiv.org/abs/1803.10787%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -year = {2018} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the `Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a {\$}(100 \backslash,\backslashrm cMpc){\^{}}3{\$} and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts {\$}0{\$} and {\$}1{\$}, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar `downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Rudnick2006, -author = {Trujillo\, I and {\F\$\backslash$"o\rster Schreiber\}, N.\$\sim$M. and \Rudnick\, G and \Barden\, M and \Franx\, M and \Rix\, H.-W. and \Caldwell\, J.\$\sim$A.\$\sim$R. and \McIntosh\, D.\$\sim$H. and \Toft\, S and \H\$\backslash$"a\ussler\, B and \Zirm\, A and {\van Dokkum\}, P.\$\sim$G. and \Labb\$\backslash$'e\, L}, -title = {{{\textless}JiaoWen1.pdf{\textgreater}}}, -year = {2006} -} -@article{Messias2014, -abstract = {Context. The submillimetre-bright galaxy population is believed to comprise, aside from local galaxies and radio-loud sources, intrinsically active star-forming galaxies, the brightest of which are lensed gravitationally. The latter enable studies at a level of detail beyond what is usually possible by the observation facility. Aims. This work focuses on one of these lensed systems, HATLAS{\^{a}}‰ J142935.3-002836 (H1429-0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation. Methods. Multi-wavelength high-resolution data is utilised to assess the nature of the system. A lensing-analysis algorithm that simultaneously fits different wavebands is adopted to characterise the lens. The background galaxy dynamical information is studied by reconstructing the 3D source plane of the ALMA CO{\^{a}}‰ (J:4{\^{a}}‰ →{\^{a}}‰ 3) transition. Near-IR imaging from HST and Keck-AO allows to constrain rest-frame optical photometry independently for the foreground and background systems. Physical parameters (such as stellar and dust masses) are estimated via modelling of the spectral energy distribution taking source blending, foreground obscuration, and differential magnification into account. Results. The system comprises a foreground edge-on disk galaxy (at zsp = 0.218) with an almost complete Einstein ring around it. The background source (at zsp = 1.027) is magnified by a factor of $\mu$ $\sim$ 8-10 depending on wavelength. It is comprised of two components and a tens-of-kpc-long tidal tail resembling the Antenn{\ae} merger. As a whole, the background source is a massive stellar system (1.32-0.41+ 0.63 × 1011 M ⊙) forming stars at a rate of 394 ± 90 M⊙ yr-1, and it has a significant gas reservoir MISM = 4.6 ± 1.7 × 1010 M⊙. Its depletion time due to star formation alone is thus expected to be $\tau$SF = M ISM/SFR = 117 ± 51 Myr. The dynamical mass of one of the components is estimated to be 5.8 ± 1.7 × 1010 M ⊙, and, together with the photometric total mass estimate, it implies that H1429-0028 is a major merger system (1:2.8-1.5+1.8). {\textcopyright} 2014 ESO.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1406.4859v1}, -author = {Messias, Hugo and Dye, Simon and Nagar, Neil and Orellana, Gustavo and {Shane Bussmann}, R. and Calanog, Jae and Dannerbauer, Helmut and Fu, Hai and Ibar, Edo and Inohara, Andrew and Ivison, R. J. and Negrello, Mattia and Riechers, Dominik A. and Sheen, Yun Kyeong and Aguirre, James E. and Amber, Simon and Birkinshaw, Mark and Bourne, Nathan and Bradford, Charles M. and Clements, Dave L. and Cooray, Asantha and {De Zotti}, Gianfranco and Demarco, Ricardo and Dunne, Loretta and Eales, Stephen and Fleuren, Simone and Kamenetzky, Julia and Lupu, Roxana E. and Maddox, Steve J. and Marrone, Daniel P. and Micha{\l}owski, Micha{\l} J. and Murphy, Eric J. and Nguyen, Hien T. and Omont, Alain and Rowlands, Kate and Smith, Dan and Smith, Matt and Valiante, Elisabetta and Vieira, Joaquin D.}, -doi = {10.1051/0004-6361/201424410}, -eprint = {arXiv:1406.4859v1}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: ISM,Galaxies: kinematics and dynamics,Gravitational lensing: strong}, -number = {3}, -pages = {A92}, -pmid = {18274343}, -title = {{Herschel-ATLAS and ALMA: Hatlas j142935.3-002836, a lensed major merger at redshift 1.027}}, -url = {http://www.aanda.org/10.1051/0004-6361/201424410}, -volume = {568}, -year = {2014} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of $\sim$3692 galaxies, with -18.5 <= M_g < -22.0 mag and redshift 0.01 <= z < 0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of $\sim$2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined (>60 degrees) systems, we find the following results. (1) The optical r-band fraction (f_opt-r) of barred galaxies is $\sim$48%-52%. (2) When galaxies are separated according to normalized half light radius (r_e/R_24), a remarkable result is seen: f_opt-r rises sharply, from $\sim$40% in galaxies that have small r_e/R_24 and visually appear to host prominent bulges, to $\sim$70% for galaxies that have large r_e/R_24 and appear disk-dominated. (3) f_opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that $\sim$20% of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity >=0.4) and large enough (semi-major axis >=1.5 kpc) to be reliably characterized via ellipse-fitting out to z$\sim$0.8, we get an optical r-band fraction for strong bars f_opt-s of $\sim$34%. This value is higher only by a modest factor of 1.4, compared to the value of $\sim$24%+-4% reported at z$\sim$0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z$\sim$0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Johnson, Crockett}, -doi = {10.2307/3616804}, -eprint = {0802.3961}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Johnson - 1975 - A Construction for a Regular Heptagon.pdf:pdf}, -issn = {00255572}, -journal = {The Mathematical Gazette}, -keywords = {Astrophysics}, -number = {407}, -pages = {17}, -title = {{A Construction for a Regular Heptagon}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {59}, -year = {1975} -} -@article{Veale2016, -abstract = {We present spatially resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (ETGs; MK ≲ -25.7 mag, stellar mass M* ≳ 1011.8 M⊙) of the volumelimited (D {\textless} 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650-5850 {\AA}from the 246-fibre Mitchell integral-field spectrograph at McDonald Observatory, covering a 107 arcsec×107 arcsec field of view(often reaching 2 to 3 effective radii).We measure the 2D spatial distribution of each galaxy's angular momentum ($\lambda$ and fast or slow rotator status), velocity dispersion ($\sigma$), and higher order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ({\$\sim${}}80 per cent) of slow and non-rotators with $\lambda$ ≲ 0.2. When combined with the lower mass ETGs in the ATLAS3D survey, we find the fraction of slow rotators to increase dramatically with galaxy mass, reaching {\$\sim${}}50 per cent at MK {\$\sim${}} -25.5 mag and {\$\sim${}}90 per cent at MK ≲ -26 mag. All of our fast rotators show a clear anticorrelation between h3 and V/$\sigma$, and the slope of the anticorrelation is steeper in more round galaxies. The radial profiles of s show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK ≲ -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat s profiles, whereas five of the seven 'isolated' galaxies are all fainter than MK = -25.8 mag and have falling $\sigma$. All of our galaxies have positive average h4; the most luminous galaxies have average h4 {\$\sim${}} 0.05, while less luminous galaxies have a range of values between 0 and 0.05. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising s profiles. We discuss the implications for the relationship among dynamical mass, $\sigma$, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E and McConnell, Nicholas J and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by a global driving force and a local positive feedback mechanism, which creates regular geometric and/or temporal patterns, and decreases the entropy locally, in contrast to random processes. Here we investigate for the first time a comprehensive number of (17) self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous “order out of randomness”, during the evolution from an initially disordered system to an ordered quasi-stationary system, mostly by quasi-periodic limit-cycle dynamics, but also by harmonic (mechanical or gyromagnetic) resonances. The global driving force can be due to gravity, electromagnetic forces, mechanical forces (e.g., rotation or differential rotation), thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational (Balbus-Hawley) instability, the convective (Rayleigh-B{\'{e}}nard) instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or a loss-cone instability. Physical models of astrophysical self-organization processes require hydrodynamic, magneto-hydrodynamic (MHD), plasma, or N-body simulations. Analytical formulations of self-organizing systems generally involve coupled differential equations with limit-cycle solutions of the Lotka-Volterra or Hopf-bifurcation type.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C M and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G and Scargle, Jeffrey D and Melatos, Andrew and Wagoner, Robert V and Trimble, Virginia and Green, William H}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Lovell2018a, -abstract = {We use the IllustrisTNG (TNG) cosmological simulations to provide theoretical expectations for the dark matter mass fractions (DMFs) and circular velocity profiles of galaxies. TNG predicts flat circular velocity curves for z = 0 Milky Way (MW)-like galaxies beyond a few kpc from the galaxy centre, in better agreement with observational constraints than its predecessor, Illustris. TNG also predicts an enhancement of the dark matter mass within the 3D stellar half-mass radius (rhalf; M200c = 1010-1013M⊙, z ≤ 2) compared to its dark matter only and Illustris counterparts. This enhancement leads TNG present-day galaxies to be dominated by dark matter within their inner regions, with fDM({\textless} rhalf) ≳ 0.5 at all masses and with a minimum for MW-mass galaxies. The 1$\sigma$ scatter is ≲10 per cent at all apertures, which is smaller than that inferred by some observational data sets, e.g. 40 per cent from the SLUGGS survey. TNG agrees with the majority of the observationally inferred values for elliptical galaxies once a consistent initial mass function is adopted (Chabrier) and the DMFs are measured within the same apertures. The DMFs measured within rhalf increase towards lower redshifts: this evolution is dominated by the increase in galaxy size with time. At z {\$\sim${}} 2, the DMF in disc-like TNG galaxies decreases with increasing galaxy mass, with fDM({\textless} rhalf) {\$\sim${}} 0.10-0.65 for 1010 ≲ Mstars/M⊙ ≲ 1012, and are two times higher than if TNG galaxies resided in Navarro-Frenk-White dark matter haloes unaffected by baryonic physics. It remains to be properly assessed whether recent observational estimates of the DMFs at z {\$\sim${}}2 rule out the contraction of the dark matter haloes predicted by the TNG model.}, -archivePrefix = {arXiv}, -arxivId = {1801.10170}, -author = {Lovell, Mark R and Pillepich, Annalisa and Genel, Shy and Nelson, Dylan and Springel, Volker and Pakmor, R{\"{u}}diger and Marinacci, Federico and Weinberger, Rainer and Torrey, Paul and Vogelsberger, Mark and Alabi, Adebusola and Hernquist, Lars}, -doi = {10.1093/MNRAS/STY2339}, -eprint = {1801.10170}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {(cosmology:) dark matter,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1950--1975}, -title = {{The fraction of dark matter within galaxies from the IllustrisTNG simulations}}, -volume = {481}, -year = {2018} -} -@article{Enzi2021, -abstract = {We derive joint constraints on the warm dark matter (WDM) half-mode scale by combining the analyses of a selection of astrophysical probes: strong gravitational lensing with extended sources, the Ly $\alpha$ forest, and the number of luminous satellites in the Milky Way. We derive an upper limit of $\lambda$hm = 0.089 Mpc h-1 at the 95 per cent confidence level, which we show to be stable for a broad range of prior choices. Assuming a Planck cosmology and that WDM particles are thermal relics, this corresponds to an upper limit on the half-mode mass of Mhm < 3 ∼ 107 M{\textperiodcentered} h-1, and a lower limit on the particle mass of mth > 6.048 keV, both at the 95 per cent confidence level. We find that models with $\lambda$hm > 0.223 Mpc h-1 (corresponding to mth > 2.552 keV and Mhm < 4.8 ∼ 108 M{\textperiodcentered} h-1) are ruled out with respect to the maximum likelihood model by a factor ≤1/20. For lepton asymmetries L6 > 10, we rule out the 7.1 keV sterile neutrino dark matter model, which presents a possible explanation to the unidentified 3.55 keV line in the Milky Way and clusters of galaxies. The inferred 95 percentiles suggest that we further rule out the ETHOS-4 model of self-interacting DM. Our results highlight the importance of extending the current constraints to lower half-mode scales. We address important sources of systematic errors and provide prospects for how the constraints of these probes can be improved upon in the future.}, -archivePrefix = {arXiv}, -arxivId = {2010.13802}, -author = {Enzi, Wolfgang and Murgia, Riccardo and Newton, Oliver and Vegetti, Simona and Frenk, Carlos and Viel, Matteo and Cautun, Marius and Fassnacht, Christopher D. and Auger, Matt and Despali, Giulia and McKean, John and Koopmans, L{\'{e}}on V.E. and Lovell, Mark}, -doi = {10.1093/mnras/stab1960}, -eprint = {2010.13802}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Enzi2020JointConstraintsthermalRelic.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Galaxy: structure,Gravitational lensing: strong,Intergalactic medium}, -number = {4}, -pages = {5848--5862}, -title = {{Joint constraints on thermal relic dark matter from strong gravitational lensing, the Ly $\alpha$ forest, and Milky Way satellites}}, -volume = {506}, -year = {2021} -} -@article{Blumenthal1986, -abstract = {Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in. radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.}, -author = {Blumenthal, G R and Faber, S M and Flores, R and Primack, J R}, -doi = {10.1086/163867}, -isbn = {9781848000919}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Astronomical Models,Baryons,Galactic Evolution,Galactic Rotation,Galactic Structure,Gravitational Collapse,Halos,Interstellar Matter,Many Body Problem,Mass Distribution,Missing Mass (Astrophysics),Spiral Galaxies}, -month = {feb}, -pages = {27}, -title = {{Contraction of dark matter galactic halos due to baryonic infall}}, -url = {http://adsabs.harvard.edu/doi/10.1086/163867}, -volume = {301}, -year = {2002} -} -@article{Xie2015, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high-resolution N-body simulations of galactic dark matter haloes to test if this remarkable property can be understood within the context of the cold dark matter (CDM) cosmology. We construct halo merger trees from the simulations and use a semi-analytic model to follow the formation of satellite galaxies. We find that in all six of our simulations, the 11 brightest satellites are indeed distributed along thin, disc-like structures analogous to that traced by the satellites of the Milky Way. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhaloes within it, which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhaloes but is similar to that of the subset of subhaloes that had the most massive progenitors at earlier times. The elongated disc-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I. and Frenk, Carlos S. and Cole, Shaun and Helly, John C. and Jenkins, Adrian and Navarro, Julio F. and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Libeskind et al. - 2005 - The distribution of satellite galaxies The great pancake.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Dutton2011, -abstract = {We investigate the origin of the relations between stellar mass and optical circular velocity for early-type galaxies (ETGs) and late-type galaxies (LTGs) - the Faber-Jackson (FJ) and Tully-Fisher (TF) relations. We combine measurements of dark halo masses (from satellite kinematics and weak lensing), and the distribution of baryons in galaxies (from a new compilation of galaxy scaling relations), with constraints on dark halo structure from cosmological simulations. The principal unknowns are the halo response to galaxy formation and the stellar initial mass function (IMF). The slopes of the TF and FJ relations are naturally reproduced for a wide range of halo response and IMFs. However, models with a universal IMF and universal halo response cannot simultaneously reproduce the zero-points of both the TF and FJ relations. For a model with a universal Chabrier IMF, LTGs require halo expansion, while ETGs require halo contraction. A Salpeter IMF is permitted for high-mass ($\sigma$≳ 180kms-1) ETGs, but is inconsistent for intermediate masses, unless Vcirc(Re)/$\sigma$e≳ 1.6. If the IMF is universal and close to Chabrier, we speculate that the presence of a major merger may be responsible for the contraction in ETGs while clumpy accreting streams and/or feedback leads to expansion in LTGs. Alternatively, a recently proposed variation in the IMF disfavours halo contraction in both types of galaxies. Finally we show that our models naturally reproduce flat and featureless circular velocity profiles within the optical regions of galaxies without fine-tuning. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1012.5859}, -author = {Dutton, Aaron A. and Conroy, Charlie and van den Bosch, Frank C. and Simard, Luc and Mendel, J. Trevor and Courteau, St{\'{e}}phane and Dekel, Avishai and More, Surhud and Prada, Francisco}, -doi = {10.1111/j.1365-2966.2011.19038.x}, -eprint = {1012.5859}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular, cD,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: spiral,Galaxies: structure}, -month = {sep}, -number = {1}, -pages = {322--345}, -title = {{Dark halo response and the stellar initial mass function in early-type and late-type galaxies}}, -volume = {416}, -year = {2011} -} -@article{Lanusse2017a, -abstract = {Galaxy-scale strong gravitational lensing can not only provide a valuable probe of the dark matter distribution of massive galaxies, but also provide valuable cosmological constraints, either by studying the population of strong lenses or by measuring time delays in lensed quasars. Due to the rarity of galaxy-scale strongly lensed systems, fast and reliable automated lens finding methods will be essential in the era of large surveys such as Large Synoptic Survey Telescope, Euclid and Wide-Field Infrared Survey Telescope. To tackle this challenge, we introduce CMU DeepLens, a new fully automated galaxy-galaxy lens finding method based on deep learning. This supervised machine learning approach does not require any tuning after the training step which only requires realistic image simulations of strongly lensed systems. We train and validate our model on a set of 20 000 LSST-like mock observations including a range of lensed systems of various sizes and signal-to-noise ratios (S/N).We find on our simulated data set that for a rejection rate of non-lenses of 99 per cent, a completeness of 90 per cent can be achieved for lenses with Einstein radii larger than 1.4 arcsec and S/N larger than 20 on individual g-band LSST exposures. Finally, we emphasize the importance of realistically complex simulations for training such machine learning methods by demonstrating that the performance of models of significantly different complexities cannot be distinguished on simpler simulations.}, -archivePrefix = {arXiv}, -arxivId = {1703.02642}, -author = {Lanusse, Fran{\c{c}}ois and Ma, Quanbin and Li, Nan and Collett, Thomas E. and Li, Chun Liang and Ravanbakhsh, Siamak and Mandelbaum, Rachel and P{\'{o}}czos, Barnab{\'{a}}s}, -doi = {10.1093/mnras/stx1665}, -eprint = {1703.02642}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lanusse et al. - 2018 - CMU DeepLens Deep learning for automatic image-based galaxy-galaxy strong lens finding(2).pdf:pdf}, -isbn = {0021-9258 (Print)$\$r0021-9258 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: statistical,gravitational lensing: strong}, -number = {3}, -pages = {3895--3906}, -pmid = {10913147}, -title = {{CMU DeepLens: Deep learning for automatic image-based galaxy-galaxy strong lens finding}}, -url = {http://arxiv.org/abs/1703.02642}, -volume = {473}, -year = {2018} -} -@article{Strigari2008, -abstract = {We use kinematic data from three new, nearby, extremely low-luminosity Milky Way dwarf galaxies (Ursa Major II, Willman 1, and Coma Berenices) to constrain the properties of their dark matter halos, and from these make predictions for the gamma-ray flux from annihilation of dark matter particles in these halos. We show that these 10^3 solar luminosity dwarfs are the most dark matter dominated galaxies in the Universe, with total masses within 100 pc in excess of 10^6 solar masses. Coupled with their relative proximity, their large masses imply that they should have mean gamma-ray fluxes comparable to or greater than any other known satellite galaxy of the Milky Way. Our results are robust to both variations of the inner slope of the density profile and the effect of tidal interactions. The fluxes could be boosted by up to two orders of magnitude if we include the density enhancements caused by surviving dark matter substructure.}, -archivePrefix = {arXiv}, -arxivId = {0709.1510}, -author = {Strigari, Louis E. and Koushiappas, Savvas M. and Bullock, James S. and Kaplinghat, Manoj and Simon, Joshua D. and Geha, Marla and Willman, Beth}, -doi = {10.1086/529488}, -eprint = {0709.1510}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Subject headingg s,cosmology,theory — dark matter}, -number = {2}, -pages = {614--620}, -pmid = {22580847}, -title = {{The Most Dark‐Matter–dominated Galaxies: Predicted Gamma‐Ray Signals from the Faintest Milky Way Dwarfs}}, -url = {http://arxiv.org/abs/0709.1510%0Ahttp://dx.doi.org/10.1086/529488}, -volume = {678}, -year = {2008} -} -@article{Khochfar2011a, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* > 1010.5M⊙ contributing $\sim$20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between $\sim$50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z > 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) > 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z < 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive (>1010M⊙) fast rotators being more than one order of magnitude more frequent at z$\sim$ 2. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R. and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Khochfar et al. - 2011 - The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies.pdf:pdf}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: structure}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Treu2011, -abstract = {The relative contribution of baryons and dark matter to the inner regions of spiral galaxies provides critical clues to their formation and evolution, but it is generally difficult to determine. For spiral galaxies that are strong gravitational lenses, however, the combination of lensing and kinematic observations can be used to break the disc-halo degeneracy. In turn, such data constrain fundamental parameters such as (i) the mass density profile slope and axial ratio of the dark matter halo, and by comparison with dark matter-only numerical simulations the modifications imposed by baryons; (ii) the mass in stars and therefore the overall star formation efficiency, and the amount of feedback; (iii) by comparison with stellar population synthesis models, the normalization of the stellar initial mass function. In this first paper of a series, we present a sample of 16 secure, one probable and six possible strong lensing spiral galaxies, for which multiband high-resolution images and rotation curves were obtained using the Hubble Space Telescope and KeckII telescope as part of the Sloan WFC Edge-on Late-type Lens Survey (SWELLS). The sample includes eight newly discovered secure systems. We characterize the sample of deflector galaxies in terms of their morphologies, structural parameters and stellar masses. We find that the SWELLS sample of secure lenses spans a broad range of morphologies (from lenticular to late-type spiral), spectral types (quantified by H$\alpha$ emission) and bulge to total stellar mass ratio (0.22-0.85), while being limited to M* > 1010.5M⊙. The SWELLS sample is thus well suited for exploring the relationship between dark and luminous matter in a broad range of galaxies. We find that the deflector galaxies obey the same size-mass relation as that of a comparison sample of elongated non-lens galaxies selected from the Sloan Digital Sky Survey. We conclude that the SWELLS sample is consistent with being representative of the overall population of high-mass high-inclination discy galaxies. {\textcopyright} 2011 The Authors. Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1104.5663}, -author = {Treu, Tommaso and Dutton, Aaron A. and Auger, Matthew W. and Marshall, Philip J. and Bolton, Adam S. and Brewer, Brendon J. and Koo, David C. and Koopmans, L{\`{e}}on V.E.}, -doi = {10.1111/j.1365-2966.2011.19378.x}, -eprint = {1104.5663}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: spiral,Galaxies: structure,Gravitational lensing: strong}, -number = {3}, -pages = {1601--1620}, -title = {{The SWELLS survey - I. A large spectroscopically selected sample of edge-on late-type lens galaxies}}, -volume = {417}, -year = {2011} -} -@article{Ou2017, -author = {Ou, Teresa}, -file = {:C\:/Users/Jammy/Documents/Papers/Software/NUFFTGPU.pdf:pdf}, -title = {{gNUFFTW: Auto-Tuning for High-Performance GPU-Accelerated Non-Uniform Fast Fourier Transforms}}, -url = {http://www2.eecs.berkeley.edu/Pubs/TechRpts/2017/EECS-2017-90.html}, -year = {2017} -} -@article{Griffiths2019, -author = {Griffiths, Matthew and Wales, David J}, -doi = {10.1021/acs.jctc.9b00567}, -issn = {1549-9618}, -journal = {Journal of Chemical Theory and Computation}, -title = {{Nested basin-sampling}}, -year = {2019} -} -@article{McCully2014, -abstract = {In strong gravitational lens systems, the light bending is usually dominated by one main galaxy, but may be affected by other mass along the line of sight (LOS). Shear and convergence can be used to approximate the contributions from less significant perturbers (e.g. those that are projected far from the lens or have a small mass), but higher order effects need to be included for objects that are closer or more massive. We develop a framework for multiplane lensing that can handle an arbitrary combination of tidal planes treated with shear and convergence and planes treated exactly (i.e. including higher order terms). This framework addresses all of the traditional lensing observables including image positions, fluxes, and time delays to facilitate lens modelling that includes the non-linear effects due to mass along the LOS. It balances accuracy (accounting for higher order terms when necessary) with efficiency (compressing all other LOS effects into a set of matrices that can be calculated up front and cached for lens modelling). We identify a generalized multiplane mass sheet degeneracy, in which the effective shear and convergence are sums over the lensing planes with specific, redshift-dependent weighting factors. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1401.0197}, -author = {McCully, Curtis and Keeton, Charles R. and Wong, Kenneth C. and Zabludoff, Ann I.}, -doi = {10.1093/mnras/stu1316}, -eprint = {1401.0197}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: strong,Gravitational lensing: weak}, -month = {oct}, -number = {4}, -pages = {3631--3642}, -title = {{A new hybrid framework to efficiently model lines of sight to gravitational lenses}}, -volume = {443}, -year = {2014} -} -@article{Wilson1995, -abstract = {The recent development of unified theories of active galactic nuclei (AGN) has indicated that there are two physically distinct classes of these objects - radio-loud and radio-quiet. The primary observational distinctions between the two types are: (1) The radio-loud objects produce large scale radio jets and lobes, with the kinetic power of the jets being a significant fraction of the total bolometric luminosity. On the other hand, the weak radio ejecta of the radio-quiet objects are energetically insignificant. (2) The radio-loud objects are associated with elliptical galaxies which have undergone recent mergers, while the radio-quiets prefer spiral hosts. (3) The space density of the radio-louds at a given optical luminosity is $\approx$ 10 times lower than that of the radio-quiets. Despite these differences, the (probably) thermal emissions from the AGN (continua and lines from X-ray to infrared wavelengths) are quite similar in the two classes of object. We argue that this last result suggests that the black hole masses and mass accretion rates in the two classes are not greatly different, and that the difference between the classes is associated with the spin of the black hole. We assume that the normal process of accretion through a disk does not lead to rapidly spinning holes, and propose instead that galaxies (e.g. spirals) which have not suffered a recent major merger event contain non-rotating or only slowly rotating black holes. When two such galaxies merge, the two black holes are known to form a binary and we assume that they eventually coalesce. In the small fraction of mergers in which the two ``parent'' galaxies contain very massive holes of roughly equal mass, a rapidly spinning, very massive hole results. It is proposed that such mergers are the progenitors of powerful radio}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9408005}, -author = {Wilson, A. S. and Colbert, E. J. M.}, -doi = {10.1086/175054}, -eprint = {9408005}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Active Galactic Nuclei,Black Holes (Astronomy),Cosmology,Interacting Galaxies,Luminosity,Quasars,Radio Astronomy,Radio Jets (Astronomy)}, -month = {jan}, -pages = {62}, -primaryClass = {astro-ph}, -title = {{The difference between radio-loud and radio-quiet active galaxies}}, -url = {http://adsabs.harvard.edu/doi/10.1086/175054}, -volume = {438}, -year = {1995} -} -@article{Dekel2014, -abstract = {We study the origin of high-redshift, compact, quenched spheroids (red nuggets) through the dissipative shrinkage of gaseous discs into compact star-forming systems (blue nuggets). The discs, fed by cold streams, undergo violent disc instability that drives gas into the centre (along with mergers). The inflow is dissipative when its time-scale is shorter than the star formation time-scale. This implies a threshold of $\sim$0.28 in the cold-to-total mass ratio within the disc radius. For the typical gas fraction $\sim$0.5 at z $\sim$ 2, this threshold is traced back to a maximum spin parameter of $\sim$0.05, implying that $\sim$half the star-forming galaxies contract to blue nuggets, while the rest form extended stellar discs. Thus, the surface density of blue galaxies is expected to be bimodal about $\sim$109M⊙ kpc-2, slightly increasing with mass. The blue nuggets are expected to be rare at low z when the gas fraction is low. The blue nuggets quench to red nuggets by complementary internal and external mechanisms. Internal quenching by a compact bulge, in a fast mode and especially at high z, may involve starbursts, stellar and active galactic nucleus feedback, or Q-quenching. Quenching due to hot-medium haloes above 1012M⊙ provides maintenance and a slower mode at low redshift. These predictions are confirmed in simulations and are consistent with observations at z = 0-3. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1310.1074}, -author = {Dekel, A. and Burkert, A.}, -doi = {10.1093/mnras/stt2331}, -eprint = {1310.1074}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: Spiral,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,cD}, -month = {feb}, -number = {2}, -pages = {1870--1879}, -title = {{Wet disc contraction to galactic blue nuggets and quenching to red nuggets}}, -volume = {438}, -year = {2014} -} -@article{Springel2005, -abstract = {The cold dark matter model has become the leading theoretical picture for the formation of structure in the Universe. This model, together with the theory of cosmic inflation, makes a clear prediction for the initial conditions for structure formation and predicts that structures grow hierarchically through gravitational instability. Testing this model requires that the precise measurements delivered by galaxy surveys can be compared to robust and equally precise theoretical calculations. Here we present a simulation of the growth of dark matter structure using 2,1603 particles, following them from redshift z = 127 to the present in a cube-shaped region 2.230 billion lightyears on a side. In postprocessing, we also follow the formation and evolution of the galaxies and quasars. We show that baryon-induced features in the initial conditions of the Universe are reflected in distorted form in the low-redshift galaxy distribution, an effect that can be used to constrain the nature of dark energy with future generations of observational surveys of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0504097}, -author = {Springel, Volker and White, Simon D.M. and Jenkins, Adrian and Frenk, Carlos S. and Yoshida, Naoki and Gao, Liang and Navarro, Julio and Thacker, Robert and Croton, Darren and Helly, John and Peacock, John A. and Cole, Shaun and Thomas, Peter and Couchman, Hugh and Evrard, August and Colberg, J{\"{o}}rg and Pearce, Frazer}, -doi = {10.1038/nature03597}, -eprint = {0504097}, -isbn = {0028-0836}, -issn = {00280836}, -journal = {Nature}, -month = {jun}, -number = {7042}, -pages = {629--636}, -pmid = {15931216}, -primaryClass = {astro-ph}, -title = {{Simulations of the formation, evolution and clustering of galaxies and quasars}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/15931216}, -volume = {435}, -year = {2005} -} -@article{Keeton1997, -abstract = {Galaxies modeled as singular isothermal ellipsoids with an axis ratio distribution similar to the observed axis ratio distribution of E and S0 galaxies are statistically consistent with both the observed numbers of two-image and four-image lenses and the inferred ellipticities of individual lenses. However, no four-image lens is well fit by the model (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 20{\$}), the axis ratio of the model can be significantly different from that of the observed lens galaxy, and the major axes of the model and the galaxy may be slightly misaligned. We found that models with a second, independent, external shear axis could fit the data well (typical {\$}\backslashchi{\^{}}2/N{\_}{\{}dof{\}} \backslashsim 1{\$}), while adding the same number of extra parameters to the radial mass distribution does not produce such a dramatic improvement in the fit. An independent shear axis can be produced by misalignments between the luminous galaxy and its dark matter halo, or by external shear perturbations due to galaxies and clusters correlated with the primary lens or along the line of sight. We estimate that the external shear perturbations have no significant effect on the expected numbers of two-image and four-image lenses, but that they can be important perturbations in individual lens models. However, the amplitudes of the external shears required to produce the good fits are larger than our estimates for typical external shear perturbations (10-15{\%} shear instead of 1-3{\%} shear) suggesting that the origin of the extra angular structure must be intrinsic to the primary lens galaxy in most cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610163}, -author = {Keeton, C R and Kochanek, C S and Seljak, U}, -doi = {10.1086/304172}, -eprint = {9610163}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Elliptical and Lenticular,cD,cosmology: theory}, -number = {2}, -pages = {604--620}, -primaryClass = {astro-ph}, -title = {{Shear and Ellipticity in Gravitational Lenses}}, -url = {http://arxiv.org/abs/astro-ph/9610163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/304172}, -volume = {482}, -year = {1997} -} -@article{Pub---ae2019, -abstract = {Strong-gravitational lens systems with quadruply imaged quasars (quads) are unique probes to address several fundamental problems in cosmology and astrophysics. Although they are intrinsically very rare, ongoing and planned wide-field deep-sky surveys are set to discover thousands of such systems in the next decade. It is thus paramount to devise a general framework to model strong-lens systems to cope with this large influx without being limited by expert investigator time. We propose such a general modelling framework (implemented with the publicly available software lenstronomy) and apply it to uniformly model three-band Hubble Space Telescope Wide Field Camera 3 images of 13 quads. This is the largest uniformly modelled sample of quads to date and paves the way for a variety of studies. To illustrate the scientific content of the sample, we investigate the alignment between the mass and light distribution in the deflectors. The position angles of these distributions are well-aligned, except when there is strong external shear. However, we find no correlation between the ellipticity of the light and mass distributions. We also show that the observed flux-ratios between the images depart significantly from the predictions of simple smooth models. The departures are strongest in the bluest band, consistent with microlensing being the dominant cause in addition to millilensing. Future papers will exploit this rich data set in combination with ground-based spectroscopy and time delays to determine quantities such as the Hubble constant, the free streaming length of dark matter, and the normalization of the initial stellar mass function.}, -archivePrefix = {arXiv}, -arxivId = {1807.09278}, -author = {Shajib, A. J. and Birrer, S. and Treu, T. and Auger, M. W. and Agnello, A. and Anguita, T. and Buckley-Geer, E. J. and Chan, J. H.H. and Collett, T. E. and Courbin, F. and Fassnacht, C. D. and Frieman, J. and Kayo, I. and Lemon, C. and Lin, H. and Marshall, P. J. and McMahon, R. and More, A. and Morgan, N. D. and Motta, V. and Oguri, M. and Ostrovski, F. and Rusu, C. E. and Schechter, P. L. and Shanks, T. and Suyu, S. H. and Meylan, G. and Abbott, T. M.C. and Allam, S. and Annis, J. and Avila, S. and Bertin, E. and Brooks, D. and {Carnero Rosell}, A. and {Carrasco Kind}, M. and Carretero, J. and Cunha, C. E. and {Da Costa}, L. N. and {De Vicente}, J. and Desai, S. and Doel, P. and Flaugher, B. and Fosalba, P. and Garc{\'{i}}a-Bellido, J. and Gerdes, D. W. and Gruen, D. and Gruendl, R. A. and Gutierrez, G. and Hartley, W. G. and Hollowood, D. L. and Hoyle, B. and James, D. J. and Kuehn, K. and Kuropatkin, N. and Lahav, O. and Lima, M. and Maia, M. A.G. and March, M. and Marshall, J. L. and Melchior, P. and Menanteau, F. and Miquel, R. and Plazas, A. A. and Sanchez, E. and Scarpine, V. and Sevilla-Noarbe, I. and Smith, M. and Soares-Santos, M. and Sobreira, F. and Suchyta, E. and Swanson, M. E.C. and Tarle, G. and Walker, A. R.}, -doi = {10.1093/mnras/sty3397}, -eprint = {1807.09278}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shajib et al. - 2019 - Is every strong lens model unhappy in its own way Uniform modelling of a sample of 13 quadruply imaged quasars(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: structure,gravitational lensing: strong,methods: data analysis}, -number = {4}, -pages = {5649--5671}, -title = {{Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 13 quadruply+ imaged quasars}}, -volume = {483}, -year = {2019} -} -@article{Cautun2015a, -abstract = {We investigate the angular and kinematic distributions of satellite galaxies around a large sample of bright isolated primaries in the spectroscopic and photometric catalogues of the Sloan Digital Sky Survey (SDSS). We detect significant anisotropy in the spatial distribution of satellites. To test whether this anisotropy could be related to the rotating disks of satellites recently found by Ibata et al. in a sample of SDSS galaxies, we repeat and extend their analysis. Ibata et al. found an excess of satellites on opposite sides of their primaries having anticorrelated radial velocities. We find that this excess is sensitive to small changes in the sample selection criteria which can greatly reduce its significance. In addition, we find no evidence for correspondingly correlated velocities for satellites observed on the same side of their primaries, which would be expected for rotating disks of satellites. We conclude that the detection of coherent rotation in the satellite population in current observational samples is not robust. We compare our data to the {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM Millennium simulations populated with galaxies according to the semi-analytic model of Guo et al. We find excellent agreement with the spatial distribution of satellites in the SDSS data and the lack of a strong signal from coherent rotation.}, -archivePrefix = {arXiv}, -arxivId = {1410.7778}, -author = {Cautun, Marius and Wang, Wenting and Frenk, Carlos S and Sawala, Till}, -doi = {10.1093/mnras/stv490}, -eprint = {1410.7778}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {3}, -pages = {2576--2587}, -title = {{A new spin on discs of satellite galaxies}}, -volume = {449}, -year = {2015} -} -@article{Sonnenfeld2025, -abstract = {The Sloan Lens ACS (SLACS) is the best studied sample of strong lenses to date. Much of our knowledge of the SLACS lenses has been obtained by combining strong lensing with stellar kinematics constraints. However, interpreting stellar kinematics data is difficult: it requires reconstructing the three-dimensional structure of a galaxy and the orbits of its stars. In this work we pursued an alternative approach to the study of galaxy structure with SLACS, based purely on gravitational lensing data. The primary goal of this study is to constrain the stellar population synthesis mismatch parameter $\alpha_{sps}$, quantifying the ratio between the true stellar mass of a galaxy and that obtained with a reference stellar population synthesis model, and the efficiency of the dark matter response to the infall of baryons, $\epsilon$. We combined Einstein radius measurements from the SLACS lenses with weak lensing information from their parent sample, while accounting for selection effects. The data can be fit comparatively well by a model with $\log{\alpha_{sps}}=0.22$ and $\epsilon=0$, corresponding to an IMF slightly lighter than Salpeter and no dark matter contraction, or $\log{\alpha_{sps}}=0$ and $\epsilon=0.8$, equivalent to a Chabrier IMF and almost maximal contraction. This degeneracy could be broken with lensing-only measurements of the projected density slope, but existing data are completely inconsistent with our model. We suspect systematic errors in the measurements to be at the origin of this discrepancy. Number density constraints would also help break the degeneracy. Because of selection effects, SLACS lenses have a larger velocity dispersion than galaxies with the same projected mass distribution, and their velocity dispersion is overestimated. These two biases combined produce a $5\%$ upward shift in the observed velocity dispersion.}, -archivePrefix = {arXiv}, -arxivId = {2501.02054}, -author = {Sonnenfeld, Alessandro}, -eprint = {2501.02054}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnefendl2025SLACSDebiadedII.pdf:pdf}, -keywords = {cd - galaxies,elliptical and lenticular,fundamental parameters,gravitational lensing,strong - galaxies}, -number = {2011}, -pages = {1--10}, -title = {{The SLACS strong lens sample, debiased. II. Lensing-only constraints on the stellar IMF and dark matter contraction in early-type galaxies}}, -url = {http://arxiv.org/abs/2501.02054}, -year = {2025} -} -@article{Kochanek2001, -abstract = {We develop a theory of Einstein rings and demonstrate it using the infrared Einstein ring images of the quasar host galaxies observed in PG 1115]080, B1608]656, and B1938]666. The shape of an Ein-stein ring accurately and independently determines the shape of the lens potential and the shape of the lensed host galaxy. We Ðnd that the host galaxies of PG 1115]080, B1608]656, and B1938]666 have axis ratios of 0.58 {\^{}} 0.02, 0.69 {\^{}} 0.02, and 0.62 {\^{}} 0.14, respectively, including the uncertainties in the lens models. The Einstein rings break the degeneracies in the mass distributions or Hubble constants inferred from observations of gravitational lenses. In particular, the Einstein ring in PG 1115]080 rules out the centrally concentrated mass distributions that lead to a high Hubble constant km s{\$\sim${}}1 Mpc{\$\sim${}}1) (H 0 [ 60 given the measured time delays. Deep, detailed observations of Einstein rings will be revolutionary for constraining mass models and determining the Hubble constant from time-delay measurements.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0006116}, -author = {Kochanek, C S and Keeton, C R and McLeod, B A}, -doi = {10.1086/318350}, -eprint = {0006116}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Distance Scale,Cosmology: Gravitational Lensing,Cosmology: Observations}, -month = {jan}, -number = {1}, -pages = {50--59}, -primaryClass = {astro-ph}, -title = {{The Importance of Einstein Rings}}, -url = {http://stacks.iop.org/0004-637X/547/i=1/a=50}, -volume = {547}, -year = {2002} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C. and Mo, H. J. and Mao, Shude and Kang, Xi and Weinmann, Simone M. and Guo, Yicheng and Jing, Y. P.}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yang et al. - 2006 - The alignment between the distribution of satellites and the orientation of their central galaxy(3).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Schombert2015a, -abstract = {Using isophotal radius correlations for a sample of 2MASS ellipticals, we have constructed a series of template surface brightness profiles to describe the profile shapes of ellipticals as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that ellipticals are weakly non-homologous with respect to structure. Through comparison to the templates, it is discovered that ellipticals are divided into two families; those well matched to the templates and a second class of ellipticals with distinctly shallower profile slopes. We refer to these second type of ellipticals as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D ellipticals cover the same range of luminosity, size and kinematics as normal ellipticals, but maintain a signature of recent equal mass dry mergers. We propose that normal ellipticals grow after an initial dissipation formation era by accretion of low mass companions as outlined in hierarchical formation scenarios, while D ellipticals are the result of later equal mass mergers producing shallow luminosity profiles.}, -archivePrefix = {arXiv}, -arxivId = {1509.08381}, -author = {Schombert, James M}, -doi = {10.1088/0004-6256/150/5/162}, -eprint = {1509.08381}, -isbn = {doi:10.1088/0004-6256/150/5/162}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: structure}, -number = {5}, -pages = {162}, -publisher = {IOP Publishing}, -title = {{The structure of galaxies. III. Two structural families of ellipticals}}, -url = {http://dx.doi.org/10.1088/0004-6256/150/5/162}, -volume = {150}, -year = {2015} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since z = 1.0. We find that lower mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher mass or lower redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single-aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys; we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xu et al. - 2017 - The inner structure of early-type galaxies in the Illustris simulation.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1824--1848}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {469}, -year = {2017} -} -@article{Ferrero2017, -abstract = {The Tully-Fisher relation (TFR) links the stellar mass of a disc galaxy, Mstr, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass-velocity scaling (M ∝ V3) of dark matter haloes, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy-halo mass relation to deviate substantially from a single power law and to evolve rapidly with redshift. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of $\Lambda$ cold dark matter ($\Lambda$CDM) cosmological simulations. Matching both relations requires disc sizes to satisfy constraints given by the concentration of haloes and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass-velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass-size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass-size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass-size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. $\Lambda$CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1607.03100}, -author = {Ferrero, Ismael and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw2691}, -eprint = {1607.03100}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {4}, -pages = {4736--4746}, -title = {{Size matters: Abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE}}, -volume = {464}, -year = {2017} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Buitrago2017a, -abstract = {Using the exquisite depth of the Hubble Ultra Deep Field (HUDF12 programme) dataset, we explore the ongoing assembly of the outermost regions of the most massive galaxies (M{\_}{\{}stellar{\}} {\textgreater} 5x10{\^{}}{\{}10{\}} M{\_}{\{}Sun{\}}) at z {\textless} 1. The outskirts of massive objects, particularly Early-Types Galaxies (ETGs), are expected to suffer a dramatic transformation across cosmic time due to continuous accretion of small galaxies. HUDF imaging allows us to study this process at intermediate redshifts in 6 massive galaxies, exploring the individual surface brightness profiles out to 25 effective radii. We find that 10-30{\%} of the total stellar mass for the galaxies in our sample is contained within 10 {\textless} R {\textless} 50 kpc. These values are in close agreement with numerical simulations, and at least 2-3 times higher than those reported for late-type galaxies. The fraction of stellar mass stored in the outer envelopes/haloes of Massive Early-Type Galaxies increases with decreasing redshift, being 28.7{\%} at {\textless} z {\textgreater} = 0.1, 22.6{\%} at {\textless} z {\textgreater} = 0.65 and 3.5{\%} at {\textless} z {\textgreater} = 2. The fraction of mass in diffuse features linked with ongoing minor merger events is {\textgreater} 1-3{\%}, very similar to predictions based on observed close pair counts. Therefore, our results suggest that the size and mass growth of the most massive galaxies have been solely driven by minor and major merging from z = 1 to today.}, -archivePrefix = {arXiv}, -arxivId = {1602.01846}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Curtis-Lake, Emma and Montes, Mireia and Cooper, Andrew P and Bruce, Victoria A and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Cirasuolo, Michele}, -doi = {10.1093/mnras/stw3382}, -eprint = {1602.01846}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cd,elliptical and lenticular,evolution,galaxies,haloes,high-redshift,morphology,structure}, -number = {January}, -pages = {stw3382}, -title = {{The cosmic assembly of stellar haloes in massive Early-Type Galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3382}, -volume = {000}, -year = {2017} -} -@article{Brewer2014, -abstract = {The long-standing assumption that the stellar initial mass function (IMF) is universal has recently been challenged by a number of observations. Several studies have shown that a "heavy" IMF (e.g., with a Salpeter-like abundance of low mass stars and thus normalisation) is preferred for massive early-type galaxies, while this IMF is inconsistent with the properties of less massive, later-type galaxies. These discoveries motivate the hypothesis that the IMF may vary (possibly very slightly) across galaxies and across components of individual galaxies (e.g. bulges vs discs). In this paper we use a sample of 19 late-type strong gravitational lenses from the SWELLS survey to investigate the IMFs of the bulges and discs in late-type galaxies. We perform a joint analysis of the galaxies' total masses (constrained by strong gravitational lensing) and stellar masses (constrained by optical and near-infrared colours in the context of a stellar population synthesis [SPS] model, up to an IMF normalisation parameter). Using minimal assumptions apart from the physical constraint that the total stellar mass within any aperture must be less than the total mass within the aperture, we find that the bulges of the galaxies cannot have IMFs heavier (i.e. implying high mass per unit luminosity) than Salpeter, while the disc IMFs are not well constrained by this data set. We also discuss the necessity for hierarchical modelling when combining incomplete information about multiple astronomical objects. This modelling approach allows us to place upper limits on the size of any departures from universality. More data, including spatially resolved kinematics (as in paper V) and stellar population diagnostics over a range of bulge and disc masses, are needed to robustly quantify how the IMF varies within galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1310.5177}, -author = {Brewer, Brendon J. and Marshal, Philip J. and Auger, Matthew W. and Treu, Tommaso and Dutton, Aaron A. and Barnab{\`{e}}, Matteo}, -doi = {10.1093/mnras/stt2026}, -eprint = {1310.5177}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies:Fundamental parameters,Galaxies:Spiral,Methods:Statistical}, -month = {jan}, -number = {2}, -pages = {1950--1961}, -title = {{The SWELLS survey - VI. Hierarchical inference of the initial mass functions of bulges and discs}}, -volume = {437}, -year = {2013} -} -@article{Krajnovic2011, -abstract = {We use the ATLAS3D sample of 260 early-type galaxies to study the apparent kinematic misalignment angle, $\Psi$, defined as the angle between the photometric and kinematic major axes. We find that 71 per cent of nearby early-type galaxies are strictly aligned systems ($\Psi$≤ 5°), an additional 14 per cent have 5° < $\Psi$≤ 10° and 90 per cent of galaxies have $\Psi$≤ 15°. Taking into account measurement uncertainties, 90 per cent of galaxies can be considered aligned to better than 5°, suggesting that only a small fraction of early-type galaxies (∼10 per cent) are not consistent with the axisymmetry within the projected half-light radius. We identify morphological features such as bars and rings (30 per cent), dust structures (16 per cent), blue nuclear colours (6 per cent) and evidence of interactions (8 per cent) visible on ATLAS3D galaxies. We use kinemetry to analyse the mean velocity maps and separate galaxies into two broad types of regular and non-regular rotators. We find 82 per cent of regular rotators and 17 per cent of non-regular rotators, with two galaxies that we were not able to classify due to the poor data quality. The non-regular rotators are typically found in dense regions and are massive. We characterize the specific features in the mean velocity and velocity dispersion maps. The majority of galaxies do not have any specific features, but we highlight here the frequency of the kinematically distinct cores (7 per cent of galaxies) and the aligned double peaks in the velocity dispersion maps (4 per cent of galaxies). We separate galaxies into five kinematic groups based on the kinemetric features, which are then used to interpret the ($\Psi$-$\epsilon$) diagram. Most of the galaxies that are misaligned have complex kinematics and are non-regular rotators. In addition, some show evidence of the interaction and might not be in equilibrium, while some are barred. While the trends are weak, there is a tendency that large values of $\Psi$ are found in galaxies at intermediate environmental densities and among the most massive galaxies in the sample. Taking into account the kinematic alignment and the kinemetric analysis, the majority of early-type galaxies have velocity maps more similar to that of the spiral discs than to that of the remnants of equal-mass mergers. We suggest that the most common formation mechanism for early-type galaxies preserves the axisymmetry of the disc progenitors and their general kinematic properties. Less commonly, the formation process results in a triaxial galaxy with much lower net angular momentum. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1102.3801}, -author = {Krajnovi{\'{c}}, Davor and Emsellem, Eric and Cappellari, Michele and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Khochfar, Sadegh and Kuntschner, Harald and Lablanche, Pierre Yves and Mcdermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.18560.x}, -eprint = {1102.3801}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Krajnovi{\'{c}} et al. - 2011 - The ATLAS3D project - II. Morphologies, kinemetric features and alignment between photometric and kinematic(2).pdf:pdf}, -isbn = {1751-7362}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: formation,Galaxies: kinematics and dynamics,cD}, -number = {4}, -pages = {2923--2949}, -pmid = {18340335}, -title = {{The ATLAS3D project - II. Morphologies, kinemetric features and alignment between photometric and kinematic axes of early-type galaxies}}, -volume = {414}, -year = {2011} -} -@article{Agustsson2007a, -abstract = {We investigate the locations of the satellites of relatively isolated host galaxies in the Sloan Digital Sky Survey and the Millennium Run simulation. Provided we use two distinct prescriptions to embed luminous galaxies within the simulated dark matter halos (ellipticals share the shapes of their halos, while disks have angular momenta that are aligned with the net angular momenta of their halos), we find a fair agreement between observation and theory. Averaged over scales rp 500 kpc, the satellites of red, high-mass hosts with low star formation rates are found preferentially near the major axes of their hosts. In contrast, the satellites of blue, low-mass hosts with low star formation rates show little to no anisotropy when averaged over the same scale. The difference between the locations of the satellites of red and blue hosts cannot be explained by the effects of interlopers in the data. Instead, it is caused primarily by marked differences in the dependence of the mean satellite location, $\phi$, on the projected distance at which the satellites are found. We also find that the locations of red, high-mass satellites with low star formation rates show considerably more anisotropy than do the locations of blue, low-mass satellites with high star formation rates. There are two contributors to this result. First, the blue satellites have only recently arrived within their hosts' halos, while the red satellites arrived in the far distant past. Second, the sample of blue satellites is heavily contaminated by interlopers, which suppresses the measured anisotropy compared to the intrinsic anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {0704.3441}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G.}, -doi = {10.1088/0004-637X/709/2/1321}, -eprint = {0704.3441}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Agustsson, Brainerd - 2010 - Anisotropic locations of satellite galaxies Clues to the orientations of galaxies within their dark matter.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: dwarf,Galaxies: fundamental parameters,Galaxies: halos,Galaxies: structure}, -number = {2}, -pages = {1321--1336}, -title = {{Anisotropic locations of satellite galaxies: Clues to the orientations of galaxies within their dark matter halos}}, -url = {http://arxiv.org/abs/0704.3441%0Ahttp://dx.doi.org/10.1088/0004-637X/709/2/1321}, -volume = {709}, -year = {2010} -} -@article{Cooper:2010aa, -author = {Cooper, A P and Cole, S and Frenk, C S and White, S D M and Helly, J and Benson, A J and Lucia, G De and Helmi, A and Jenkins, A and Navarro, J F and Springel, V and Wang, J and Trieste, Inaf-osservatorio Astronomico and Tiepolo, Via G B and Trieste, I-}, -doi = {10.1111/j.1365-2966.2010.16740.x}, -journal = {$\backslash$mnras}, -keywords = {1 i n t,al-,an extended and diffuse,dwarf,formation,galaxies,galaxy,halo,haloes,methods,milky way,numerical,ro d u c,stellar halo envelops the,structure,t i o n}, -month = {aug}, -pages = {744--766}, -title = {{Galactic stellar haloes in the CDM model 1 I N T RO D U C T I O N}}, -volume = {766}, -year = {2010} -} -@article{VanDokkum2017, -abstract = {There is good evidence that the centers of massive early-type galaxies have a bottom-heavy stellar initial mass function (IMF) compared to the IMF of the Milky Way. Here we study the radial variation of the IMF within such galaxies, using a combination of high quality Keck spectroscopy and a new suite of stellar population synthesis models that cover a wide range in metallicity. As in the previous studies in this series, the models are fitted directly to the spectra and treat all elemental abundance ratios as free parameters. Using newly obtained spectroscopy for six galaxies, including deep data extending to $\sim$1Re for the galaxies NGC1407, NGC1600, and NGC2695, we find that the IMF varies strongly with galactocentric radius. For all six galaxies the IMF is bottom-heavy in the central regions, with average mass-to-light ratio "mismatch" parameter a$\sim$2.5 at R=0. The IMF rapidly becomes more bottom-light with increasing radius, flattening off near the Milky Way value (a$\sim$1.1) at R>0.4Re. A consequence is that the luminosity-weighted average IMF depends on the measurement aperture: within R=Re we find =1.3-1.5, consistent with recent lensing and dynamical results from SLACS and ATLAS-3D. Our results are also consistent with several earlier studies that were based on analyses of radial gradients of line indices. The observed IMF gradients support galaxy formation models in which the central regions of massive galaxies had a different formation history than their outer parts. Finally, we make use of the high signal-to-noise central spectra of NGC1407 and NGC2695 to demonstrate how we can disentangle IMF effects and abundance effects.}, -archivePrefix = {arXiv}, -arxivId = {1611.09859}, -author = {van Dokkum, Pieter and Conroy, Charlie and Villaume, Alexa and Brodie, Jean and Romanowsky, Aaron J.}, -doi = {10.3847/1538-4357/aa7135}, -eprint = {1611.09859}, -file = {:C\:/Users/Jammy/Documents/Papers/Ellipticals/vanDokkum2017IMFDwarfs.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/van Dokkum et al. - 2017 - The Stellar Initial Mass Function in Early-type Galaxies from Absorption Line Spectroscopy. III. Radial Gradi.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {abundances,evolution,galaxies,luminosity function,mass function,stars,stellar content,structure}, -number = {2}, -pages = {68}, -title = {{The Stellar Initial Mass Function in Early-type Galaxies from Absorption Line Spectroscopy. III. Radial Gradients}}, -volume = {841}, -year = {2017} -} -@article{Benitez-Llambay2020, -abstract = {We present a model for the formation of the first galaxies before and after the reionization of hydrogen in the early universe. In this model, galaxy formation can only take place in dark matter haloes whose mass exceeds a redshift-dependent critical value, which, before reionization, is equal (in the simplest case) to the mass at which atomic hydrogen cooling becomes effective and, after reionization, is equal to the mass above which gas cannot remain in hydrostatic equilibrium. We define the Halo Occupation Fraction (HOF) as the fraction of haloes that host a luminous galaxy as a function of halo mass. The HOF is established by the interplay between the evolution of the critical mass and the assembly history of haloes and depends on three factors: the minimum halo mass for galaxy formation before reionization, the redshift of reionization, and the intensity of the (evolving) external photoheating rate. Our fiducial model predicts a cutoff in the galaxy mass function at a present-day halo mass, M200 ∼ 3 × 108M⊙; 100% occupation at M200 > 5 × 109M⊙; and a population of starless gaseous haloes of present-day mass in the range 106 ≲ M200/M⊙ ≲ 5 × 109, in which the gas is in thermal equilibrium with the ultraviolet background radiation and in hydrostatic equilibrium in the gravitational potential of the halo. The transition between HOF = 0 and HOF = 1 reflects the stochastic nature of halo mass growth. We explore how these characteristic masses vary with model assumptions and parameter values. The results of our model are in excellent agreement with cosmological hydrodynamic simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {2004.06124}, -author = {Benitez-Llambay, Alejandro and Frenk, Carlos}, -doi = {10.1093/mnras/staa2698}, -eprint = {2004.06124}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Benitez-Llambay, Frenk - 2020 - The detailed structure and the onset of galaxy formation in low-mass gaseous dark matter haloes.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {cos-,cosmology,dark ages,dark matter,dwarf,first stars,formation,galaxies,mology,reionization,star formation}, -number = {April}, -pages = {1--13}, -title = {{The detailed structure and the onset of galaxy formation in low-mass gaseous dark matter haloes}}, -url = {http://arxiv.org/abs/2004.06124}, -volume = {13}, -year = {2020} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the LambdaCDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no statistically significant detection of a stellar halo, as in the case of M101, NGC3351 and NGC1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction f{\_}SH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming and assemble their dark matter halos on average earlier than galaxies with similar stellar masses. Accreted satellites are also lower in stellar mass and have earlier infall times than centrals with high f{\_}SH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretion-dominated r{\$\sim${}}45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers only at higher redshifts and evolved relatively unperturbed in the last {\$\sim${}}10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M and Sales, Laura V and Creasey, Peter and Cooper, Michael C and Bullock, James S and {Michael Rich}, R and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/19158792}, -volume = {457}, -year = {2009} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of stellar parameters and abundances ("stellar labels") for hundreds of thousands of stars; this poses a formidable spectral modeling challenge. In many cases, there is a subset of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the "known" labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with and as the labels, and then applying it to the spectra of 55,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one-ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ness, M and Hogg, David W and Rix, H W and Ho, Anna Y Q and Zasowski, G}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{THE CANNON: A DATA-DRIVEN APPROACH to STELLAR LABEL DETERMINATION}}, -volume = {808}, -year = {2015} -} -@article{PASJEditionalOffice2015, -abstract = {We present the results from the Suzaku satellite of the surrounding region of a galaxy clus-ter, A2744, at z = 0.3. To search for oxygen emission lines from the warm-hot intergalactic medium (WHIM), we analyzed X-ray spectra from two northeast regions 2.2–3.3 and 3.3– 4.4 Mpc from the center of the cluster, which offers the first test on the presence of a WHIM near the typical accretion shock radius (∼ 2r 200) predicted by hydrodynamical simulations. For the 2.2–3.3 Mpc region, the spectral fit significantly (99.2{\%} significance) improved when we include O VII and O VIII lines in the spectral model. A comparable WHIM surface bright-ness was obtained in the 3.3–4.4 Mpc region and the redshift of O VIII line is consistent with z = 0.3 within errors. The present results support that the observed soft X-ray emission orig-inated from the WHIM. However, considering both statistical and systematic uncertainties, O VIII detection in the northeast regions was marginal. The surface brightness of the O VIII line in 10 −7 photons cm −2 s −1 arcmin −2 was measured to be 2.7 ± 1.0, 2.1 ± 1.2 for the 2.2–3.3, 3.3– 4.4 Mpc regions, giving the upper limit on the baryon overdensity of $\delta$ = 319({\textless} 443), 283({\textless} 446), respectively. This is comparable with previous observations of cluster outskirts and their the-oretical predictions. The future prospect for WHIM detection using the Athena X-IFU micro-calorimeter is briefly discussed here. In addition, we also derived the ICM temperature distri-bution of A2744 to detect a clear discontinuity at the location of the radio relic. This suggests that the cluster has undergone strong shock heating by mass accretion along the filament.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1702.02157v1}, -author = {Hattori, Shiho and Ota, Naomi and Zhang, Yu-Ying and Akamatsu, Hiroki and Finoguenov, Alexis}, -doi = {10.1093/pasj/xxx000}, -eprint = {arXiv:1702.02157v1}, -journal = {Publ. Astron. Soc. Japan}, -keywords = {clusters,cosmology,galaxies,individual (Abell 2744) — X-rays}, -number = {0}, -pages = {1--9}, -title = {{arXiv:1702.02157v1 [astro-ph.HE] 7 Feb 2017}}, -volume = {00}, -year = {2014} -} -@article{James2018, -abstract = {We present the first spatially resolved rest-frame ultraviolet (UV) study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z = 2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each {\$\sim${}}4-8 kpc2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with C III] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. Themapped C III] emission shows distinct kinematical structure, with velocity offsets of {\$\sim${}}±50 km s-1 between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionization parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing in the range -200 ≲ v (km s-1) ≲ -50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star formation rates remain relatively constant ({\$\sim${}}8-16M⊙ yr-1), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced.We measure electron densities with a range of log (Ne)= 3.92-4.36 cm-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large-scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially resolved rest-frame UV studies expected with future observatories, such as James Webb Space Telescope.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L and Auger, Matt and Pettini, Max and Stark, Daniel P and Belokurov, V and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Dynesty, -abstract = {We present dynesty, a public, open-source, python package to estimate Bayesian posteriors and evidences (marginal likelihoods) using the dynamic nested sampling methods developed by Higson et al. By adaptively allocating samples based on posterior structure, dynamic nested sampling has the benefits of Markov chain Monte Carlo (MCMC) algorithms that focus exclusively on posterior estimation while retaining nested sampling's ability to estimate evidences and sample from complex, multimodal distributions. We provide an overview of nested sampling, its extension to dynamic nested sampling, the algorithmic challenges involved, and the various approaches taken to solve them in this and previous work. We then examine dynesty's performance on a variety of toy problems along with several astronomical applications. We find in particular problems dynesty can provide substantial improvements in sampling efficiency compared to popular MCMC approaches in the astronomical literature. More detailed statistical results related to nested sampling are also included in the appendix.}, -archivePrefix = {arXiv}, -arxivId = {1904.02180}, -author = {Speagle, Joshua S}, -doi = {10.1093/mnras/staa278}, -eprint = {1904.02180}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {data analysis,methods,statistical}, -number = {3}, -pages = {3132--3158}, -title = {{dynesty: a dynamic nested sampling package for estimating Bayesian posteriors and evidences}}, -volume = {493}, -year = {2020} -} -@article{LSSTDarkEnergyScienceCollaboration2012, -abstract = {This white paper describes the LSST Dark Energy Science Collaboration (DESC), whose goal is the study of dark energy and related topics in fundamental physics with data from the Large Synoptic Survey Telescope (LSST). It provides an overview of dark energy science and describes the current and anticipated state of the field. It makes the case for the DESC by laying out a robust analytical framework for dark energy science that has been defined by its members and the comprehensive three-year work plan they have developed for implementing that framework. The analysis working groups cover five key probes of dark energy: weak lensing, large scale structure, galaxy clusters, Type Ia supernovae, and strong lensing. The computing working groups span cosmological simulations, galaxy catalogs, photon simulations and a systematic software and computational framework for LSST dark energy data analysis. The technical working groups make the connection between dark energy science and the LSST system. The working groups have close linkages, especially through the use of the photon simulations to study the impact of instrument design and survey strategy on analysis methodology and cosmological parameter estimation. The white paper describes several high priority tasks identified by each of the 16 working groups. Over the next three years these tasks will help prepare for LSST analysis, make synergistic connections with ongoing cosmological surveys and provide the dark energy community with state of the art analysis tools. Members of the community are invited to join the LSST DESC, according to the membership policies described in the white paper. Applications to sign up for associate membership may be made by submitting the Web form at http://www.slac.stanford.edu/exp/lsst/desc/signup.html with a short statement of the work they wish to pursue that is relevant to the LSST DESC.}, -archivePrefix = {arXiv}, -arxivId = {1211.0310}, -author = {{LSST Dark Energy Science Collaboration}}, -eprint = {1211.0310}, -journal = {arXiv preprint arXiv:1211.0310}, -keywords = {Astrophysics - Cosmology and Extragalactic Astroph,High Energy Physics - Experiment}, -pages = {133}, -title = {{Large Synoptic Survey Telescope: Dark Energy Science Collaboration}}, -url = {http://arxiv.org/abs/1211.0310}, -year = {2012} -} -@article{Version2018, -abstract = {We perform a systematic search for sub-parsec binary supermassive black holes (BHs) in normal broad-line quasars at z {\textless} 0.8, using multi-epoch Sloan Digital Sky Survey (SDSS) spectroscopy of the broad H$\beta$ line. Our working model is that (1) one and only one of the two BHs in the binary is active; (2) the active BH dynamically dominates its own broad-line region (BLR) in the binary system, so that the mean velocity of the BLR reflects the mean velocity of its host BH; (3) the inactive companion BH is orbiting at a distance of a few R BLR, where R BLR 0.01-0.1 pc is the BLR size. We search for the expected line-of-sight acceleration of the broad-line velocity from binary orbital motion by cross-correlating SDSS spectra from two epochs separated by up to several years in the quasar rest frame. Out of 00 pairs of spectra for which we have good measurements of the velocity shift between two epochs (1$\sigma$ error 0 km s-1), we detect 28 systems with significant velocity shifts in broad H$\beta$, among which 7 are the best candidates for the hypothesized binaries, 4 are most likely due to broad-line variability in single BHs, and the rest are ambiguous. Continued spectroscopic observations of these candidates will easily strengthen or disprove these claims. We use the distribution of the observed accelerations (mostly non-detections) to place constraints on the abundance of such binary systems among the general quasar population. Excess variance in the velocity shift is inferred for observations separated by longer than 0.4 yr (quasar rest frame). Attributing all the excess to binary motion would imply that most of the quasars in this sample must be in binaries, that the inactive BH must be on average more massive than the active one, and that the binary separation is at most a few times the size of the BLR. However, if this excess variance is partly or largely due to long-term broad-line variability, the requirement of a large population of close binaries is much weakened or even disfavored for massive companions. Future time-domain spectroscopic surveys of normal quasars can provide vital prior information on the structure function of stochastic velocity shifts induced by broad-line variability in single BHs. Such surveys with improved spectral quality, increased time baseline, and more epochs can greatly improve the statistical constraints of this method on the general binary population in broad-line quasars, further shrink the allowed binary parameter space, and detect true sub-parsec binaries. {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1306.4330}, -author = {Shen, Yue and Liu, Xin and Loeb, Abraham and Tremaine, Scott}, -doi = {10.1088/0004-637X/775/1/49}, -eprint = {1306.4330}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {black hole physics,galaxies: active,line: profiles,quasars: general,surveys}, -number = {1}, -title = {{Constraining sub-parsec binary supermassive black holes in quasars with multi-epoch spectroscopy. I. the general quasar population}}, -volume = {775}, -year = {2013} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since z = 1.0. We find that lower mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher mass or lower redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single-aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys; we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1824--1848}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {469}, -year = {2017} -} -@article{Naab2007, -abstract = {We describe high-resolution smoothed particle hydrodynamics (SPH) simulations of three approximately M* field galaxies starting from $\Lambda$CDM initial conditions. The simulations are made intentionally simple, and include photoionization, cooling of the intergalactic medium, and star formation, but not feedback from AGNs or supernovae. All of the galaxies undergo an initial burst of star formation at z{\$\sim${}}5, accompanied by the formation of a bubble of heated gas. Two out of three galaxies show early-type properties at present, whereas only one of them experienced a major merger. Heating from shocks and PdV work dominates over cooling so that for most of the gas the temperature is an increasing function of time. By z{\$\sim${}}1 a significant fraction of the final stellar system is in place and the spectral energy distribution resembles those of observed massive red galaxies. The galaxies have grown from z=1--{\textgreater}0 on average by 25{\%} in mass and in size by gas-poor (dry) stellar mergers. By the present day the simulated galaxies are old ({\$\sim${}}10 Gyr), kinematically hot stellar systems surrounded by hot gaseous haloes. Stars dominate the mass of the galaxies up to {\$\sim${}}4 effective radii ({\$\sim${}}10 kpc). Kinematic and most photometric properties are in good agreement with those of observed elliptical galaxies. The galaxy with a major merger develops a counter-rotating core. Our simulations show that realistic intermediate-mass giant elliptical galaxies with plausible formation histories can be formed from $\Lambda$CDM initial conditions even without requiring recent major mergers or feedback from supernovae or AGNs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0512235}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P and Efstathiou, George}, -doi = {10.1086/510841}, -eprint = {0512235}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {710--720}, -primaryClass = {astro-ph}, -title = {{Formation of Early‐Type Galaxies from Cosmological Initial Conditions}}, -url = {http://stacks.iop.org/0004-637X/658/i=2/a=710}, -volume = {658}, -year = {2007} -} -@article{More2012, -abstract = {We have presented the Strong Lensing Legacy Survey-ARCS (SARCS) sample compiled from the T0006 data release of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) covering a total non-overlapping area of 159 deg 2. We have adopted a semi-automatic method to find gravitational arcs in the survey that makes use of an arc-finding algorithm. The SARCS sample consists of 127 lens candidates, out of which, 54 systems are promising lenses. From our sample, we have detected a systematic alignment of the giant arcs with the major axis of the baryonic component of the putative lens in concordance with previous studies. This alignment is also observed for all arcs in the sample and does not vary significantly with increasing arc radius. Owing to the large area and depth of the CFHTLS, we have found the largest sample of lenses probing mass scales that are intermediate to cluster and galaxy lenses for the first time. We have compared the observed image separation distribution (ISD) of our arcs with theoretical models. A two-component density profile for the lenses, which accounts for both the central galaxy and the dark matter component is required by the data to explain the observed ISD. Unfortunately, current levels of uncertainties and degeneracies accommodate models both with and without adiabatic contraction. We have also shown the effects of changing parameters of the model that predict the ISD and that a larger lens sample might constrain relations such as the concentration-mass relation, mass-luminosity relation and the faint-end slope of the luminosity function. {\textcopyright} Published under licence by IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1109.1821}, -author = {More, A. and Cabanac, R. and More, S. and Alard, C. and Limousin, M. and Kneib, J. P. and Gavazzi, R. and Motta, V.}, -doi = {10.1088/1742-6596/484/1/012041}, -eprint = {1109.1821}, -issn = {17426596}, -journal = {Journal of Physics: Conference Series}, -keywords = {dark matter,ethods: data analysis,gravitational lensing: strong,surveys}, -month = {apr}, -number = {1}, -pages = {38}, -pmid = {12345678}, -title = {{The CFHTLS-Strong Lensing Legacy Survey (SL2S): Investigating the group-scale lenses with the SARCS sample}}, -url = {http://arxiv.org/abs/1109.1821}, -volume = {484}, -year = {2014} -} -@article{Geometryej, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Eales1999, -abstract = {We present the first results of a deep unbiased submillimetre survey carried out at 450 and 850 microns. We detected 12 sources at 850 microns, giving a surface density of sources with 850-micron flux densities > 2.8mJy of of 0.49+-0.16 per square arcmin. The sources constitute 20-30% of the background radiation at 850 microns and thus a significant fraction of the entire background radiation produced by stars. This implies, through the connection between metallicity and background radiation, that a significant fraction of all the stars that have ever been formed were formed in objects like those detected here. The combination of their large contribution to the background radiation and their extreme bolometric luminosities make these objects excellent candidates for being proto-ellipticals. Optical astronomers have recently shown that the UV-luminosity density of the universe increases by a factor of about 10 between z=0 and z=1 and then decreases again at higher redshifts. Using the results of a parallel submillimetre survey of the local universe, we show that both the submillimetre source density and background can be explained if the submillimetre luminosity density evolves in a similar way to the UV-luminosity density. Thus, if these sources are ellipticals in the process of formation, they may be forming at relatively modest redshifts.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9808040}, -author = {Eales, Stephen and Lilly, Simon and Gear, Walter and Dunne, Loretta and Bond, J. Richard and Hammer, Francois and {Le Fevre}, Olivier and Crampton, David}, -doi = {10.1086/307069}, -eprint = {9808040}, -isbn = {9780473203641}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {518--524}, -pmid = {17121902}, -primaryClass = {astro-ph}, -title = {{The Canada‐UK Deep Submillimeter Survey: First Submillimeter Images, the Source Counts, and Resolution of the Background}}, -url = {http://stacks.iop.org/0004-637X/515/i=2/a=518}, -volume = {515}, -year = {1999} -} -@article{Hopkins2011, -abstract = {We present analytic calculations of angular momentum transport and gas inflow in galaxies, from scales of {\$\sim${}}kpc to deep inside the potential of a central massive black hole (BH). We compare these analytic calculations to numerical simulations and use them to develop a sub-grid model of BH growth that can be incorporated into semi-analytic calculations or cosmological simulations. Motivated by both analytic calculations and simulations of gas inflow in galactic nuclei, we argue that the strongest torque on gas arises when non-axisymmetric perturbations to the stellar gravitational potential produce orbit crossings and shocks in the gas. This is true both at large radii {\$\sim${}}0.01-1kpc, where bar-like stellar modes dominate the non-axisymmetric potential, and at smaller radii ≲10pc, where a lopsided/eccentric stellar disc dominates. The traditional orbit-crossing criterion is not always adequate to predict the locations of, and inflow due to, shocks in gas+stellar discs with finite sound speeds. We derive a modified criterion that predicts the presence of shocks in stellar-dominated systems even absent formal orbit crossing. We then derive analytic expressions for the loss of angular momentum and the resulting gas inflow rates in the presence of such shocks. We test our analytic predictions using hydrodynamic simulations at a range of galactic scales, and show that they successfully predict the mass inflow rates and quasi-steady gas surface densities with a small scatter ≃0.3dex. We use our analytic results to construct a new estimate of the BH accretion rate given galaxy properties at larger radii, for use in galaxy and cosmological simulations and semi-analytic models. While highly simplified, this accretion rate predictor captures the key scalings in the numerical simulations. By contrast, alternate estimates such as the local viscous accretion rate or the spherical Bondi rate fail systematically to reproduce the simulations and have significantly larger scatter. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1007.2647}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1365-2966.2011.18542.x}, -eprint = {1007.2647}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Quasars: general}, -number = {2}, -pages = {1027--1050}, -title = {{An analytic model of angular momentum transport by gravitational torques: From galaxies to massive black holes}}, -volume = {415}, -year = {2011} -} -@article{Geometryeo, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Maresca2022, -abstract = {We present modelling of ∼0.1 arcsec resolution Atacama Large Millimetre/submillimetre Array imaging of seven strong gravitationally lensed galaxies detected by the Herschel Space Observatory. Four of these systems are galaxy-galaxy strong lenses, with the remaining three being group-scale lenses. Through careful modelling of visibilities, we infer the mass profiles of the lensing galaxies and by determining the magnification factors, we investigate the intrinsic properties and morphologies of the lensed submillimetre sources. We find that these submillimetre sources all have ratios of star formation rate to dust mass that are consistent with, or in excess of, the mean ratio for high-redshift submillimetre galaxies and low redshift ultra-luminous infrared galaxies. Reconstructions of the background sources reveal that the majority of our sample display disturbed morphologies. The majority of our lens models have mass density slopes close to isothermal, but some systems show significant differences.}, -archivePrefix = {arXiv}, -arxivId = {2111.09680}, -author = {Maresca, Jacob and Dye, Simon and Amvrosiadis, Aristeidis and Bendo, George and Cooray, Asantha and {De Zotti}, Gianfranco and Dunne, Loretta and Eales, Stephen and Furlanetto, Cristina and Gonz{\'{a}}lez-Nuevo, Joaquin and Greener, Michael and Ivison, Robert and Lapi, Andrea and Negrello, Mattia and Riechers, Dominik and Serjeant, Stephen and Tergolina, M{\^{o}}nica and Wardlow, Julie}, -doi = {10.1093/mnras/stac585}, -eprint = {2111.09680}, -file = {:C\:/Users/Jammy/Documents/Papers/PyAutoLens/Maresca2021ALMAFunctionality.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {galaxies: structure,gravitational lensing: strong}, -number = {2}, -pages = {2426--2438}, -title = {{Modelling high-resolution ALMA observations of strongly lensed dusty star-forming galaxies detected by Herschel}}, -volume = {512}, -year = {2022} -} -@article{Rybak2015, -abstract = {We present a sub-100 pc-scale analysis of the CO molecular gas emission and kinematics of the gravitational lens system SDP.81 at redshift 3.042 using Atacama Large Millimetre/submillimetre Array (ALMA) science verification data and a visibility-plane lens reconstruction technique. We find clear evidence for an excitation-dependent structure in the unlensed molecular gas distribution, with emission in CO (5-4) being significantly more diffuse and structured than in CO (8-7). The intrinsic line luminosity ratio is r8-7/5-4=0.30± 0.04, which is consistent with other low-excitation starbursts at z $\sim$ 3. An analysis of the velocity fields shows evidence for a star-forming disc with multiple velocity components that is consistent with a merger/post-coalescence merger scenario, and a dynamical mass of M(<1.56 kpc)=1.6±0.6×1010 M⊙. Source reconstructions from ALMA and the Hubble Space Telescope show that the stellar component is offset from the molecular gas and dust components. Together with Karl G. Jansky Very Large Array CO (1-0) data, they provide corroborative evidence for a complex $\sim$ 2kpc-scale starburst that is embedded within a larger $\sim$ 15kpc structure.}, -archivePrefix = {arXiv}, -arxivId = {1506.01425}, -author = {Rybak, M. and Vegetti, S. and McKean, J. P. and Andreani, P. and White, S. D.M.}, -doi = {10.1093/mnrasl/slv092}, -eprint = {1506.01425}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Galaxies: high redshift,Gravitational lensing: strong,Submillimetre: galaxies}, -number = {1}, -pages = {L26--L30}, -title = {{ALMA imaging of SDP.81-II. A pixelated reconstruction of the CO emission lines}}, -volume = {453}, -year = {2015} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright} 2009 The American Astronomical Society. All rights reserved.}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel, Sari, Ceverino - 2009 - Formation of massive galaxies at high redshift Cold streams, clumpy disks, and compact spheroids(2).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Pourrahmani2018, -abstract = {In this work, we present our machine learning classification algorithm for identifying strong gravitational lenses from wide-area surveys using convolutional neural networks; LensFlow . We train and test the algorithm using a wide variety of strong gravitational lens configurations from simulations of lensing events. Images are processed through multiple convolutional layers that extract feature maps necessary to assign a lens probability to each image. LensFlow provides a ranking scheme for all sources that could be used to identify potential gravitational lens candidates by significantly reducing the number of images that have to be visually inspected. We apply our algorithm to the HST /ACS i-band observations of the COSMOS field and present our sample of identified lensing candidates. The developed machine learning algorithm is more computationally efficient and complimentary to classical lens identification algorithms and is ideal for discovering such events across wide areas from current and future surveys such as LSST and WFIRST .}, -archivePrefix = {arXiv}, -arxivId = {1705.05857}, -author = {Pourrahmani, Milad and Nayyeri, Hooshang and Cooray, Asantha}, -doi = {10.3847/1538-4357/aaae6a}, -eprint = {1705.05857}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Pourrahmani2017LensExtractor.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {data analysis,gravitational lensing,image processing,methods,strong,techniques}, -number = {1}, -pages = {68}, -title = {{LensFlow: A Convolutional Neural Network in Search of Strong Gravitational Lenses}}, -volume = {856}, -year = {2018} -} -@article{Leauthaud2017, -abstract = {We present high signal-to-noise galaxy-galaxy lensing measurements of the Baryon Oscillation Spectroscopic Survey constant mass (CMASS) sample using 250 deg2 of weak-lensing data from Canada-France-Hawaii Telescope Lensing Survey and Canada-France-Hawaii Telescope Stripe 82 Survey. We compare this signal with predictions from mock catalogues trained to match observables including the stellar mass function and the projected and twodimensional clustering of CMASS. We show that the clustering of CMASS, together with standard models of the galaxy-halo connection, robustly predicts a lensing signal that is 20-40 per cent larger than observed. Detailed tests show that our results are robust to a variety of systematic effects. Lowering the value of S8 = $\sigma$8 √ $\Omega$m/0.3 compared to Planck Collaboration XIII reconciles the lensing with clustering. However, given the scale of our measurement (r < 10 h-1 Mpc), other effects may also be at play and need to be taken into consideration. We explore the impact of baryon physics, assembly bias, massive neutrinos and modifications to general relativity on $\Delta$$\Sigma$ and show that several of these effects may be non-negligible given the precision of our measurement. Disentangling cosmological effects from the details of the galaxy-halo connection, the effect of baryons, and massive neutrinos, is the next challenge facing joint lensing and clustering analyses. This is especially true in the context of large galaxy samples from Baryon Acoustic Oscillation surveys with precise measurements but complex selection functions.}, -archivePrefix = {arXiv}, -arxivId = {1611.08606}, -author = {Leauthaud, Alexie and Saito, Shun and Hilbert, Stefan and Barreira, Alexandre and More, Surhud and White, Martin and Alam, Shadab and Behroozi, Peter and Bundy, Kevin and Coupon, Jean and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Mandelbaum, Rachel and Miller, Lance and Moraes, Bruno and Pereira, Maria E.S. and Rodr{\'{i}}guez-Torres, Sergio A. and Schmidt, Fabian and Shan, Huan Yuan and Viel, Matteo and Villaescusa-Navarro, Francisco}, -doi = {10.1093/mnras/stx258}, -eprint = {1611.08606}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Leauthaud et al. - 2017 - Lensing is low Cosmology, galaxy formation or new physics(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {3}, -pages = {3024--3047}, -title = {{Lensing is low: Cosmology, galaxy formation or new physics?}}, -volume = {467}, -year = {2017} -} -@article{Martig2009, -abstract = {We point out a natural mechanism for quenching of star formation in early-type galaxies (ETGs). It automatically links the color of a galaxy with its morphology and does not require gas consumption, removal or termination of gas supply. Given that star formation takes place in gravitationally unstable gas disks, it can be quenched when a disk becomes stable against fragmentation to bound clumps. This can result from the growth of a stellar spheroid, for instance by mergers. We present the concept of morphological quenching (MQ) using standard disk instability analysis, and demonstrate its natural occurrence in a cosmological simulation using an efficient zoom-in technique. We show that the transition from a stellar disk to a spheroid can be sufficient to stabilize the gas disk, quench star formation, and turn an ETG red and dead while gas accretion continues. The turbulence necessary for disk stability can be stirred up by sheared perturbations within the disk in the absence of bound star-forming clumps. While other quenching mechanisms, such as gas stripping, active galactic nucleus feedback, virial shock heating, and gravitational heating are limited to massive halos, MQ can explain the appearance of red ETGs also in halos less massive than ∼ 1012 M ⊙. The dense gas disks observed in some of today's red ellipticals may be the relics of this mechanism, whereas red galaxies with quenched gas disks could be more frequent at high redshift. {\textcopyright} 2009. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0905.4669}, -author = {Martig, Marie and Bournaud, Fr{\'{e}}d{\'{e}}ric and Teyssier, Romain and Dekel, Avishai}, -doi = {10.1088/0004-637X/707/1/250}, -eprint = {0905.4669}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation}, -month = {dec}, -number = {1}, -pages = {250--267}, -pmid = {15927618}, -title = {{Morphological quenching of star formation: Making early-type galaxies red}}, -url = {http://stacks.iop.org/0004-637X/707/i=1/a=250?key=crossref.e16a49e629b633bd010bf08856fa4c85}, -volume = {707}, -year = {2009} -} -@article{Kuhlen2007, -abstract = {We present a study of the shapes, orientations, and alignments of Galactic dark matter subhalos in the ``Via Lactea'' simulation of a Milky Way-size LCDM host halo. Whereas isolated dark matter halos tend to be prolate, subhalos are predominantly triaxial. Overall subhalos are more spherical than the host halo, with minor to major and intermediate to major axis ratios of 0.68 and 0.83, respectively. Like isolated halos, subhalos tend to be less spherical in their central regions. The principal axis ratios are independent of subhalo mass, when the shapes are measured within a physical scale like r_Vmax, the radius of the peak of the circular velocity curve. Subhalos tend to be slightly more spherical closer to the host halo center. The spatial distribution of the subhalos traces the prolate shape of the host halo when they are selected by the largest V_max they ever had, i.e. before they experienced strong tidal mass loss. The subhalos' orientation is not random: the major axis tends to align with the direction towards the host halo center. This alignment disappears for halos beyond 3 r_200 and is more pronounced when the shapes are measured in the outer regions of the subhalos. The radial alignment is preserved during a subhalo's orbit and they become elongated during pericenter passage, indicating that the alignment is likely caused by the host halo's tidal forces. These tidal interactions with the host halo act to make subhalos rounder over time.}, -archivePrefix = {arXiv}, -arxivId = {0705.2037}, -author = {Kuhlen, Michael and Diemand, Jurg and Madau, Piero}, -doi = {10.1086/522878}, -eprint = {0705.2037}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {1135--1146}, -title = {{The Shapes, Orientation, and Alignment of Galactic Dark Matter Subhalos}}, -url = {http://stacks.iop.org/0004-637X/671/i=2/a=1135}, -volume = {671}, -year = {2007} -} -@article{Costantin2017, -abstract = {Context. The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. Aims. We aim to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. Methods. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the i-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new (B=A, C=A) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. Results. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations of 25° ≤ $\theta$ ≤ 65° we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66{\%}), with a smaller fraction of prolate spheroids (19{\%}), and triaxial ellipsoids (15{\%}). The majority of triaxial bulges are in barred galaxies (75{\%}). Moreover, we found that bulges with low S{\'{e}}rsic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, bulges in late-type galaxies or in less massive galaxies have no preference for being oblate, prolate, or triaxial. On the contrary, bulges with high S{\'{e}}rsic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. Conclusions. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L and M{\'{e}}ndez-Abreu, J and Corsini, E M and Eliche-Moral, M C and Tapia, T and Morelli, L and Elena, Dalla Bont{\`{a}} and Pizzella, A}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -volume = {609}, -year = {2018} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the 'Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a (100 cMpc)3 and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts 0 and 1, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar 'downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G. and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S. and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rosas-Guevara et al. - 2016 - Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Savorgnan2015, -abstract = {The S\'ersic $R^{1/n}$ model is the best approximation known to date for describing the light distribution of stellar spheroidal and disk components, with the S\'ersic index $n$ providing a direct measure of the central radial concentration of stars. The S\'ersic index of a galaxy's spheroidal component, $n_{sph}$, has been shown to tightly correlate with the mass of the central supermassive black hole, $M_{BH}$. The $M_{BH}-n_{sph}$ correlation is also expected from other two well known scaling relations involving the spheroid luminosity, $L_{sph}$: the $L_{sph}-n_{sph}$ and the $M_{BH}-L_{sph}$. Obtaining an accurate estimate of the spheroid S\'ersic index requires a careful modelling of a galaxy's light distribution and some studies have failed to recover a statistically significant $M_{BH}-n_{sph}$ correlation. With the aim of re-investigating the $M_{BH}-n_{sph}$ and other black hole mass scaling relations, we performed a detailed (i.e.$\sim$bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, that had been imaged at $3.6\rm\sim\mu m$ with Spitzer. In this paper, the third of this series, we present an analysis of the $L_{sph}-n_{sph}$ and $M_{BH}-n_{sph}$ diagrams. While early-type (elliptical+lenticular) and late-type (spiral) galaxies split into two separate relations in the $L_{sph}-n_{sph}$ and $M_{BH}-L_{sph}$ diagrams, they reunite into a single $M_{BH} \propto n_{sph}^{3.39 \pm 0.15}$ sequence with relatively small intrinsic scatter ($\epsilon \simeq 0.25 \rm\simdex$). The black hole mass appears to be closely related to the spheroid central concentration of stars, which mirrors the inner gradient of the spheroid gravitational potential.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1603.01910}, -author = {Savorgnan, Giulia A. D.}, -doi = {10.3847/0004-637x/821/2/88}, -eprint = {1603.01910}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Savorgnan - 2016 - SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE M BH – n sph CORRELATION.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {88}, -title = {{ SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE M BH – n sph CORRELATION }}, -url = {http://arxiv.org/abs/1603.01910%0Ahttp://dx.doi.org/10.3847/0004-637X/821/2/88}, -volume = {821}, -year = {2016} -} -@article{Wang2017, -abstract = {Difference imaging or image subtraction is a method that measures differential photometry by matching the pointing and point-spread function (PSF) between image frames. It is used for the detection of time-variable phenomena. Here we present a new category of method---CPM Difference Imaging, in which differences are not measured between matched images but instead between image frames and a data-driven predictive model that has been designed only to predict the pointing, PSF, and detector effects but not astronomical variability. In CPM Difference Imaging each pixel is modelled by the Causal Pixel Model (CPM) originally built for modeling Kepler data, in which pixel values are predicted by a linear combination of other pixels at the same epoch but far enough away such that these pixels are causally disconnected, astrophysically. It does not require that the user have any explicit model or description of the pointing or point-spread function of any of the images. Its principal drawback is that---in its current form---it requires an imaging campaign with many epochs and fairly stable telescope pointing. The method is applied to simulated data and also the K2 Campaign 9 microlensing data. We show that CPM Difference Imaging can detect variable objects and produce precise differentiate photometry in a crowded field. CPM Difference Imaging is capable of producing image differences at nearly photon-noise precision.}, -archivePrefix = {arXiv}, -arxivId = {1710.02428}, -author = {Wang, Dun and Hogg, David W. and Foreman-Mackey, Daniel and Sch{\"{o}}lkopf, Bernhard}, -eprint = {1710.02428}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2017 - A pixel-level model for event discovery in time-domain imaging.pdf:pdf}, -pages = {1--23}, -title = {{A pixel-level model for event discovery in time-domain imaging}}, -url = {http://arxiv.org/abs/1710.02428}, -year = {2017} -} -@article{Zibetti2020, -abstract = {We perform spatially resolved stellar population analysis for a sample of 69 early-type galaxies (ETGs) from the CALIFA integral field spectroscopic survey, including 48 ellipticals and 21 S0's. We generate and quantitatively characterize profiles of light-weighted mean stellar age and metallicity within ≲2Re, as a function of radius and stellar-mass surface density $\mu$*. We study in detail the dependence of profiles on galaxies' global properties, including velocity dispersion $\sigma$e, stellar mass, morphology. ETGs are universally characterized by strong, negative metallicity gradients ($\sim \!-0.3\, \text{dex}$ per Re) within 1Re, which flatten out moving towards larger radii. A quasi-universal local $\mu$*–metallicity relation emerges, which displays a residual systematic dependence on $\sigma$e, whereby higher $\sigma$e implies higher metallicity at fixed $\mu$*. Age profiles are typically U-shaped, with minimum around 0.4 Re, asymptotic increase to maximum ages beyond $\sim 1.5\, $Re, and an increase towards the centre. The depth of the minimum and the central increase anticorrelate with $\sigma$e. A possible qualitative interpretation of these observations is a two-phase scenario. In the first phase, dissipative collapse occurs in the inner 1Re, establishing a negative metallicity gradient. The competition between the outside-in quenching due to feedback-driven winds and some form of inside-out quenching, possibly caused by central AGN feedback or dynamical heating, determines the U-shaped age profiles. In the second phase, the accretion of ex-situ stars from quenched and low-metallicity satellites shapes the flatter stellar population profiles in the outer regions.}, -archivePrefix = {arXiv}, -arxivId = {1906.02209}, -author = {Zibetti, Stefano and Gallazzi, Anna R and Hirschmann, Michaela and Consolandi, Guido and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and van de Ven, Glenn and Lyubenova, Mariya}, -doi = {10.1093/mnras/stz3205}, -eprint = {1906.02209}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Zibetti et al. - 2020 - Insights into formation scenarios of massive early-type galaxies from spatially resolved stellar population anal.pdf:pdf}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {abundances,cd,elliptical and lenticular,evolution,formation,galax-,galaxies,ies,imaging,stellar content,techniques}, -number = {3}, -pages = {3562--3585}, -title = {{Insights into formation scenarios of massive early-type galaxies from spatially resolved stellar population analysis in CALIFA}}, -volume = {491}, -year = {2020} -} -@article{Swinbank2015, -abstract = {We exploit long baseline ALMA submillimeter observations of the lensed star-forming galaxy SDP 81 at z = 3.042 to investigate the properties of the interstellar medium (ISM) on scales of 50-100 pc. The kinematics of the 12CO gas within this system are well described by a rotationally supported disk with an inclination-corrected rotation speed, vrot = 320 ± 20 km s-1, and a dynamical mass of Mdyn= (3.5 ± 1.0)× 1010 within a radius of 1.5 kpc. The disk is gas-rich and unstable, with a Toomre parameter, Q = 0.30 ± 0.10, and so into star-forming regions with Jeans length LJ∼130 pc. We identify five star-forming regions within the ISM on these scales and show that their scaling relations between luminosity, line widths, and sizes are significantly offset from those typical of molecular clouds in local galaxies (Larson's relations). These offsets are likely to be caused by the high external hydrostatic pressure for the ISM, Ptot/KB∼ 40-20+30 × 107 K cm-3, which is ∼104× higher than the typical ISM pressure in the Milky Way. The physical conditions of the star-forming ISM and giant molecular clouds appear to be similar to those found in the densest environments in the local universe, such as those in the Galactic center.}, -archivePrefix = {arXiv}, -arxivId = {1505.05148}, -author = {Swinbank, A. M. and Dye, S. and Nightingale, J. W. and Furlanetto, C. and Smail, Ian and Cooray, A. and Dannerbauer, H. and Dunne, L. and Eales, S. and Gavazzi, R. and Hunter, T. and Ivison, R. J. and Negrello, M. and Oteo-Gomez, I. and Smit, R. and Werf, P. Van Der and Vlahakis, C.}, -doi = {10.1088/2041-8205/806/1/L17}, -eprint = {1505.05148}, -issn = {20418213}, -journal = {Astrophysical Journal Letters}, -keywords = {evolution,galaxies: high-redshift,galaxies: starburst}, -number = {1}, -pages = {L17}, -title = {{ALMA resolves the properties of star-forming regions in a dense gas disk at z ∼ 3}}, -url = {http://stacks.iop.org/2041-8205/806/i=1/a=L17?key=crossref.1b0d809c74a12e05028991e4a510e0b6%5Cnhttp://adsabs.harvard.edu/abs/2015ApJ...806L..17S}, -volume = {806}, -year = {2015} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ({\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashgamma{\}}{\$}), we find that, although the zero cosmic curvature is still included within {\$}2 \backslashsigma{\$} confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile {\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashalpha{\}}{\$} to be different from that of the total-mass density profile {\$}\backslashnu\backslashsim r{\^{}}{\{}-\backslashdelta{\}}{\$}, a weaker constraint on the curvature ({\$}\backslashOmega{\_}k{\textless}0.197{\$} at 68$\backslash${\%} confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of {\$}\backslashDelta \backslashOmega{\_}k\backslashsimeq 10{\^{}}{\{}-3{\}}{\$}, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{Sonnenfeld2013c, -abstract = {We present optical and near-infrared spectroscopy obtained at Keck, Very Large Telescope, and Gemini for a sample of 36 secure strong gravitational lens systems and 17 candidates identified as part of the Strong Lensing Legacy Survey. The deflectors are massive early-type galaxies in the redshift range zd = 0.2-0.8, while the lensed sources are at zs = 1-3.5. We combine these data with photometric and lensing measurements presented in the companion paper III and with lenses from the Sloan Lens Advanced Camera for Surveys and L{\`{e}}nses Structure and Dynamics surveys to investigate the cosmic evolution of the internal structure of massive early-type galaxies over half the age of the universe. We study the dependence of the slope of the total mass density profile, $\gamma$′ (), on stellar mass, size, and redshift. We find that two parameters are sufficient to determine $\gamma$′ with less than 6% residual scatter. At fixed redshift, $\gamma$′ depends solely on the surface stellar mass density ∂$\gamma$′/ ∂$\Sigma$* = 0.38 ± 0.07, i.e., galaxies with denser stars also have steeper slopes. At fixed M * and R eff, $\gamma$′ depends on redshift, in the sense that galaxies at a lower redshift have steeper slopes (∂$\gamma$′/∂z = -0.31 ± 0.10). However, the mean redshift evolution of $\gamma$′ for an individual galaxy is consistent with zero d$\gamma$′/dz = -0.10 ± 0.12. This result is obtained by combining our measured dependencies of $\gamma$′ on z, M *,R eff with the evolution of the R eff-M* taken from the literature, and is broadly consistent with current models of the formation and evolution of massive early-type galaxies. Detailed quantitative comparisons of our results with theory will provide qualitatively new information on the detailed physical processes at work. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1307.4759}, -author = {Sonnenfeld, Alessandro and Treu, Tommaso and Gavazzi, Rapha{\"{e}}l and Suyu, Sherry H. and Marshall, Philip J. and Auger, Matthew W. and Nipoti, Carlo}, -doi = {10.1088/0004-637X/777/2/98}, -eprint = {1307.4759}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,gravitational lensing: strong}, -number = {2}, -pages = {98}, -title = {{THE Sl2S Galaxy-scale lens sample. IV. the dependence of the total mass density profile of early-type galaxies on redshift, stellar mass, and size}}, -url = {http://arxiv.org/abs/1307.4759}, -volume = {777}, -year = {2013} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -month = {aug}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -volume = {370}, -year = {2006} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of Mstar{\textgreater}10{\^{}}11Msolar galaxies at 1{\textless}z{\textless}3 in the CANDELS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disk components according to their H(160)-band morphologies. By extending this analysis to multiple bands we have been able to conduct individual bulge and disk component SED fitting which has provided us with stellar-mass and star-formation rate estimates for the separate bulge and disk components. These have been combined with size measurements to explore the evolution of these massive high-redshift galaxies. By utilising the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the disks. This can be seen from both the fraction of bulge components which lie below the local relation and the median sizes of the bulge components, where the bulges are a median factor of 2.93+/-0.32 times smaller than similarly massive local galaxies at 1{\textless}z{\textless}2 and 3.41+/-0.58 smaller at 2{\textless}z{\textless}3; for the disks the corresponding factors are 1.65+/-0.14 and 1.99+/-0.25. Moreover, by splitting our sample into the passive and star-forming bulge and disk sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming disks are larger, while the passive disks have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-Sersic fits and adopting the overall star-formation rates. Finally, by evolving the star-formation histories of the passive disks back to the redshifts when the passive disks were last active, we show that the passive and star-forming disks have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.5221}, -volume = {444}, -year = {2014} -} -@article{Reynolds2015, -abstract = {Compact radio sources sometimes exhibit intervals of large, rapid changes in their flux-density, due to lensing by interstellar plasma crossing the line-of-sight. A novel survey program has made it possible to discover these "Extreme Scattering Events" (ESEs) in real time, resulting in a high-quality dynamic spectrum of an ESE observed in PKS 1939-315. Here we present a method for determining the column-density profile of a plasma lens, given only the dynamic radio spectrum of the lensed source, under the assumption that the lens is either axisymmetric or totally anisotropic. Our technique relies on the known, strong frequency dependence of the plasma refractive index in order to determine how points in the dynamic spectrum map to positions on the lens. We apply our method to high-frequency (4.2-10.8 GHz) data from the Australia Telescope Compact Array of the PKS 1939-315 ESE. The derived electron column-density profiles are very similar for the two geometries we consider, and both yield a good visual match to the data. However, the fit residuals are substantially above the noise level, and deficiencies are evident when we compare the predictions of our model to lower-frequency (1.6-3.1 GHz) data on the same ESE, thus motivating future development of more sophisticated inversion techniques.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1512.03411}, -author = {Tuntsov, Artem V and Walker, Mark A and Koopmans, Leon V E and Bannister, Keith W and Stevens, Jamie and Johnston, Simon and Reynolds, Cormac and Bignall, Hayley E}, -doi = {10.3847/0004-637x/817/2/176}, -eprint = {1512.03411}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {176}, -title = {{Dynamic Spectral Mapping of Interstellar Plasma Lenses}}, -url = {http://arxiv.org/abs/1512.03411%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/2/176}, -volume = {817}, -year = {2016} -} -@article{Murray2013a, -abstract = {Pocket-pumping is an established technique for identifying the locations of charge trapping sites within the transport channels of CCDs. Various parameters of the pumping process can be manipulated to increase the efficiency, or allow characterisation of the trap sites effective during nominal operating modes. A CCD273 was irradiated in a triangular region by protons to a 10 MeV equivalent fluence of 1.2E9 p.cm-2, ensuring a suitably low trap density for the development of an automated trap recognition algorithm. X-rays of 5, 898 eV were incident on the CCD above the region irradiated with the triangle, such that events could be analysed having passed through an increasing length of irradiated silicon and hence number of trapping sites as a function of column number. Here we present the relationship between the number of traps identified by pocket pumping within the parallel transport channels of a CCD273 and the amount of signal that is deferred by the trapping process during readout. {\textcopyright}2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Hall, David and Holland, Andrew D}, -doi = {10.1117/12.2024826}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {ccd,cic,cte,eper,euclid vis,fpr,multi-level,pocket pumping,trap pumping,tri-level}, -number = {0}, -pages = {88600H}, -title = {{The relationship between pumped traps and signal loss in buried channel CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024826}, -volume = {8860}, -year = {2013} -} -@article{LeFloch2005, -abstract = {We analyze a sample of {\$\sim${}}2600 MIPS/Spitzer 24mic sources brighter than {\$\sim${}}80muJy and located in the Chandra Deep Field South to characterize the evolution of the comoving infrared (IR) energy density of the Universe up to z{\$\sim${}}1. Using published ancillary optical data we first obtain a nearly complete redshift determination for the 24mic objects associated with R{\textless}24 counterparts at z{\textless}1. We find that the 24mic population at 0.5{\textless}z{\textless}1 is dominated by ``Luminous Infrared Galaxies'' (i.e., 10{\^{}}11 L{\_}sol {\textless} L{\_}IR {\textless} 10{\^{}}12 L{\_}sol), the counterparts of which appear to be also luminous at optical wavelengths and tend to be more massive than the majority of optically-selected galaxies. We finally derive 15mic and total IR luminosity functions (LFs) up to z{\$\sim${}}1. In agreement with the previous results from ISO and SCUBA and as expected from the MIPS source number counts, we find very strong evolution of the contribution of the IR-selected population with lookback time. Pure evolution in density is firmly excluded by the data, but we find considerable degeneracy between strict evolution in luminosity and a combination of increases in both density and luminosity (L*{\_}IR prop. to (1+z){\^{}}{\{}3.2{\_}{\{}-0.2{\}}{\^{}}{\{}+0.7{\}}{\}}, Phi*{\_}IR prop. to (1+z){\^{}}{\{}0.7{\_}{\{}-0.6{\}}{\^{}}{\{}+0.2{\}}{\}}). Our results imply that the comoving IR energy density of the Universe evolves as (1+z){\^{}}(3.9+/-0.4) up to z{\$\sim${}}1 and that galaxies luminous in the infrared (i.e., L{\_}IR {\textgreater} 10{\^{}}11 L{\_}IR) are responsible for 70+/-15{\%} of this energy density at z{\$\sim${}}1. Taking into account the contribution of the UV luminosity evolving as (1+z){\^{}}{\$\sim${}}2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z{\$\sim${}}0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24mic fluxes into luminosities.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506462}, -author = {Floc'h, E Le and Papovich, C and Dole, H and Bell, E and Lagache, G and Rieke, G and Egami, E and Perez-Gonzalez, P and Alonso-Herrero, A and Rieke, M and Blaylock, M and Engelbracht, C and Gordon, K and Hines, D and Misselt, K and Morrison, J and Mould, J}, -doi = {10.1086/432789}, -eprint = {0506462}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Observations,Galaxies: Evolution,Galaxies: High-Redshift,Infrared: Galaxies}, -month = {oct}, -number = {1}, -pages = {169--190}, -primaryClass = {astro-ph}, -title = {{Infrared luminosity functions from the Chandra Deep Field South : the Spitzer view on the history of dusty star formation at 0{\textless}z{\textless}1}}, -url = {http://arxiv.org/abs/astro-ph/0506462%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/432789}, -volume = {632}, -year = {2005} -} -@article{De-Lucia:2007aa, -author = {Lucia, Gabriella De and Planck, Max}, -doi = {10.1111/j.1365-2966.2006.11287.x}, -journal = {$\backslash$mnras}, -keywords = {1 i n t,are the very bright,bcgs,brightest cluster galaxies,cd,elliptical and lenticular,evolution,formation,fundamental parameters,galaxies,galaxies that,ro d u c,stellar content,t i o n}, -month = {feb}, -pages = {2--14}, -title = {{The hierarchical formation of the brightest cluster galaxies Gabriella De Lucia ⋆ and J ´ emy Blaizot ⋆}}, -volume = {14}, -year = {2007} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for $\sim$20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J. and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Coenda, Mart{\'{i}}nez, Muriel - 2018 - Green valley galaxies as a transition population in different environments.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disk galaxies. Under this bulge-formation model, though, the high rates of mergers in Cold Dark Matter galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disk galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Barro2013, -abstract = {We combine high-resolution Hubble Space Telescope/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (M* {\textgreater} 1010 M⊙) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z ≳ 2, cSFGs present SFR = 100-200 M yr-1, yet their specific star formation rates (sSFR ∼ 10-9 yr -1) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (∼30{\%}) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 108 yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z ∼ 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z ≳ 2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z ≲ 2) path in which larger SFGs form extended QGs without passing through a compact state. {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1206.5000}, -author = {Barro, Guillermo and Faber, S M and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Koo, David C and Williams, Christina C and Kocevski, Dale D and Trump, Jonathan R and Mozena, Mark and McGrath, Elizabeth and {Van Der Wel}, Arjen and Wuyts, Stijn and Bell, Eric F and Croton, Darren J and Daniel, Ceverino and Dekel, Avishai and Ashby, M L N and Cheung, Edmond and Ferguson, Henry C and Fontana, Adriano and Fang, Jerome and Giavalisco, Mauro and Grogin, Norman A and Guo, Yicheng and Hathi, Nimish P and Hopkins, Philip F and Huang, Kuang Han and Koekemoer, Anton M and Kartaltepe, Jeyhan S and Lee, Kyoung Soo and Newman, Jeffrey A and Porter, Lauren A and Primack, Joel R and Ryan, Russell E and Rosario, David and Somerville, Rachel S and Salvato, Mara and Hsu, Li Ting}, -doi = {10.1088/0004-637X/765/2/104}, -eprint = {1206.5000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: high-redshift,galaxies: photometry,galaxies: starburst}, -number = {2}, -pmid = {7117407}, -title = {{Candels: The progenitors of compact quiescent galaxies at Z ∼ 2}}, -volume = {765}, -year = {2013} -} -@article{Wang2017, -abstract = {Difference imaging or image subtraction is a method that measures differential photometry by matching the pointing and point-spread function (PSF) between image frames. It is used for the detection of time-variable phenomena. Here we present a new category of method---CPM Difference Imaging, in which differences are not measured between matched images but instead between image frames and a data-driven predictive model that has been designed only to predict the pointing, PSF, and detector effects but not astronomical variability. In CPM Difference Imaging each pixel is modelled by the Causal Pixel Model (CPM) originally built for modeling Kepler data, in which pixel values are predicted by a linear combination of other pixels at the same epoch but far enough away such that these pixels are causally disconnected, astrophysically. It does not require that the user have any explicit model or description of the pointing or point-spread function of any of the images. Its principal drawback is that---in its current form---it requires an imaging campaign with many epochs and fairly stable telescope pointing. The method is applied to simulated data and also the K2 Campaign 9 microlensing data. We show that CPM Difference Imaging can detect variable objects and produce precise differentiate photometry in a crowded field. CPM Difference Imaging is capable of producing image differences at nearly photon-noise precision.}, -archivePrefix = {arXiv}, -arxivId = {1710.02428}, -author = {Wang, Dun and Hogg, David W and Foreman-Mackey, Daniel and Sch{\"{o}}lkopf, Bernhard}, -eprint = {1710.02428}, -pages = {1--23}, -title = {{A pixel-level model for event discovery in time-domain imaging}}, -url = {http://arxiv.org/abs/1710.02428}, -year = {2017} -} -@article{Morishita2018a, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {evolution,formation,galaxies,star formation}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Chirivi2017, -abstract = {Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we aim to present the first attempt at modelling line-of-sight (LOS) mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We have focussed on the Hubble Frontier Field cluster MACS J0416.1-2403, and our multi-plane model reproduces the observed image positions with a rms offset of {\$\sim${}}0.′′53. Starting from this best-fitting model, we simulated a mock cluster that resembles MACS J0416.1-2403 in order to explore the effects of LOS structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms {\$\sim${}}0.′′3); accounting for LOS galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factor of the lensed multiple images are recovered within {\$\sim${}}10{\%} for {\$\sim${}}95{\%} of them, those {\$\sim${}}5{\%} that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models. In addition, LOS galaxies cannot explain the apparent discrepancy in the properties of massive sub-halos between MACS J0416.1-2403 and N-body simulated clusters. Since our model of MACS J0416.1-2403 with LOS galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities would be needed in future models of MACS J0416.1-2403.}, -archivePrefix = {arXiv}, -arxivId = {1706.07815}, -author = {Chiriv{\`{i}}, G and Suyu, S H and Grillo, C and Halkola, A and Balestra, I and Caminha, G B and Mercurio, A and Rosati, P}, -doi = {10.1051/0004-6361/201731433}, -eprint = {1706.07815}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Dark matter,Galaxies: clusters: general,Galaxies: clusters: individual: MACS J0416.1-2403,Gravitational lensing: strong}, -pages = {1--29}, -title = {{MACS J0416.1-2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters}}, -url = {http://arxiv.org/abs/1706.07815%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731433}, -volume = {614}, -year = {2018} -} -@article{Iwanus2017, -abstract = {We describe and test a novel dark matter annihilation feedback (DMAF) scheme that has been implemented into the well-known cosmological simulation code GADGET-2. In the models considered here, dark matter can undergo self-annihilation/decay into radiation and baryons. These products deposit energy into the surrounding gas particles and then the dark matter/baryon fluid is self-consistently evolved under gravity and hydrodynamics. We present tests of this new feedback implementation in the case of idealized dark matter haloes with gas components for a range of halomasses, concentrations and annihilation rates. For some darkmattermodels, DMAF's ability to evacuate gas is enhanced in lower mass, concentrated haloes where the injected energy is comparable to its gravitational binding energy. Therefore, we expect the strongest signs of darkmatter annihilation to imprint themselves on to the baryonic structure of concentrated dwarf galaxies through their baryonic fraction and star formation history. Finally, we present preliminary results of the first self-consistent DMAF cosmological box simulations showing that the small-scale substructure is washed out for large annihilation rates.}, -archivePrefix = {arXiv}, -arxivId = {1707.06770}, -author = {Iwanus, N and Elahi, P J and Lewis, G F}, -doi = {10.1093/MNRAS/STX1974}, -eprint = {1707.06770}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Large-scale structure of Universe}, -number = {1}, -pages = {1214--1225}, -title = {{Dark matter annihilation feedback in cosmological simulations - I: Code convergence and idealized haloes}}, -url = {http://arxiv.org/abs/1707.06770%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1974}, -volume = {472}, -year = {2017} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ({\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashgamma{\}}{\$}), we find that, although the zero cosmic curvature is still included within {\$}2 \backslashsigma{\$} confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile {\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashalpha{\}}{\$} to be different from that of the total-mass density profile {\$}\backslashnu\backslashsim r{\^{}}{\{}-\backslashdelta{\}}{\$}, a weaker constraint on the curvature ({\$}\backslashOmega{\_}k{\textless}0.197{\$} at 68$\backslash${\%} confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of {\$}\backslashDelta \backslashOmega{\_}k\backslashsimeq 10{\^{}}{\{}-3{\}}{\$}, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{He2022a, -abstract = {A fundamental prediction of the cold dark matter (CDM) model of structure formation is the existence of a vast population of dark matter haloes extending to subsolar masses. By contrast, other dark matter models, such as a warm thermal relic (WDM), predict a cutoff in the mass function at a mass which, for popular models, lies approximately between 107 and 1010, M⊙. We use mock observations to demonstrate the viability of a forward modelling approach to extract information about low-mass dark haloes lying along the line of sight to galaxy-galaxy strong lenses. This can be used to constrain the mass of a thermal relic dark matter particle, mDM. With 50 strong lenses at Hubble Space Telescope resolution and a maximum pixel signal-to-noise ratio of ∼50, the expected median 2$\sigma$ constraint for a CDM-like model (with a halo mass cutoff at 107M⊙) is m DM > 4.10, keV (50 per cent chance of constraining mDM to be better than 4.10 keV). If, however, the dark matter is a warm particle of m_ DM=2.2, keV, our 'approximate Bayesian computation' method would result in a median estimate of mDM between 1.43 and 3.21 keV. Our method can be extended to the large samples of strong lenses that will be observed by future telescopes and could potentially rule out the standard CDM model of cosmogony. To aid future survey design, we quantify how these constraints will depend on data quality (spatial resolution and integration time) as well as on the lensing geometry (source and lens redshifts).}, -archivePrefix = {arXiv}, -arxivId = {2010.13221}, -author = {He, Qiuhan and Robertson, Andrew and Nightingale, James and Cole, Shaun and Frenk, Carlos S. and Massey, Richard and Amvrosiadis, Aristeidis and Li, Ran and Cao, Xiaoyue and Etherington, Amy}, -doi = {10.1093/mnras/stac191}, -eprint = {2010.13221}, -file = {:C\:/Users/Jammy/Documents/Papers/PyAutoLens/He2021DMABC.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Gravitational lensing: strong,Methods: statistical}, -number = {2}, -pages = {3046--3062}, -title = {{A forward-modelling method to infer the dark matter particle mass from strong gravitational lenses}}, -volume = {511}, -year = {2022} -} -@article{Ajello2015, -abstract = {The origin of the extragalactic $\gamma$-ray background (EGB) has been debated for some time. The EGB comprises the $\gamma$-ray emission from resolved and unresolved extragalactic sources, such as blazars, star-forming galaxies, and radio galaxies, as well as radiation from truly diffuse processes. This Letter focuses on the blazar source class, the most numerous detected population, and presents an updated luminosity function and spectral energy distribution model consistent with the blazar observations performed by the Fermi-Large Area Telescope (LAT). We show that blazars account for 50% of the EGB photons (>0.1 GeV), and that Fermi-LAT has already resolved ∼70% of this contribution. Blazars, and in particular hard-spectrum sources such as BL Lacs, are responsible for most of the EGB emission above 100 GeV. We find that the extragalactic background light, which attenuates blazars' high-energy emission, is responsible for the high-energy cutoff observed in the EGB spectrum. Finally, we show that blazars, star-forming galaxies, and radio galaxies can naturally account for the amplitude and spectral shape of the background in the 0.1-820 GeV range, leaving only modest room for other contributions. This allows us to set competitive constraints on the dark matter annihilation cross section.}, -archivePrefix = {arXiv}, -arxivId = {1501.05301}, -author = {Ajello, M. and Gasparrini, D. and S{\'{a}}nchez-Conde, M. and Zaharijas, G. and Gustafsson, M. and Cohen-Tanugi, J. and Dermer, C. D. and Inoue, Y. and Hartmann, D. and Ackermann, M. and Bechtol, K. and Franckowiak, A. and Reimer, A. and Romani, R. W. and Strong, A. W.}, -doi = {10.1088/2041-8205/800/2/L27}, -eprint = {1501.05301}, -issn = {20418213}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,dark matter,galaxies: active,galaxies: jets,gamma rays: diffuse background,surveys}, -number = {2}, -pages = {L27}, -title = {{The origin of the extragalactic gamma-ray background and implications for dark matter annihilation}}, -url = {http://stacks.iop.org/2041-8205/800/i=2/a=L27?key=crossref.e04757679f7ff1daf7eacf1c24dabba1}, -volume = {800}, -year = {2015} -} -@article{Humphrey2012, -abstract = {The Elliptical Isolated X-ray (ElIXr) Galaxy Survey is a volume-limited (<110Mpc) study of optically selected, isolated, L * elliptical galaxies to provide an X-ray census of galaxy-scale (virial mass, M vir ≲ 1013 M ⊙) objects and identify candidates for detailed hydrostatic mass modeling. In this paper, we present a Chandra and XMM study of one such candidate, NGC 1521, and constrain its distribution of dark and baryonic matter. We find a morphologically relaxed hot gas halo, extending almost to R 500, that is well described by hydrostatic models similar to the benchmark, baryonically closed, Milky Way mass elliptical galaxy NGC 720. We obtain good constraints on the enclosed gravitating mass (M 500 = [3.8 ± 1.0] × 1012 M ⊙, slightly higher than NGC 720) and baryon fraction (f b, 500 = 0.13 ± 0.03). We confirm at 8.2$\sigma$ the presence of a dark matter (DM) halo consistent with $\Lambda$CDM. Assuming a Navarro-Frenk-White DM profile, our self-consistent, physical model enables meaningful constraints beyond R 500, revealing that most of the baryons are in the hot gas. Within the virial radius, fb is consistent with the cosmic mean, suggesting that the predicted massive, quasi-hydrostatic gas halos may be more common than previously thought. We confirm that the DM and stars conspire to produce an approximately power-law total mass profile ($\rho$totr -$\alpha$) that follows the recently discovered scaling relation between $\alpha$ and optical effective radius. Our conclusions are insensitive to modest, observationally motivated, deviations from hydrostatic equilibrium. Finally, after correcting for the enclosed gas fraction, the entropy profile is close to the self-similar prediction of gravitational structure formation simulations, as observed in massive galaxy clusters. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1204.3095}, -author = {Humphrey, Philip J. and Buote, David A. and O'Sullivan, Ewan and Ponman, Trevor J.}, -doi = {10.1088/0004-637X/755/2/166}, -eprint = {1204.3095}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Humphrey et al. - 2012 - The ElIXr galaxy survey. II. baryons and dark matter in an isolated elliptical galaxy.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {X-rays: galaxies,dark matter,galaxies: ISM,galaxies: elliptical and lenticular, cD,galaxies: formation,galaxies: fundamental parameters,galaxies: individual (NGC 1521)}, -number = {2}, -pages = {1--18}, -title = {{The ElIXr galaxy survey. II. baryons and dark matter in an isolated elliptical galaxy}}, -volume = {755}, -year = {2012} -} -@article{Yang2006, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{VanDokkum2002, -abstract = {Conventional algorithms for rejecting cosmic-rays in single CCD exposures rely on the contrast between cosmic-rays and their surroundings, and may produce erroneous results if the Point Spread Function (PSF) is smaller than the largest cosmic-rays. This paper describes a robust algorithm for cosmic-ray rejection, based on a variation of Laplacian edge detection. The algorithm identifies cosmic-rays of arbitrary shapes and sizes by the sharpness of their edges, and reliably discriminates between poorly sampled point sources and cosmic-rays. Examples of its performance are given for spectroscopic and imaging data, including HST WFPC2 images.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108003}, -author = {van Dokkum, Pieter G.}, -doi = {10.1086/323894}, -eprint = {0108003}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/van Dokkum - 2001 - Cosmic‐Ray Rejection by Laplacian Edge Detection.pdf:pdf}, -issn = {0004-6280}, -journal = {Publ. Astron. Soc. Pac.}, -number = {789}, -pages = {1420--1427}, -primaryClass = {astro-ph}, -title = {{Cosmic‐Ray Rejection by Laplacian Edge Detection}}, -volume = {113}, -year = {2001} -} -@article{Harvey2015, -abstract = {Collisions between galaxy clusters provide a test of the nongravitational forces acting on dark matter. Dark matter's lack of deceleration in the "bullet cluster" collision constrained its self-interaction cross section $\sigma$DM/m {\textless} 1.25 square centimeters per gram (cm2/g) [68{\%} confidence limit (CL)] ($\sigma$DM, self-interaction cross section; m, unit mass of dark matter) for long-ranged forces. Using the Chandra and Hubble Space Telescopes, we have now observed 72 collisions, including both major and minor mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6s significance. The position of the dark mass has remained closely aligned within 5.8 T 8.2 kiloparsecs of associated stars, implying a self-interaction cross section $\sigma$DM/m {\textless} 0.47 cm2/g (95{\%} CL) and disfavoring some proposed extensions to the standard model.}, -archivePrefix = {arXiv}, -arxivId = {1503.07675}, -author = {Harvey, David and Massey, Richard and Kitching, Thomas and Taylor, Andy and Tittley, Eric}, -doi = {10.1126/science.1261381}, -eprint = {1503.07675}, -issn = {10959203}, -journal = {Science}, -number = {6229}, -pages = {1462--1465}, -pmid = {25814581}, -title = {{The nongravitational interactions of dark matter in colliding galaxy clusters}}, -volume = {347}, -year = {2015} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P_KS \simeq 1.5 \times 10^{-4}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability \simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R. and Kravtsov, Andrey V. and Gnedin, Oleg Y. and Klypin, Anatoly A.}, -doi = {10.1086/431355}, -eprint = {0502496}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Zentner et al. - 2005 - The Anisotropic Distribution of Galactic Satellites.pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Hermans2019, -abstract = {Posterior inference with an intractable likelihood is becoming an increasingly common task in scientific domains which rely on sophisticated computer simulations. Typically, these mechanistic models do not admit tractable densities forcing practitioners to rely on approximations during inference. This work proposes a novel approach to address the intractability of the likelihood and the marginal model. We achieve this by learning a flexible estimator which approximates the likelihood-to-evidence ratio. The resulting amortized ratio estimator is embedded in MCMC samplers such as Metropolis-Hastings and Hamiltonian Monte Carlo to approximate the likelihood-ratio between consecutive states in the Markov chain, allowing us to draw samples from the intractable posterior. Techniques are presented to improve the numerical stability. We demonstrate our approach on a variety of benchmarks and compare against well-established approximate inference techniques. Scientific applications in high energy and astrophysics with high-dimensional observations show its applicability.}, -archivePrefix = {arXiv}, -arxivId = {1903.04057}, -author = {Hermans, Joeri and Begy, Volodimir and Louppe, Gilles}, -eprint = {1903.04057}, -number = {i}, -title = {{Likelihood-free MCMC with Amortized Approximate Likelihood Ratios}}, -url = {http://arxiv.org/abs/1903.04057}, -year = {2019} -} -@article{Wang2014a, -abstract = {Charged Coupled Devices (CCDs) have been successfully used in several low energy X-ray astronomical satellites over the past two decades. Their high energy resolution and high spatial resolution make them a perfect tool for low energy astronomy, such as observing the formation of galaxy clusters and the environment around black holes. The Low Energy X-ray Telescope (LE) group is developing a Swept Charge Device (SCD) for the Hard X-ray Modulation Telescope (HXMT) satellite. A SCD is a special low energy X-ray CCD, which can be read out a thousand times faster than traditional CCDs, simultaneously keeping excellent energy resolution. A test method for measuring the charge transfer efficiency (CTE) of a prototype SCD has been set up. Studies of the charge transfer inefficiency (CTI) with a proton-irradiated SCD have been performed at a range of operating temperatures. The SCD is irradiated by 3 × 10 8cm-2 10 MeV protons. {\textcopyright}2014 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1308.1698}, -author = {Wang, Yu Sa and Yang, Yan Ji and Chen, Yong and Liu, Xiao Yan and Cui, Wei Wei and Xu, Yu Peng and Li, Cheng Kui and Li, Mao Shun and Han, Da Wei and Chen, Tian Xiang and Huo, Jia and Wang, Juan and Li, Wei and Hu, Wei and Zhang, Yi and Lu, Bo and Yin, Guo He and Zhu, Yue and Zhang, Zi Liang}, -doi = {10.1088/1674-1137/38/6/066001}, -eprint = {1308.1698}, -issn = {16741137}, -journal = {Chinese Physics C}, -keywords = {CCD,CTE,CTI,HXMT,LE,SCD,proton-irradiated}, -number = {6}, -pages = {66001}, -title = {{Measurements of charge transfer efficiency in a proton-irradiated swept charge device}}, -url = {http://stacks.iop.org/1674-1137/38/i=6/a=066001?key=crossref.02a5cb134fd3859a1cfa309d04df9b61}, -volume = {38}, -year = {2014} -} -@article{Hsu2018, -abstract = {We present a new framework to characterize the occurrence rates of planet candidates identified by Kepler based on hierarchical Bayesian modeling, Approximate Bayesian Computing (ABC), and sequential importance sampling. For this study we adopt a simple 2-D grid in planet radius and orbital period as our model and apply our algorithm to estimate occurrence rates for Q1-Q16 planet candidates orbiting around solar-type stars. We arrive at significantly increased planet occurrence rates for small planet candidates ({\$}R{\_}p{\textless}1.25 R{\_}{\{}\backslashoplus{\}}{\$}) at larger orbital periods ({\$}P{\textgreater}80{\$}d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is {\$}1.6{\^{}}{\{}+1.2{\}}{\_}{\{}-0.5{\}}{\$} per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2{\$}R{\_}{\{}\backslashoplus{\}}{\$} that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C and Ford, Eric B and Ragozzine, Darin and Morehead, Robert C}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -number = {5}, -pages = {205}, -title = {{ Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation }}, -url = {http://arxiv.org/abs/1803.10787%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -volume = {155}, -year = {2018} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 {\textless} z {\textless} 0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 percent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.0763}, -author = {Lackner, C N and Gunn, J E}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data%7B%5C_%7Dquery?bibcode=2012arXiv1201.0763L%7B%5C&%7Dlink%7B%5C_%7Dtype=ABSTRACT%7B%5C%25%7D5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Bothwell2013, -abstract = {We present the results from a survey of 12CO emission in 40 luminous sub-millimetre galaxies (SMGs), with 850-$\mu$m fluxes of S850$\mu$m = 4-20 mJy, conducted with the Plateau de Bure Interferometer. We detect 12CO emission in 32 SMGs at z $\sim$ 1.2-4.1, including 16 SMGs not previously published. Using multiple 12CO line (Jup = 2-7) observations, we derive a median spectral line energy distribution for luminous SMGs. We report the discovery of a fundamental relationship between 12CO FWHM and 12CO line luminosity in high-redshift starbursts, which we interpret as a natural consequence of the baryon-dominated dynamics within the regions probed by our observations. We use far-infrared luminosities to assess the star formation efficiency in our SMGs, finding that the slope of the L' CO -LFIR relation is close to linear. We derive molecular gas masses, finding a mean gas mass of (5.3 ± 1.0) × 10)10 M⊙. Combining these with dynamical masses, we determine the redshift evolution of the gas content of SMGs, finding that they do not appear to be significantly more gas rich than less vigorously star-forming galaxies at high redshifts. Finally, we collate X-ray observations, and study the interdependence of gas and dynamical properties of SMGs with their AGN activity and supermassive black holemasses (MBH), finding that SMGs lie significantly below the local MBH-$\sigma$ relation. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1205.1511}, -author = {Bothwell, M. S. and Smail, Ian and Chapman, S. C. and Genzel, R. and Ivison, R. J. and Tacconi, L. J. and Alaghband-Zadeh, S. and Bertoldi, F. and Blain, A. W. and Casey, C. M. and Cox, P. and Greve, T. R. and Lutz, D. and Neri, R. and Omont, A. and Swinbank, A. M.}, -doi = {10.1093/mnras/sts562}, -eprint = {1205.1511}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Galaxies: ISM,Galaxies: evolution,Galaxies: formation}, -number = {4}, -pages = {3047--3067}, -pmid = {24874120}, -title = {{A survey of molecular gas in luminous sub-millimetre galaxies}}, -volume = {429}, -year = {2013} -} -@article{Libeskind2014, -abstract = {We examine the angular infall pattern of subhaloes on to host haloes in the context of the large-scale structure. We find that this infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are found to be preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that it is always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range (∼10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large-scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group. {\textcopyright} 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1407.0394}, -author = {Libeskind, Noam I. and Knebe, Alexander and Hoffman, Yehuda and Gottl{\"{o}}ber, Stefan}, -doi = {10.1093/mnras/stu1216}, -eprint = {1407.0394}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Libeskind et al. - 2014 - The universal nature of subhalo accretion(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Large-scale structure of universe}, -number = {2}, -pages = {1274--1280}, -title = {{The universal nature of subhalo accretion}}, -volume = {443}, -year = {2014} -} -@article{Alexander2005, -abstract = {Deep SCUBA surveys have uncovered a large population of massive submillimeter-emitting galaxies (SMGs; f850$\mu$m>$\sim$4 mJy) at z>$\sim$1. Although it is generally believed that these galaxies host intense star formation activity, there is growing evidence that a substantial fraction also harbor an active galactic nucleus (AGN; i.e., an accreting super-massive black hole [SMBH]). We present here possibly the strongest evidence for this viewpoint to date: the combination of ultradeep X-ray observations (the 2 Ms Chandra Deep Field-North) and deep Keck spectroscopic data of SMGs with radio counterparts. We find that the majority ($\sim$75%) of these radio-selected spectroscopically identified SMGs host AGN activity; the other $\sim$25% have X-ray properties consistent with star formation (X-ray-derived star formation rates of $\sim$1300-2700 Msolar yr-1). The AGNs have properties generally consistent with those of nearby luminous AGNs ($\Gamma$$\sim$1.8+/-0.5, NH$\sim$1020-1024 cm-2, and LX$\sim$1043-1044.5 ergs s-1), and the majority ($\sim$80%) are heavily obscured (NH>$\sim$1023 cm-2). We construct composite rest-frame 2-20 keV spectra for three different obscuration classes [NH<1023 cm-2, NH=(1-5)×1023 cm-2, and NH>5×1023 cm-2], which reveal features not seen in the individual X-ray spectra. An $\sim$1 keV equivalent width Fe K$\alpha$ emission line is seen in the composite X-ray spectrum of the most heavily obscured AGNs, suggesting Compton-thick or near Compton-thick absorption. Even taking into account the effects of absorption, we find that the average X-ray to far-IR luminosity ratio of the AGN-classified SMGs (LX/LFIR=0.004) is approximately 1 order of magnitude below that found for typical quasars. This result suggests that intense star formation activity (of order $\sim$1000 Msolar yr-1) dominates the bolometric output of these SMGs. However, we also explore the possibility that the X-ray to far-IR luminosity ratio of the AGN components is intrinsically less than that found for typical quasars and postulate that some SMGs may be AGN dominated. We investigate the implications of our results for the growth of massive black holes, discuss the prospects for deeper X-ray observations, and explore the scientific potential offered by the next generation of X-ray observatories.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506608}, -author = {Alexander, D. M. and Bauer, F. E. and Chapman, S. C. and Smail, I. and Blain, A. W. and Brandt, W. N. and Ivison, R. J.}, -doi = {10.1086/444342}, -eprint = {0506608}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {736--750}, -primaryClass = {astro-ph}, -title = {{The X‐Ray Spectral Properties of SCUBA Galaxies}}, -url = {http://stacks.iop.org/0004-637X/632/i=2/a=736}, -volume = {632}, -year = {2005} -} -@article{2001et, -author = {عامر, د. وفاء محروس}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/عامر - 2001 - No Title المعالجة الحيوية للمولوثات البيئية(8).pdf:pdf}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T < 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim & Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H. and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Amvrosiadis2025, -abstract = {DOI: 10.1093/mnras/staf048 Monthly Notices of the Royal Astronomical Society, 537, 2, 11-1-2025. Abstract: We examine the morphological and kinematical properties of SPT-2147, a strongly lensed, massive, dusty, star-forming galaxy at . Combining data from JWST, Hubble Space Telescope, and ALMA, we study the galaxy’s stellar emission, dust continuum, and gas properties. The imaging reveals a central bar structure in the stars and gas embedded within an extended disc with a spiral arm-like feature. The kinematics confirm the presence of the bar and of the regularly rotating disc. Dynamical modelling yields a dynamical mass, , and a maximum rotational velocity to velocity dispersion ratio, . From multiband imaging we infer, via spectral energy distribution fitting, a stellar mass, , and a star formation rate, , after correcting for magnification. Combining these measurements with the molecular gas mass, we derive a baryonic-to-total mass ratio of within 4.0 kpc. This finding suggests that the formation of bars in galaxies begins earlier in the history of the Universe than previously thought and can also occur in galaxies with elevated gas fractions.}, -author = {Amvrosiadis, A and Lange, S and Nightingale, J W and He, Q and Frenk, C S and Oman, K A and Smail, I and Swinbank, A M and Fragkoudi, F and Gadotti, D A and Cole, S and Borsato, E and Robertson, A and Massey, R and Cao, X and Li, R}, -doi = {10.1093/mnras/staf048}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Amvrosiadis2025OnsetBar.pdf:pdf}, -issn = {1365-2966}, -journal = {MNRAS}, -keywords = {1,1 i n t,amongst high redshift,barger et al,blain 1997,galaxies,galaxy populations,gravitational lensing,ivison,ro d u c,smail,smgs,strong,sub-mm,submillimetre,t i o n,z}, -pages = {1163--1181}, -publisher = {Oxford University Press}, -title = {{The onset of bar formation in a massive galaxy at z $\sim$ 3.8}}, -url = {https://doi.org/10.1093/mnras/staf048}, -volume = {537}, -year = {2025} -} -@article{Greene2013, -abstract = {We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions $\sigma$* ≳ 150 km s-1. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼ 10 Gyr), relatively metal-poor ([Fe/H] ≈ -0.5), and $\alpha$-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z ≈ 1.5-2). {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1308.2682}, -author = {Greene, Jenny E. and Murphy, Jeremy D. and Graves, Genevieve J. and Gunn, James E. and Raskutti, Sudhir and Comerford, Julia M. and Gebhardt, Karl}, -doi = {10.1088/0004-637X/776/2/64}, -eprint = {1308.2682}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2013 - The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: abundances,galaxies: elliptical and lenticular, cD,galaxies: evolution}, -number = {2}, -title = {{The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius}}, -volume = {776}, -year = {2013} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10% of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://adsabs.harvard.edu/abs/2010ApJ...709.1138D}, -volume = {709}, -year = {2010} -} -@article{Barthelme2014, -abstract = {Many models of interest in the natural and social sciences have no closed-form likelihood function, which means that they cannot be treated using the usual techniques of statistical inference. In the case where such models can be efficiently simulated, Bayesian inference is still possible thanks to the approximate Bayesian computation (ABC) algorithm. Although many refinements have been suggested, ABC inference is still far from routine. ABC is often excruciatingly slow due to very low acceptance rates. In addition, ABC requires introducing a vector of "summary statistics" s(y), the choice of which is relatively arbitrary, and often require some trial and error, making the whole process laborious for the user.We introduce in this work the EP-ABC algorithm, which is an adaptation to the likelihood-free context of the variational approximation algorithm known as expectation propagation. The main advantage of EP-ABC is that it is faster by a few orders of magnitude than standard algorithms, while producing an overall approximation error that is typically negligible. A second advantage of EP-ABC is that it replaces the usual global ABC constraint {pipe}{pipe}s(y) - s(y*) ≤ $\epsilon$, where s(y*) is the vector of summary statistics computed on the whole dataset, by n local constraints of the form {pipe}{pipe}si (yi) - si (yi*){pipe}{pipe} ≤ $\epsilon$ that apply separately to each data point. In particular, it is often possible to take si (yi) = yi, making it possible to do away with summary statistics entirely. In that case, EP-ABC makes it possible to approximate directly the evidence (marginal likelihood) of the model. Comparisons are performed in three real-world applications that are typical of likelihood-free inference, including one application in neuroscience that is novel, and possibly too challenging for standard ABC techniques. {\textcopyright} 2014 American Statistical Association.}, -archivePrefix = {arXiv}, -arxivId = {1107.5959}, -author = {Barthelm{\'{e}}, Simon and Chopin, Nicolas}, -doi = {10.1080/01621459.2013.864178}, -eprint = {1107.5959}, -file = {:C\:/Users/Jammy/Documents/Papers/Stats/Barthelme2014EPABC.pdf:pdf}, -issn = {1537274X}, -journal = {Journal of the American Statistical Association}, -keywords = {Approximate Bayesian computation,Approximate inference,Composite likelihood,Quasi-Monte Carlo}, -number = {505}, -pages = {315--333}, -title = {{Expectation propagation for likelihood-free inference}}, -volume = {109}, -year = {2014} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani} and Caldwell, Nelson}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Bullock2005a, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted $\sim$100-200 luminous satellite galaxies in the past \$\sim$12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ($\sim$80%) coming from the \$\sim$15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of $\sim$9 Gyr in the past, while surviving satellite systems have median accretion times of $\sim$5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S. and Johnston, Kathryn V.}, -doi = {10.1086/497422}, -eprint = {0506467}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bullock, Johnston - 2005 - Tracing Galaxy Formation with Stellar Halos. I. Methods.pdf:pdf}, -isbn = {0272-9490 (Print)$\$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Pontzen2012, -abstract = {We propose and successfully test against new cosmological simulations a novel analytical description of the physical processes associated with the origin of cored dark matter density profiles. In the simulations, the potential in the central kiloparsec changes on sub-dynamical time-scales over the redshift interval 4 > z > 2, as repeated, energetic feedback generates large underdense bubbles of expanding gas from centrally concentrated bursts of star formation. The model demonstrates how fluctuations in the central potential irreversibly transfer energy into collisionless particles, thus generating a dark matter core. A supply of gas undergoing collapse and rapid expansion is therefore the essential ingredient. The framework, based on a novel impulsive approximation, breaks with the reliance on adiabatic approximations which are inappropriate in the rapidly changing limit. It shows that both outflows and galactic fountains can give rise to cusp flattening, even when only a few per cent of the baryons form stars. Dwarf galaxies maintain their core to the present time. The model suggests that constant density dark matter cores will be generated in systems of a wide mass range if central starbursts or active galactic nucleus phases are sufficiently frequent and energetic. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1106.0499}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1111/j.1365-2966.2012.20571.x}, -eprint = {1106.0499}, -isbn = {doi:10.1111/j.1365-2966.2012.20571.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: dwarf}, -month = {apr}, -number = {4}, -pages = {3464--3471}, -title = {{How supernova feedback turns dark matter cusps into cores}}, -volume = {421}, -year = {2012} -} -@article{Speagle2020, -abstract = {We present dynesty, a public, open-source, python package to estimate Bayesian posteriors and evidences (marginal likelihoods) using the dynamic nested sampling methods developed by Higson et al. By adaptively allocating samples based on posterior structure, dynamic nested sampling has the benefits of Markov chain Monte Carlo (MCMC) algorithms that focus exclusively on posterior estimation while retaining nested sampling's ability to estimate evidences and sample from complex, multimodal distributions. We provide an overview of nested sampling, its extension to dynamic nested sampling, the algorithmic challenges involved, and the various approaches taken to solve them in this and previous work. We then examine dynesty's performance on a variety of toy problems along with several astronomical applications. We find in particular problems dynesty can provide substantial improvements in sampling efficiency compared to popular MCMC approaches in the astronomical literature. More detailed statistical results related to nested sampling are also included in the appendix.}, -archivePrefix = {arXiv}, -arxivId = {1904.02180}, -author = {Speagle, Joshua S}, -doi = {10.1093/mnras/staa278}, -eprint = {1904.02180}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Speagle - 2020 - dynesty a dynamic nested sampling package for estimating Bayesian posteriors and evidences.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {data analysis,methods,statistical}, -number = {3}, -pages = {3132--3158}, -title = {{dynesty: a dynamic nested sampling package for estimating Bayesian posteriors and evidences}}, -volume = {493}, -year = {2020} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright}2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, n=10[cm-3], results in strong expansion of the DM halo in galaxies with stellar masses in the range 107.5 ≤ Mstar ≤ 109.5 M⊙. We find that lower thresholds such as n = 0.1 (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e. ≤50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with n = 10 have gas fractions of ∼0.2 and variations of ∼0.1, while n = 0.1 simulations have order of magnitude lower gas fractions and hence do not expand the halo. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with n = 0.1 and n = 1, but in a reasonable agreement with n = 10. Star formation rates are more variable for higher n, lower galaxy masses, and when star formation is measured on shorter time-scales. For example, simulations with n = 10 have up to 0.4 dex higher scatter in specific star formation rates than simulations with n = 0.1. Thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625}, -author = {Dutton, Aaron A and MacCi{\`{o}}, Andrea V and Buck, Tobias and Dixon, Keri L and Blank, Marvin and Obreja, Aura}, -doi = {10.1093/mnras/stz889}, -eprint = {1811.10625}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure,methods: numerical}, -number = {1}, -pages = {655--671}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://arxiv.org/abs/1811.10625%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stz889}, -volume = {486}, -year = {2019} -} -@article{Peng2010, -abstract = {We present a two-dimensional (2-D) fitting algorithm (GALFIT, Version 3) with new capabilities to study the structural components of galaxies and other astronomical objects in digital images. Our technique improves on previous 2-D fitting algorithms by allowing for irregular, curved, logarithmic and power-law spirals, ring and truncated shapes in otherwise traditional parametric functions like the Sersic, Moffat, King, Ferrer, etc., profiles. One can mix and match these new shape features freely, with or without constraints, apply them to an arbitrary number of model components and of numerous profile types, so as to produce realistic-looking galaxy model images. Yet, despite the potential for extreme complexity, the meaning of the key parameters like the Sersic index, effective radius or luminosity remain intuitive and essentially unchanged. The new features have an interesting potential for use to quantify the degree of asymmetry of galaxies, to quantify low surface brightness tidal features beneath and beyond luminous galaxies, to allow more realistic decompositions of galaxy subcomponents in the presence of strong rings and spiral arms, and to enable ways to gauge the uncertainties when decomposing galaxy subcomponents. We illustrate these new features by way of several case studies that display various levels of complexity.}, -archivePrefix = {arXiv}, -arxivId = {0912.0731}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans Walter}, -doi = {10.1088/0004-6256/139/6/2097}, -eprint = {0912.0731}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Galaxies: bulges,Galaxies: fundamental parameters,Galaxies: structure,Techniques: image processing,Techniques: photometric}, -number = {6}, -pages = {2097--2129}, -title = {{Detailed decomposition of galaxy images. II. beyond axisymmetric models}}, -volume = {139}, -year = {2010} -} -@article{Peng2002, -abstract = {We present a two-dimensional (2-D) fitting algorithm (GALFIT) designed to extract structural components from galaxy images, with emphasis on closely modeling light profiles of spatially well-resolved, nearby galaxies observed with the Hubble Space Telescope. Our algorithm improves on previous techniques in two areas, by being able to simultaneously fit a galaxy with an arbitrary number of components, and with optimization in computation speed, suited for working on large galaxy images. We use 2-D models such as the ``Nuker'' law, the Sersic (de Vaucouleurs) profile, an exponential disk, and Gaussian or Moffat functions. The azimuthal shapes are generalized ellipses that can fit disky and boxy components. Many galaxies with complex isophotes, ellipticity changes, and position-angle twists can be modeled accurately in 2-D. When examined in detail, we find that even simple-looking galaxies generally require at least three components to be modeled accurately, rather than the one or two components more often employed. We illustrate this by way of 7 case studies, which include regular and barred spiral galaxies, highly disky lenticular galaxies, and elliptical galaxies displaying various levels of complexities. A useful extension of this algorithm is to accurately extract nuclear point sources in galaxies. We compare 2-D and 1-D extraction techniques on simulated images of galaxies having nuclear slopes with different degrees of cuspiness, and we then illustrate the application of the program to several examples of nearby galaxies with weak nuclei.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0204182}, -author = {Peng, Chien Y. and Ho, Luis C. and Impey, Chris D. and Rix, Hans-Walter}, -doi = {10.1086/340952}, -eprint = {0204182}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Peng et al. - 2002 - Detailed Structural Decomposition of Galaxy Images.pdf:pdf}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {1}, -pages = {266--293}, -primaryClass = {astro-ph}, -title = {{Detailed Structural Decomposition of Galaxy Images}}, -url = {http://arxiv.org/abs/astro-ph/0204182%0Ahttp://dx.doi.org/10.1086/340952}, -volume = {124}, -year = {2002} -} -@article{Herbert-Fort2007, -abstract = {We measure the distribution of velocities for prograde and retrograde satellite galaxies using a combination of published data and new observations for 78 satellites of 63 extremely isolated disc galaxies (169 satellites total). We find that the velocity distribution is non-Gaussian ({\textgreater}99.9 per cent confidence), but that it can be described as the sum of two Gaussians, one of which is broad ($\sigma$ = 176 ± 15 km s-1), has a mean prograde velocity of 86 ± 30 km s-1, and contains ∼55 per cent of the satellites, while the other is slightly retrograde with a mean velocity of -21 ± 22 km s-1 and $\sigma$ = 74 ± 18 km s-1 and contains ∼45 per cent of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy, and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Enia2018, -abstract = {We perform lens modelling and source reconstruction of Sub-millimetre Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500$\mu$m in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). A previous analysis of the same data set used a single S{\'{e}}rsic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from theH-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission.We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5s. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value reff {\$\sim${}} 1.77 kpc and a median Gaussian full width at half-maximum {\$\sim${}}1.47 kpc. After correction for magnification, our sources have intrinsic star formation rates (SFR) {\$\sim${}} 900-3500M⊙ yr-1, resulting in a median SFR surface density $\Sigma$SFR {\$\sim${}} 132M⊙ yr-1 kpc-2 (or {\$\sim${}}218M⊙ yr-1 kpc-2 for the Gaussian fit). This is consistent with that observed for other star-forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst.}, -archivePrefix = {arXiv}, -arxivId = {1801.01831}, -author = {Enia, A and Negrello, M and Gurwell, M and Dye, S and Rodighiero, G and Massardi, M and {De Zotti}, G and Franceschini, A and Cooray, A and van der Werf, P and Birkinshaw, M and Michalowski, M J and Oteo, I}, -doi = {10.1093/mnras/sty021}, -eprint = {1801.01831}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong,Instrumentation: interferometers}, -number = {3}, -pages = {3467--3484}, -title = {{The Herschel-ATLAS: Magnifications and physical sizes of 500-$\mu$m-selected strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1801.01831}, -volume = {475}, -year = {2018} -} -@article{Galan2022, -abstract = {Modeling the mass distribution of galaxy-scale strong gravitational lenses is a task of increasing difficulty. The high-resolution and depth of imaging data now available render simple analytical forms ineffective at capturing lens structures spanning a large range in spatial scale, mass scale, and morphology. In this work, we address the problem with a novel multi-scale method based on wavelets. We test our method on simulated Hubble Space Telescope imaging data of strong lenses containing different types of mass substructures making them deviate from smooth models: (1) a localized small dark matter subhalo, (2) a Gaussian random field that mimics a non-localized population of subhalos along the line of sight, (3) galaxy-scale multipoles that break elliptical symmetry. We show that wavelets are able to recover all of these structures accurately. This is made technically possible by using gradient-informed optimization based on automatic differentiation over thousands of parameters, also allowing us to sample the posterior distributions of all model parameters simultaneously. By construction, our method merges all current modeling paradigms - analytical, pixelated, and deep learning - into a single modular framework. It is also well-suited for the fast modeling of large samples of lenses. All methods presented here are publicly available in our new Herculens package.}, -archivePrefix = {arXiv}, -arxivId = {2207.05763}, -author = {Galan, Aymeric and Vernardos, Georgios and Peel, Austin and Courbin, Fr{\'{e}}d{\'{e}}ric and Starck, Jean-Luc}, -eprint = {2207.05763}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Galan2022Wavelet.pdf:pdf}, -journal = {A\&A}, -keywords = {cosmology,dark matter,data analysis,galaxies,gravitation,gravitational lensing,methods,strong,structure}, -number = {A155}, -pages = {24}, -title = {{Using wavelets to capture deviations from smoothness in galaxy-scale strong lenses}}, -url = {http://arxiv.org/abs/2207.05763}, -volume = {668}, -year = {2022} -} -@article{Weijmans2014, -abstract = {We use the Atlas3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q=0.25 and standard deviation sigma{\_}q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and sigma{\_}q =0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrisations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P T and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F and Davies, Roger L and Davis, Timothy A and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular,Galaxies,Structure,cD- galaxies}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS{\textless}sup{\textgreater}3D{\textless}/sup{\textgreater}project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N. J. and Holland, A. D. and Gow, J. P. D. and Hall, D. J. and Tutt, James H. and Burt, D. and Endicott, J.}, -doi = {10.1117/12.926804}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2012 - Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps(2).pdf:pdf}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Barro2013, -abstract = {We combine high-resolution Hubble Space Telescope/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (M* {\textgreater} 1010 M⊙) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z ≳ 2, cSFGs present SFR = 100-200 M yr-1, yet their specific star formation rates (sSFR ∼ 10-9 yr -1) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (∼30{\%}) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 108 yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z ∼ 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z ≳ 2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z ≲ 2) path in which larger SFGs form extended QGs without passing through a compact state. {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1206.5000}, -author = {Barro, Guillermo and Faber, S M and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Koo, David C and Williams, Christina C and Kocevski, Dale D and Trump, Jonathan R and Mozena, Mark and McGrath, Elizabeth and {Van Der Wel}, Arjen and Wuyts, Stijn and Bell, Eric F and Croton, Darren J and Daniel, Ceverino and Dekel, Avishai and Ashby, M L N and Cheung, Edmond and Ferguson, Henry C and Fontana, Adriano and Fang, Jerome and Giavalisco, Mauro and Grogin, Norman A and Guo, Yicheng and Hathi, Nimish P and Hopkins, Philip F and Huang, Kuang Han and Koekemoer, Anton M and Kartaltepe, Jeyhan S and Lee, Kyoung Soo and Newman, Jeffrey A and Porter, Lauren A and Primack, Joel R and Ryan, Russell E and Rosario, David and Somerville, Rachel S and Salvato, Mara and Hsu, Li Ting}, -doi = {10.1088/0004-637X/765/2/104}, -eprint = {1206.5000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: high-redshift,galaxies: photometry,galaxies: starburst}, -number = {2}, -pmid = {7117407}, -title = {{Candels: The progenitors of compact quiescent galaxies at Z ∼ 2}}, -volume = {765}, -year = {2013} -} -@article{Reynolds2015, -abstract = {Compact radio sources sometimes exhibit intervals of large, rapid changes in their flux-density, due to lensing by interstellar plasma crossing the line-of-sight. A novel survey program has made it possible to discover these "Extreme Scattering Events" (ESEs) in real time, resulting in a high-quality dynamic spectrum of an ESE observed in PKS 1939-315. Here we present a method for determining the column-density profile of a plasma lens, given only the dynamic radio spectrum of the lensed source, under the assumption that the lens is either axisymmetric or totally anisotropic. Our technique relies on the known, strong frequency dependence of the plasma refractive index in order to determine how points in the dynamic spectrum map to positions on the lens. We apply our method to high-frequency (4.2-10.8 GHz) data from the Australia Telescope Compact Array of the PKS 1939-315 ESE. The derived electron column-density profiles are very similar for the two geometries we consider, and both yield a good visual match to the data. However, the fit residuals are substantially above the noise level, and deficiencies are evident when we compare the predictions of our model to lower-frequency (1.6-3.1 GHz) data on the same ESE, thus motivating future development of more sophisticated inversion techniques.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1512.03411}, -author = {Tuntsov, Artem V. and Walker, Mark A. and Koopmans, Leon V. E. and Bannister, Keith W. and Stevens, Jamie and Johnston, Simon and Reynolds, Cormac and Bignall, Hayley E.}, -doi = {10.3847/0004-637x/817/2/176}, -eprint = {1512.03411}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tuntsov et al. - 2016 - Dynamic Spectral Mapping of Interstellar Plasma Lenses(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {176}, -title = {{Dynamic Spectral Mapping of Interstellar Plasma Lenses}}, -url = {http://arxiv.org/abs/1512.03411%0Ahttp://dx.doi.org/10.3847/0004-637X/817/2/176}, -volume = {817}, -year = {2016} -} -@article{Dekel2009b, -abstract = {The massive galaxies in the young universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids (Genzel et al. 2006, 2008). Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are stream-fed galaxies, formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes (Dekel {\&} Birnboim 2006; Keres et al. 2005). A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duy cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid (Noguchi 1999; Genzel et al. 2008, Elmegreen, Bournaud {\&} Elmegreen 2008, Dekel, Sari {\&} Ceverino 2009). This stream-driven scenario for the formation of disks and spheroids is an alternative to the merger picture.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {https://ui.adsabs.harvard.edu/%7B%5C#%7Dabs/2009Natur.457..451D/abstract}, -volume = {457}, -year = {2009} -} -@article{Kochanek2021, -abstract = {The two properties of the radial mass distribution of a gravitational lens that are well constrained by Einstein rings are the Einstein radius RE and $\zeta$2 = RE$\alpha$″(RE)/(1 - $\kappa$E), where $\alpha$″(RE) and $\kappa$E are the second derivative of the deflection profile and the convergence at RE, respectively. However, if there is a tight mathematical relationship between the radial mass profile and the angular structure, as is true of ellipsoids, an Einstein ring can appear to strongly distinguish radial mass distributions with the same $\zeta$2. This problem is beautifully illustrated by the ellipsoidal models in Millon et al. When using Einstein rings to constrain the radial mass distribution, the angular structure of the models must contain all the degrees of freedom expected in nature (e.g. external shear, different ellipticities for the stars and the dark matter, modest deviations from elliptical structure, modest twists of the axes, modest ellipticity gradients, etc.) that work to decouple the radial and angular structures of the gravity. Models of Einstein rings with too few angular degrees of freedom will lead to strongly biased likelihood distinctions between radial mass distributions and very precise but inaccurate estimates of H0 based on gravitational lens time delays.}, -archivePrefix = {arXiv}, -arxivId = {2003.08395}, -author = {Kochanek, C. S.}, -doi = {10.1093/mnras/staa4033}, -eprint = {2003.08395}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Kochanek2020radialangular.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cosmological parameters,distance scale,gravitational lensing: strong}, -number = {4}, -pages = {5021--5028}, -title = {{Overconstrained models of time delay lenses redux: How the angular tail wags the radial dog}}, -volume = {501}, -year = {2021} -} -@article{Salucci2019, -abstract = {The distribution of the non-luminous matter in galaxies of different luminosity and Hubble type is much more than a proof of the existence of dark particles governing the structures of the Universe. Here, we will review the complex but well-ordered scenario of the properties of the dark halos also in relation with those of the baryonic components they host. Moreover, we will present a number of tight and unexpected correlations between selected properties of the dark and the luminous matter. Such entanglement evolves across the varying properties of the luminous component and it seems to unequivocally lead to a dark particle able to interact with the Standard Model particles over cosmological times. This review will also focus on whether we need a paradigm shift, from pure collisionless dark particles emerging from “first principles”, to particles that we can discover only by looking to how they have designed the structure of the galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1811.08843}, -author = {Salucci, Paolo}, -doi = {10.1007/s00159-018-0113-1}, -eprint = {1811.08843}, -issn = {09354956}, -journal = {Astronomy and Astrophysics Review}, -keywords = {Cosmology,Dark matter,Elementary particles,Galaxies}, -number = {1}, -title = {{The distribution of dark matter in galaxies}}, -volume = {27}, -year = {2019} -} -@article{Agustsson2007a, -abstract = {We investigate the locations of the satellites of relatively isolated host galaxies in the Sloan Digital Sky Survey and the Millennium Run simulation. Provided we use two distinct prescriptions to embed luminous galaxies within the simulated dark matter halos (ellipticals share the shapes of their halos, while disks have angular momenta that are aligned with the net angular momenta of their halos), we find a fair agreement between observation and theory. Averaged over scales rp 500 kpc, the satellites of red, high-mass hosts with low star formation rates are found preferentially near the major axes of their hosts. In contrast, the satellites of blue, low-mass hosts with low star formation rates show little to no anisotropy when averaged over the same scale. The difference between the locations of the satellites of red and blue hosts cannot be explained by the effects of interlopers in the data. Instead, it is caused primarily by marked differences in the dependence of the mean satellite location, $\phi$, on the projected distance at which the satellites are found. We also find that the locations of red, high-mass satellites with low star formation rates show considerably more anisotropy than do the locations of blue, low-mass satellites with high star formation rates. There are two contributors to this result. First, the blue satellites have only recently arrived within their hosts' halos, while the red satellites arrived in the far distant past. Second, the sample of blue satellites is heavily contaminated by interlopers, which suppresses the measured anisotropy compared to the intrinsic anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {0704.3441}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1088/0004-637X/709/2/1321}, -eprint = {0704.3441}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: dwarf,Galaxies: fundamental parameters,Galaxies: halos,Galaxies: structure}, -number = {2}, -pages = {1321--1336}, -title = {{Anisotropic locations of satellite galaxies: Clues to the orientations of galaxies within their dark matter halos}}, -url = {http://arxiv.org/abs/0704.3441%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/0004-637X/709/2/1321}, -volume = {709}, -year = {2010} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ {\textgreater} 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright}2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -volume = {786}, -year = {2014} -} -@article{Talbot2018, -abstract = {We present a catalogue of 38 spectroscopically detected strong galaxy-galaxy gravitational lens candidates identified in the Sloan Digital Sky Survey IV (SDSS-IV). We were able to simulate narrow-band images for eight of them demonstrating evidence of multiple images. Two of our systems are compound lens candidates, each with two background source-planes. One of these compound systems shows clear lensing features in the narrow-band image. Our sample is based on 2812 galaxies observed by the Mapping Nearby Galaxies at APO (MaNGA) integral field unit (IFU). This Spectroscopic Identification of Lensing Objects (SILO) survey extends the methodology of the Sloan Lens ACS Survey (SLACS) and BOSS Emission-Line Survey (BELLS) to lower redshift and multiple IFU spectra. We searched {\$\sim${}}1.5 million spectra, of which 3065 contained multiple high signal-to-noise ratio background emission-lines or a resolved [OII] doublet, that are included in this catalogue. Upon manual inspection, we discovered regions with multiple spectra containing background emission-lines at the same redshift, providing evidence of a common source-plane geometry which was not possible in previous SLACS and BELLS discovery programs. We estimate more than half of our candidates have an Einstein radius ≳ 1.7 arcsec, which is significantly greater than seen in SLACS and BELLS. These larger Einstein radii produce more extended images of the background galaxy increasing the probability that a background emission-line will enter one of the IFU spectroscopic fibres, making detection more likely.}, -archivePrefix = {arXiv}, -arxivId = {1803.03604}, -author = {Talbot, Michael S and Brownstein, Joel R and Bolton, Adam S and Bundy, Kevin and Andrews, Brett H and Cherinka, Brian and Collett, Thomas E and More, Anupreeta and More, Surhud and Sonnenfeld, Alessandro and Vegetti, Simona and Wake, David A and Weijmans, Anne Marie and Westfall, Kyle B}, -doi = {10.1093/mnras/sty653}, -eprint = {1803.03604}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: General,Gravitational lensing: Strong}, -number = {1}, -pages = {195--209}, -title = {{SDSS-IV MaNGA: The spectroscopic discovery of strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1803.03604%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty653}, -volume = {477}, -year = {2018} -} -@article{Diemand2007, -abstract = {We use the ``Via Lactea'' simulation to study the co-evolution of a Milky Way-size LambdaCDM halo and its subhalo population. While most of the host halo mass is accreted over the first 6 Gyr in a series of major mergers, the physical mass distribution [not M_vir(z)] remains practically constant since z=1. The same is true in a large sample of LambdaCDM galaxy halos. Subhalo mass loss peaks between the turnaround and virialization epochs of a given mass shell, and declines afterwards. 97% of the z=1 subhalos have a surviving bound remnant at the present epoch. The retained mass fraction is larger for initially lighter subhalos: satellites with maximum circular velocities Vmax=10 km/s at z=1 have today about 40% of their mass back then. At the first pericenter passage a larger average mass fraction is lost than during each following orbit. Tides remove mass in substructure from the outside in, leading to higher concentrations compared to field halos of the same mass. This effect, combined with the earlier formation epoch of the inner satellites, results in strongly increasing subhalo concentrations towards the Galactic center. We present individual evolutionary tracks and present-day properties of the likely hosts of the dwarf satellites around the Milky Way. The formation histories of ``field halos'' that lie today beyond the Via Lactea host are found to strongly depend on the density of their environment. This is caused by tidal mass loss that affects many field halos on eccentric orbits.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0703337}, -author = {Diemand, Jurg and Kuhlen, Michael and Madau, Piero}, -doi = {10.1086/520573}, -eprint = {0703337}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Cosmology: Dark Matter,Cosmology: Theory,Galaxies: Dwarf,Galaxies: Formation,Galaxies: Halos,Methods: Numerical}, -month = {oct}, -number = {2}, -pages = {859--877}, -primaryClass = {astro-ph}, -title = {{Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure}}, -url = {http://arxiv.org/abs/astro-ph/0703337%0Ahttp://dx.doi.org/10.1086/520573}, -volume = {667}, -year = {2007} -} -@article{Vogelsberger2014, -abstract = {We introduce the Illustris Project, a series of large-scale hydrodynamical simulations of galaxy formation. The highest resolution simulation, Illustris-1, covers a volume of (106.5 Mpc)3, has a dark mass resolution of 6.26 × 106M⊙, and an initial baryonic matter mass resolution of 1.26 × 106M⊙. At z = 0 gravitational forces are softened on scales of 710 pc, and the smallest hydrodynamical gas cells have an extent of 48 pc. We follow the dynamical evolution of 2 × 18203 resolution elements and in addition passively evolve 18203 Monte Carlo tracer particles reaching a total particle count of more than 18 billion. The galaxy formation model includes: Primordial and metal-line cooling with self-shielding corrections, stellar evolution, stellar feedback, gas recycling, chemical enrichment, supermassive black hole growth, and feedback from active galactic nuclei. Here we describe the simulation suite, and contrast basic predictions of our model for the present-day galaxy population with observations of the local universe. At z = 0 our simulation volume contains about 40 000 well-resolved galaxies covering a diverse range of morphologies and colours including early-type, late-type and irregular galaxies. The simulation reproduces reasonably well the cosmic star formation rate density, the galaxy luminosity function, and baryon conversion efficiency at z = 0. It also qualitatively captures the impact of galaxy environment on the red fractions of galaxies. The internal velocity structure of selected well-resolved disc galaxies obeys the stellar and baryonic Tully-Fisher relation together with flat circular velocity curves. In the well-resolved regime, the simulation reproduces the observed mix of early-type and late-type galaxies. Our model predicts a halo mass dependent impact of baryonic effects on the halo mass function and the masses of haloes caused by feedback from supernova and active galactic nuclei.}, -archivePrefix = {arXiv}, -arxivId = {1405.2921}, -author = {Vogelsberger, Mark and Genel, Shy and Springel, Volker and Torrey, Paul and Sijacki, Debora and Xu, Dandan and Snyder, Greg and Nelson, Dylan and Hernquist, Lars}, -doi = {10.1093/mnras/stu1536}, -eprint = {1405.2921}, -isbn = {9781424441235}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: Theory,Methods: Numerical}, -month = {oct}, -number = {2}, -pages = {1518--1547}, -pmid = {21096380}, -title = {{Introducing the illustris project: Simulating the coevolution of dark and visible matter in the universe}}, -volume = {444}, -year = {2014} -} -@article{Huang2018, -abstract = {We use {\$\sim${}}100 deg2 of deep ({\textgreater} 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach {\$\sim${}}4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) {\textgreater} 11.6 in more massive haloes at 0.3 {\textless} z {\textless} 0.5 have shallower inner stellar mass density profiles (within {\$\sim${}}10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) {\textgreater} 14.0 are {\$\sim${}}20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{Morganti2013, -abstract = {NGC 4494 is one of several intermediate-luminosity elliptical galaxies inferred to have an unusually diffuse dark matter halo. We use the $\chi$2-made-to-measure particle code nmagic to construct axisymmetric models of NGC 4494 from photometric and various kinematic data. The extended kinematics include light spectra in multiple slitlets out to 3.5Re, and hundreds of planetary nebula velocities out to ≃7Re, thus allowing us to probe the dark matter content and orbital structure in the halo. We use Monte Carlo simulations to estimate confidence boundaries for the halo parameters, given our data and modelling set-up. We find that the true potential of the dark matter halo is recovered within $\Delta$G (merit function) ≲ 26 ($\Delta$$\chi$2 ≲ 59) at the 70 per cent confidence level (CL), and within $\Delta$G ≲ 32 ($\Delta$$\chi$2 ≲ 70) at the 90 per cent CL. These numbers are much larger than the usually assumed $\Delta$$\chi$2 2.3 (4.6) for the 70 per cent (90 per cent) CL for two free parameters, perhaps case dependent, but calling into question the general validity of the standard assumptions used for halo and black hole mass determinations. The best-fitting models for NGC 4494 have a dark matter fraction of about 0.6 ± 0.1 at 5Re (70 per cent CL) and are embedded in a dark matter halo with circular velocity ∼200 km s-1. The total circular velocity curve (CVC) is approximately flat at vc 220 km s-1 outside ∼0.5Re. The orbital anisotropy of the stars is moderately radial. These results are independent of the assumed inclination of the galaxy, and edge-on models are preferred. Comparing with the haloes of NGC 3379 and NGC 4697, whose velocity dispersion profiles also decrease rapidly from the centre outwards, the outer CVCs and dark matter haloes are quite similar. NGC 4494 shows a particularly high dark matter fraction inside ∼ 3Re, and a strong concentration of baryons in the centre. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.2688}, -author = {Morganti, Lucia and Gerhard, Ortwin and Coccato, Lodovico and Martinez-valpuesta, Inma and Arnaboldi, Magda}, -doi = {10.1093/mnras/stt442}, -eprint = {1303.2688}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: individual: NGC 4494,Galaxies: kinematics and dynamics,Methods: numerical,cD}, -number = {4}, -pages = {3570--3588}, -title = {{Elliptical galaxies with rapidly decreasing velocity dispersion profiles: Nmagic models and dark halo parameter estimates for NGC 4494}}, -volume = {431}, -year = {2013} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M* > 1011M⊙ galaxies at 1 < z < 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 < z < 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V. A. and Dunlop, J. S. and McLure, R. J. and Cirasuolo, M. and Buitrago, F. and Bowler, R. A.A. and Targett, T. A. and Bell, E. F. and McIntosh, D. H. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Hartley, W. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and McGrath, E. J.}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure}, -month = {oct}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 < z < 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{VanDerWel2013, -abstract = {Using spectroscopy from the Large Binocular Telescope and imaging from the Hubble Space Telescope we discovered the first strong galaxy lens at z lens > 1. The lens has a secure photometric redshift of z = 1.53 ± 0.09 and the source is spectroscopically confirmed at z = 3.417. The Einstein radius (0.″35; 3.0 kpc) encloses 7.6 × 1010 M⊙, with an upper limit on the dark matter fraction of 60%. The highly magnified (40×) source galaxy has a very small stellar mass (∼108 M⊙) and shows an extremely strong [O III]5007{\AA} emission line (EW0 ∼ 1000 {\AA}) bolstering the evidence that intense starbursts among very low-mass galaxies are common at high redshift. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1309.2826}, -author = {{Van Der Wel}, A. and {Van De Ven}, G. and Maseda, M. and Rix, H. W. and Rudnick, G. H. and Grazian, A. and Finkelstein, S. L. and Koo, D. C. and Faber, S. M. and Ferguson, H. C. and Koekemoer, A. M. and Grogin, N. A. and Kocevski, D. D.}, -doi = {10.1088/2041-8205/777/1/L17}, -eprint = {1309.2826}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/VanDerWel2013QUADM25.pdf:pdf}, -issn = {20418205}, -journal = {ApJL}, -keywords = {gravitational lensing: strong}, -number = {1}, -title = {{Discovery of a quadruple lens in candels with a record lens redshift z = 1.53}}, -volume = {777}, -year = {2013} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the 'Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a (100 cMpc)3 and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts 0 and 1, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar 'downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of Mstar{\textgreater}10{\^{}}11Msolar galaxies at 1{\textless}z{\textless}3 in the CANDELS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disk components according to their H(160)-band morphologies. By extending this analysis to multiple bands we have been able to conduct individual bulge and disk component SED fitting which has provided us with stellar-mass and star-formation rate estimates for the separate bulge and disk components. These have been combined with size measurements to explore the evolution of these massive high-redshift galaxies. By utilising the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the disks. This can be seen from both the fraction of bulge components which lie below the local relation and the median sizes of the bulge components, where the bulges are a median factor of 2.93+/-0.32 times smaller than similarly massive local galaxies at 1{\textless}z{\textless}2 and 3.41+/-0.58 smaller at 2{\textless}z{\textless}3; for the disks the corresponding factors are 1.65+/-0.14 and 1.99+/-0.25. Moreover, by splitting our sample into the passive and star-forming bulge and disk sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming disks are larger, while the passive disks have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-Sersic fits and adopting the overall star-formation rates. Finally, by evolving the star-formation histories of the passive disks back to the redshifts when the passive disks were last active, we show that the passive and star-forming disks have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{Spavone2017, -abstract = {Observations of diffuse starlight in the outskirts of galaxies are thought to be a fundamental source of constraint on the cosmological context of galaxy assembly in the $\Lambda$CDM model. Such observations are not trivial because of the extreme faintness of such regions. In this work, we investigated the photometric properties of six massive early-type galaxies (ETGs) in the VEGAS sample (NGC 1399, NGC 3923, NGC 4365, NGC 4472, NGC 5044, and NGC 5846) out to extremely low surface brightness levels with the goal of characterizing the global structure of their light profiles for comparison to state-of-the-art galaxy formation models. We carried out deep and detailed photometric mapping of our ETG sample taking advantage of deep imaging with VST/OmegaCAM in the g and i bands. By fitting the light profiles, and comparing the results to simulations of elliptical galaxy assembly, we have identified signatures of a transition between relaxed and unrelaxed accreted components and can constrain the balance between in situ and accreted stars. The very good agreement of our results with predictions from theoretical simulations demonstrates that the full VEGAS sample of $\sim$100 ETGs will allow us to use the distribution of diffuse light as a robust statistical probe of the hierarchical assembly of massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1703.10835}, -author = {Spavone, Marilena and Capaccioli, Massimo and Napolitano, Nicola R. and Iodice, Enrichetta and Grado, Aniello and Limatola, Luca and Cooper, Andrew P. and Cantiello, Michele and Forbes, Duncan A. and Paolillo, Maurizio and Schipani, Pietro}, -doi = {10.1051/0004-6361/201629111}, -eprint = {1703.10835}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Spavone et al. - 2017 - VEGAS A VST Early-type GAlaxy Survey II. Photometric study of giant ellipticals and their stellar halos(2).pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: halos,Techniques: image processing}, -number = {3}, -pages = {A38}, -title = {{VEGAS: A VST Early-type GAlaxy Survey: II. Photometric study of giant ellipticals and their stellar halos}}, -url = {http://www.aanda.org/10.1051/0004-6361/201629111}, -volume = {603}, -year = {2017} -} -@article{Dekel2009b, -abstract = {The massive galaxies in the young universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids (Genzel et al. 2006, 2008). Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are stream-fed galaxies, formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes (Dekel {\&} Birnboim 2006; Keres et al. 2005). A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duy cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid (Noguchi 1999; Genzel et al. 2008, Elmegreen, Bournaud {\&} Elmegreen 2008, Dekel, Sari {\&} Ceverino 2009). This stream-driven scenario for the formation of disks and spheroids is an alternative to the merger picture.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/19158792}, -volume = {457}, -year = {2009} -} -@article{Gavazzi2006, -abstract = {We report the discovery of two concentric Einstein rings around the gravitational lens SDSS J0946+1006. The main lens is at redshift zl = 0.222, while the inner ring (1) is at redshift zs1 = 0.609 (E Ein1 = 1.43″ ± 0.01″). The wider image separation (REin2 = 2.07″ ± 0.02″) of the outer ring (2) implies a higher redshift than that of ring 1; the detection of ring 2 in the F814W ACS filter implies an upper limit of zs2 ≲ 6.9. The main lens can be described by a power-law total mass density profile $\rho$tot ∏ r-$\gamma$′ with $\gamma$′ = 2.00 ±0.03 and velocity dispersion $\sigma$SIE = 287 ± 5 km s-1 (the stellar velocity dispersion is $\sigma$v, * = 284 ± 24 km s_1). The strong lensing configuration is inconsistent with light traces mass. Adopting a prior on the stellar mass-to-light ratio from previous SLACS work, we infer a 73% ±9% dark matter fraction within the cylinder of radius equal to the effective radius of the lens. We find that, for the case of SDSS J0946+1006, the geometry of the two rings does not place interesting constraints on cosmography because of the suboptimal redshifts of lens and sources. We then consider the perturbing effect of the mass associated with ring 1 building a compound lens model. This introduces minor changes to the mass of the main lens and provides an estimate of zs2 = 3.1-1.0+2.0 and of the mass of the source responsible for ring 1 ($\sigma$SIE, sl = 94-47-27 km s-1). We conclude by examining the prospects of doing cosmography with a sample of 50 double rings, expected from future space-based surveys. Accounting for uncertainties in the mass profile of the lens and the effects of the perturber, we find that such a sample would constrain $\Omega$m and w within 10%, assuming flatness. {\textcopyright} 2008. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0801.1555}, -author = {Gavazzi, Rapha{\"{e}}l and Treu, Tommaso and Koopmans, L{\'{e}}on V. E. and Bolton, Adam S. and Moustakas, Leonidas A. and Burles, Scott and Marshall, Philip J.}, -doi = {10.1086/529541}, -eprint = {0801.1555}, -isbn = {0004-637x}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {1046--1059}, -title = {{The Sloan Lens ACS Survey. VI. Discovery and Analysis of a Double Einstein Ring1}}, -url = {http://stacks.iop.org/0004-637X/677/i=2/a=1046}, -volume = {677}, -year = {2008} -} -@article{Geometryed, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(14).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Wang2025, -abstract = {The stellar-to-halo mass relation (SHMR) embodies the joint evolution of galaxies and their host dark matter halos. However, the relation is poorly constrained at sub-galactic masses, because the stellar emission from such objects is so faint. However, it is possible to directly detect the mass of halos along the line of sight to a strong gravitational lens, when they perturb one of its multiple images. Space telescopes including Euclid, CSST, and Roman will soon discover millions of galaxy-galaxy strong lensing systems. We simulate Euclid-like imaging of a typical lens galaxy, and find that a lensing reconstruction is sensitive to $3\times10^{10}$ subhalos with various positions and concentrations, at statistical signficance $>$$3.6\sigma$. The subhalo mass can be measured without bias, provided the model simultaneously fits light from both the main lens and the subhalo. A future sample of 48 subhalos with $\geqslant$$5\sigma$ detection significance would constrain the SHMR at this mass range with $1\sigma$ uncertainty of 0.045 dex: distinguishing between different theoretical predictions at the sub-galactic scale. Follow-up spectroscopy is needed to measure lens and source redshifts; follow-up imaging at greater spatial resolution and depth would substantially improve the measurement, and eliminate false-positives at even lower halo masses.}, -archivePrefix = {arXiv}, -arxivId = {2501.16139}, -author = {Wang, Kaihao and Cao, Xiaoyue and Li, Ran and Nightingale, James W. and He, Qiuhan and Amvrosiadis, Aristeidis and Massey, Richard and von Wietersheim-Kramsta, Maximilian and Fung, Leo W. H. and Frenk, Carlos S. and Cole, Shaun and Robertson, Andrew and Lange, Samuel C. and Ma, Xianghao}, -eprint = {2501.16139}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Wang2025SLEuclid.pdf:pdf}, -journal = {Submitted to MNRAS}, -keywords = {dark matter,evolution,galaxies,gravitational lensing,strong}, -number = {January}, -pages = {1--11}, -title = {{Measuring the Stellar-to-Halo Mass Relation at $\sim10^{10}$ Solar masses, using space-based imaging of galaxy-galaxy strong lenses}}, -url = {http://arxiv.org/abs/2501.16139}, -volume = {11}, -year = {2025} -} -@article{Hopkins2011, -abstract = {We present analytic calculations of angular momentum transport and gas inflow in galaxies, from scales of $\sim$kpc to deep inside the potential of a central massive black hole (BH). We compare these analytic calculations to numerical simulations and use them to develop a sub-grid model of BH growth that can be incorporated into semi-analytic calculations or cosmological simulations. Motivated by both analytic calculations and simulations of gas inflow in galactic nuclei, we argue that the strongest torque on gas arises when non-axisymmetric perturbations to the stellar gravitational potential produce orbit crossings and shocks in the gas. This is true both at large radii $\sim$0.01-1kpc, where bar-like stellar modes dominate the non-axisymmetric potential, and at smaller radii ≲10pc, where a lopsided/eccentric stellar disc dominates. The traditional orbit-crossing criterion is not always adequate to predict the locations of, and inflow due to, shocks in gas+stellar discs with finite sound speeds. We derive a modified criterion that predicts the presence of shocks in stellar-dominated systems even absent formal orbit crossing. We then derive analytic expressions for the loss of angular momentum and the resulting gas inflow rates in the presence of such shocks. We test our analytic predictions using hydrodynamic simulations at a range of galactic scales, and show that they successfully predict the mass inflow rates and quasi-steady gas surface densities with a small scatter ≃0.3dex. We use our analytic results to construct a new estimate of the BH accretion rate given galaxy properties at larger radii, for use in galaxy and cosmological simulations and semi-analytic models. While highly simplified, this accretion rate predictor captures the key scalings in the numerical simulations. By contrast, alternate estimates such as the local viscous accretion rate or the spherical Bondi rate fail systematically to reproduce the simulations and have significantly larger scatter. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1007.2647}, -author = {Hopkins, Philip F. and Quataert, Eliot}, -doi = {10.1111/j.1365-2966.2011.18542.x}, -eprint = {1007.2647}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins, Quataert - 2011 - An analytic model of angular momentum transport by gravitational torques From galaxies to massive black ho(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Quasars: general}, -number = {2}, -pages = {1027--1050}, -title = {{An analytic model of angular momentum transport by gravitational torques: From galaxies to massive black holes}}, -volume = {415}, -year = {2011} -} -@article{Naab2009, -abstract = {Using a high-resolution hydrodynamical cosmological simulation of the formation of a massive spheroidal galaxy we show that elliptical galaxies can be very compact and massive at high redshift in agreement with recent observations. Accretion of stripped infalling stellar material increases the size of the system with time and the central concentration is reduced by dynamical friction of the surviving stellar cores. In a specific case of a spheroidal galaxy with a final stellar mass of 1.5 × 1011 M ⊙ we find that the effective radius re increases from 0.7 ± 0.2 kpc at z = 3 to re = 2.4 ± 0.4 kpc at z = 0 with a concomitant decrease in the effective density of an order of magnitude and a decrease of the central velocity dispersion by approximately 20{\%} over this time interval. A simple argument based on the virial theorem shows that during the accretion of weakly bound material (minor mergers) the radius can increase as the square of the mass in contrast to the usual linear rate of increase for major mergers. By undergoing minor mergers compact high-redshift spheroids can evolve into present-day systems with sizes and concentrations similar to observed local ellipticals. This indicates that minor mergers may be the main driver for the late evolution of sizes and densities of early-type galaxies. {\textcopyright}2009 The American Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {0903.1636}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P}, -doi = {10.1088/0004-637X/699/2/L178}, -eprint = {0903.1636}, -issn = {2041-821}, -journal = {Astrophysical Journal Letters}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: interactions,Galaxies: structure,Methods: numerical,cd}, -month = {jul}, -number = {2 PART 2}, -pages = {L178--------L182}, -title = {{Minor mergers and the size evolution of elliptical galaxies}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L178?key=crossref.405faa44137f4be9a7e3800a4c3e7dea}, -volume = {699}, -year = {2010} -} -@article{Vaucouleurs1948, -abstract = {Not Available}, -author = {de Vaucouleurs, G}, -doi = {10.1089/end.2005.19.a287}, -isbn = {3018804090}, -issn = {0892-7790}, -journal = {Journal of Endourology}, -number = {supplement 1}, -pages = {a287----a303}, -title = {{Author Index}}, -url = {http://linkinghub.elsevier.com/retrieve/pii/S0020706313001180}, -volume = {19}, -year = {2005} -} -@article{Deason2011, -abstract = {We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the gimic suite of simulations. gimic consists of resimulations of five cosmologically representative regions from the Millennium Simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r∼ 0.1r200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r∼r200). Misalignments of >45° are seen in ∼30 per cent of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20 per cent of the satellite systems with 10 bright galaxies within r200 exhibit a polar spatial alignment with respect to the galaxy - an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction (∼10 per cent) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z= 0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation - the memory of their accretion history can remain intact to z= 0. Understanding the phase-space distribution of the z= 0 satellite population is key for studies that estimate the host halo mass from the line-of-sight velocities and projected positions of satellite galaxies. We quantify the effects of such systematics in estimates of the host halo mass from the satellite population. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A. J. and Mccarthy, I. G. and Font, A. S. and Evans, N. W. and Frenk, C. S. and Belokurov, V. and Libeskind, N. I. and Crain, R. A. and Theuns, T.}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Deason et al. - 2011 - Mismatch and misalignment Dark haloes and satellites of disc galaxies(2).pdf:pdf}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely, the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since {\$}z=1.0{\$}. We find that lower-mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher-mass or lower-redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys, we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology,gravitational lensing,haloes - galaxies,strong - galaxies,structure -,theory - dark matter}, -number = {2}, -pages = {1824--1848}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {469}, -year = {2017} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G.}, -doi = {10.1086/507084}, -eprint = {0505272}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Agustsson, Brainerd - 2006 - The Locations of Satellite Galaxies in a $\Lambda$CDM Universe(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Veale2016, -abstract = {We present spatially-resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (MK {\textless}{\$\sim${}} -25.7 mag, stellar mass M* {\textgreater}{\$\sim${}} 10{\^{}}11.8 Msun) of the volume-limited (D {\textless}108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650 to 5850 angstroms from the 246-fiber Mitchell integral-field spectrograph (IFS) at McDonald Observatory, covering a 107 x 107 arcsec field of view (often reaching 2 to 3 effective radii). We measure the 2D spatial distribution of each galaxy's angular momentum (lambda and fast or slow rotator status), velocity dispersion (sigma), and higher-order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ({\$\sim${}}80{\%}) of slow and non-rotators with lambda {\textless}{\$\sim${}} 0.2. WHen combined with the lower-mass ETGs in the ATLAS3D survey, we find the fraction of slow rotators to increase dramatically with galaxy mass, reaching {\$\sim${}}50{\%} at MK {\$\sim${}} -25.5 mag and {\$\sim${}}90{\%} at MK {\$\sim${}} 26 mag. All of our fast rotators show a clear anti-correlation between h3 and V/sigma, and the slope of the anti-correlation is steeper in more round galaxies. The radial profiles of sigma show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK {\textless}{\$\sim${}} -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat sigma profiles, whereas five of the seven "isolated" galaxies are all fainter than MK {\$\sim${}} -25.8 mag and have falling sigma. All of our galaxies have positive {\textless}h4{\textgreater}; the most luminous galaxies have {\textless}h4{\textgreater}{\$\sim${}} 0.05 while less luminous galaxies have a range of values between 0 and 0.5. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising sigma profiles. We discuss the implications for the relationship among dynamical mass, sigma, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E and McConnell, Nicholas J and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Dutton2010, -abstract = {Using estimates of dark halo masses from satellite kinematics, weak gravitational lensing and halo abundance matching, combined with the Tully-Fisher (TF) and Faber-Jackson relations, we derive the mean relation between the optical, Vopt, and virial, V200, circular velocities of early- and late-type galaxies at redshift z≃ 0. For late-type galaxies, Vopt≃V200 over the velocity range Vopt= 90-260 km s-1, and is consistent with Vopt=Vmax,h[the maximum circular velocity of NFW dark matter haloes in the concordance $\Lambda$ cold dark matter ($\Lambda$ CDM) cosmology]. However, for early-type galaxies Vopt≠V200, with the exception of early-type galaxies with Vopt≃ 350 km s-1. This is inconsistent with early-type galaxies being, in general, globally isothermal. For low-mass (Vopt≲ 250 km s-1) early-types Vopt > Vmax,h, indicating that baryons have modified the potential well, while high-mass (Vopt > rsim 400 km s-1) early-types have Vopt < Vmax,h. Folding in measurements of the black hole mass-velocity dispersion relation, our results imply that the supermassive black hole-halo mass relation has a logarithmic slope which varies from ≃1.4 at halo masses of ≃ 1012 h-1 M⊙ to ≃0.65 at halo masses of 1013.5 h-1 M⊙. The values of Vopt/V200 we infer for the Milky Way (MW) and M31 are lower than the values currently favoured by direct observations and dynamical models. This offset is due to the fact that the MW and M31 have higher Vopt and lower V200 compared to typical late-type galaxies of the same stellar masses. We show that current high-resolution cosmological hydrodynamical simulations are unable to form galaxies which simultaneously reproduce both the Vopt/V200 ratio and the Vopt-Mstar (Tully-Fisher/Faber-Jackson) relation. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1004.4626}, -author = {Dutton, Aaron A. and Conroy, Charlie and van den Bosch, Frank C. and Prada, Francisco and More, Surhud}, -doi = {10.1111/j.1365-2966.2010.16911.x}, -eprint = {1004.4626}, -isbn = {doi:10.1111/j.1365-2966.2010.16911.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: kinematics and dynamics,Galaxies: spiral}, -month = {sep}, -number = {1}, -pages = {2--16}, -title = {{The kinematic connection between galaxies and dark matter haloes}}, -volume = {407}, -year = {2010} -} -@article{Short2013, -abstract = {The European Space Agency's Gaia mission is scheduled for launch in 2013. It will operate at L2 for 5 years, rotating slowly to scan the sky so that its two optical telescopes will repeatedly observe more than one billion stars. The resulting data set will be iteratively reduced to solve for the position, parallax and proper motion of every observed star. The focal plane contains 106 large area silicon CCDs continuously operating in a mode where the line transfer rate and the satellite rotation are in synchronization. One of the greatest challenges facing the mission is radiation damage to the CCDs which will cause charge deferral and image shape distortion. This is particularly important because of the extreme accuracy requirements of the mission. Despite steps taken at hardware level to minimize the effects of radiation, the residual distortion will need to be calibrated during the pipeline data processing. Due to the volume and inhomogeneity of data involved, this requires a model which describes the effects of the radiation damage which is physically realistic, yet fast enough to implement in the pipeline. The resulting charge distortion model was developed specifically for the Gaia CCD operating mode. However, a generalized version is presented in this paper and this has already been applied in a broader context, for example to investigate the impact of radiation damage on the Euclid dark-energy mission data. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1302.1416}, -author = {Short, A. and Crowley, C. and de Bruijne, J. H.J. and Prod'homm, T.}, -doi = {10.1093/mnras/stt114}, -eprint = {1302.1416}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Short et al. - 2013 - An analytical model of radiation-induced charge transfer inefficiency for CCD detectors.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Astrometry,Instrumentation: detectors,Methods: data analysis,Methods: numerical,Space vehicles}, -number = {4}, -pages = {3078--3085}, -title = {{An analytical model of radiation-induced charge transfer inefficiency for CCD detectors}}, -volume = {430}, -year = {2013} -} -@article{Bingham2019, -abstract = {Pyro is a probabilistic programming language built on Python as a platform for developing advanced probabilistic models in AI research. To scale to large data sets and high-dimensional models, Pyro uses stochastic variational inference algorithms and probability distributions built on top of PyTorch, a modern GPU-accelerated deep learning framework. To accommodate complex or model-specific algorithmic behavior, Pyro leverages Poutine, a library of composable building blocks for modifying the behavior of probabilistic programs.}, -archivePrefix = {arXiv}, -arxivId = {1810.09538}, -author = {Bingham, Eli and Chen, Jonathan P. and Jankowiak, Martin and Obermeyer, F. and Pradhan, Neeraj and Karaletsos, Theofanis and Singh, Rohit and Szerlip, Paul and Horsfall, Paul and Goodman, Noah D.}, -eprint = {1810.09538}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bingham et al. - 2019 - Pyro Deep universal probabilistic programming.pdf:pdf}, -issn = {15337928}, -journal = {Journal of Machine Learning Research}, -keywords = {Approximate Bayesian inference,Deep learning,Generative models,Graphical models,Probabilistic programming}, -number = {Xxxx}, -pages = {0--5}, -title = {{Pyro: Deep universal probabilistic programming}}, -volume = {20}, -year = {2019} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of Super-Massive Black Hole (SMBH) formation and evolution is used, as in Tremmel et al.(2015, 2016), allowing to explicitly follow SMBH dynamics at the center of galaxies. A high SIDM constant cross-section is chosen, {\$}\backslashbackslashsigma{\{}\backslash{\$}{\}}=10 {\$}\backslashbackslashrm cm{\^{}}2/gr{\$}, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in CDM, with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80{\$}\backslashbackslash{\{}\backslash{\%}{\}}{\$} of the SMBH population is off-centered in the SIDM case, as opposed to the CDM case in which {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}90{\$}\backslashbackslash{\{}\backslash{\%}{\}}{\$} of SMBHs have reached their host's centre. SMBHs are found as far as {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction timescale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in 'core stalling'. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@article{Vegetti2014, -abstract = {We present the results of a search for galaxy substructures in a sample of 11 gravitational lens galaxies from the Sloan Lens ACS Survey by Bolton et al. We find no significant detection of mass clumps, except for a luminous satellite in the system SDSS J0956+5110. We use these non-detections, in combination with a previous detection in the system SDSS J0946+1006, to derive constraints on the substructure mass function in massive early-type host galaxies with an average redshift zlens $\sim$0.2 and an average velocity dispersion seff $\sim$270 km s-1. We perform a Bayesian inference on the substructure mass function, within a median region of about 32 kpc2 around the Einstein radius (Rein $\sim$4.2 kpc). We infer a mean projected substructure mass fraction f = 0.0076+0.0208-0.0052 at the 68 per cent confidence level and a substructure mass function slopea < 2.93 at the 95 per cent confidence level for a uniform prior probability density on a. For a Gaussian prior based on cold dark matter (CDM) simulations, we infer f = 0.0064+0.0080-0.0042 and a slope of a =1.90+0.098-0.098 at the 68 per cent confidence level. Since only one substructure was detected in the full sample, we have little information on the mass function slope, which is therefore poorly constrained (i.e. the Bayes factor shows no positive preference for any of the two models). The inferred fraction is consistent with the expectations from CDM simulations and with inference from flux ratio anomalies at the 68 per cent confidence level. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1405.3666}, -author = {Vegetti, S. and Koopmans, L. V.E. and Auger, M. W. and Treu, T. and Bolton, A. S.}, -doi = {10.1093/mnras/stu943}, -eprint = {1405.3666}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies,Structure}, -month = {aug}, -number = {3}, -pages = {2017--2035}, -title = {{Inference of the cold dark matter substructure mass function at z = 0.2 using strong gravitational lenses}}, -volume = {442}, -year = {2014} -} -@article{Gow2016, -abstract = {{\textcopyright}2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P D and Murray, Neil J}, -doi = {10.1117/12.2232706}, -isbn = {9781510602090}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{Herbert-Fort2007, -abstract = {We measure the distribution of velocities for prograde and retrograde satellite galaxies using a combination of published data and new observations for 78 satellites of 63 extremely isolated disc galaxies (169 satellites total). We find that the velocity distribution is non-Gaussian ({\textgreater}99.9 per cent confidence), but that it can be described as the sum of two Gaussians, one of which is broad ($\sigma$ = 176 ± 15 km s-1), has a mean prograde velocity of 86 ± 30 km s-1, and contains ∼55 per cent of the satellites, while the other is slightly retrograde with a mean velocity of -21 ± 22 km s-1 and $\sigma$ = 74 ± 18 km s-1 and contains ∼45 per cent of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy, and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Hoekstra2004, -abstract = {We present the results of a study of weak lensing by galaxies based on 45.5 deg{\$}{\^{}}2{\$} of {\$}R{\_}C{\$} band imaging data from the Red-Sequence Cluster Survey (RCS). We present the first weak lensing detection of the flattening of galaxy dark matter halos. We use a simple model in which the ellipticity of the halo is {\$}f{\$} times the observed ellipticity of the lens. We find a best fit value of {\$}f=0.77{\^{}}{\{}+0.18{\}}{\_}{\{}-0.21{\}}{\$}, suggesting that the dark matter halos are somewhat rounder than the light distribution. The fact that we detect a significant flattening implies that the halos are well aligned with the light distribution. Given the average ellipticity of the lenses, this implies a halo ellipticity of {\$}{\textless}e{\_}{\{}\backslashrm halo{\}} {\textgreater}=0.33{\^{}}{\{}+0.07{\}}{\_}{\{}-0.09{\}}{\$}, in fair agreement with results from numerical simulations of CDM. This result provides strong support for the existence of dark matter, as an isotropic lensing signal is excluded with 99.5{\%} confidence. We also study the average mass profile around the lenses, using a maximum likelihood analysis. We consider two models for the halo mass profile: a truncated isothermal sphere (TIS) and an NFW profile. We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo. The best fit NFW model yields a mass {\$}M{\_}{\{}200{\}}=(8.4\backslashpm0.7\backslashpm0.4)\backslashtimes 10{\^{}}{\{}11{\}} h{\^{}}{\{}-1{\}} M{\_}\backslashodot{\$} and a scale radius {\$}r{\_}s=16.2{\^{}}{\{}+3.6{\}}{\_}{\{}-2.9{\}} h{\^{}}{\{}-1{\}}{\$} kpc. This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, H K C and Gladders, Michael D}, -doi = {10.1086/382726}, -eprint = {0306515}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of Galaxy Dark Matter Halos from Weak Lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2004} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the foreground lenses and background sources are early-type galaxies. Using imaging from Hubble Space Telescope (HST)/Advanced Camera for Studies (ACS) andKeck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population ofmassive, compact galaxies at redshifts 0.4 ≲ z ≲ 0.7, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of highredshift red nuggets or their partly evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar populations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S{\'{e}}rsic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still compact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterized by red-to-blue colour gradients as a function of radius which are stronger at low redshift - indicative of ongoing accretion - but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are pre-dominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W and Fassnacht, Christopher D and Treu, Tommaso and Brewer, Brendon J and Koopmans, L V E and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Peng2010, -abstract = {We present a two-dimensional (2D) fitting algorithm (GALFIT, ver. 3) with new capabilities to study the structural components of galaxies and other astronomical objects in digital images. Our technique improves on previous 2D fitting algorithms by allowing for irregular, curved, logarithmic and power-law spirals, ring, and truncated shapes in otherwise traditional parametric functions like the S{\'{e}}rsic, Moffat, King, Ferrer, etc., profiles. One can mix and match these new shape features freely, with or without constraints, and apply them to an arbitrary number of model components of numerous profile types, so as to produce realistic-looking galaxy model images. Yet, despite the potential for extreme complexity, the meaning of the key parameters like the S{\'{e}}rsic index, effective radius, or luminosity remains intuitive and essentially unchanged. The new features have an interesting potential for use to quantify the degree of asymmetry of galaxies, to quantify low surface brightness tidal features beneath and beyond luminous galaxies, to allow more realistic decompositions of galaxy subcomponents in the presence of strong rings and spiral arms, and to enable ways to gauge the uncertainties when decomposing galaxy subcomponents. We illustrate these new features by way of several case studies that display various levels of complexity. {\textcopyright}2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0912.0731}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans Walter}, -doi = {10.1088/0004-6256/139/6/2097}, -eprint = {0912.0731}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Galaxies: bulges,Galaxies: fundamental parameters,Galaxies: structure,Techniques: image processing,Techniques: photometric}, -number = {6}, -pages = {2097--2129}, -title = {{Detailed decomposition of galaxy images. II. beyond axisymmetric models}}, -volume = {139}, -year = {2010} -} -@article{Li2008, -abstract = {We report the discovery that substructures/subhaloes of a galaxy-size halo tend to fall in together in groups in cosmological simulations, something that may explain the oddity of the MW satellite distribution. The original clustering at the time of infall is still discernible in the angular momenta of the subhaloes even for events which took place up to eight Gyrs ago, {\$}z \backslashbackslashsim 1{\$}. This phenomenon appears to be rather common since at least 1/3 of the present-day subhaloes have fallen in groups in our simulations. Hence, this may well explain the Lynden-Bell {\&} Lynden-Bell ghostly streams. We have also found that the probability of building up a flattened distribution similar to the MW satellites is as high as {\$}\backslashbackslashsim 80{\%}{\$} if the MW satellites were from only one group and {\$}\backslashbackslashsim 20{\%}{\$} when five groups are involved. Therefore, we conclude that the `peculiar' distribution of satellites around the MW can be expected with the CDM structure formation theory. This non-random assignment of satellites to subhaloes implies an environmental dependence on whether these low-mass objects are able to form stars, possibly related to the nature of reionization in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {0807.2780}, -author = {Li, Yang Shyang and Helmi, Amina}, -doi = {10.1007/978-1-4020-5573-7_53}, -eprint = {0807.2780}, -isbn = {0000000000000}, -issn = {15706605}, -journal = {Astrophysics and Space Science Proceedings}, -keywords = {Dark matter,Galaxies: Dwarf,Galaxies: Kinematics and dynamics,Galaxy: Formation,Methods: Numerical}, -number = {202409}, -pages = {311--314}, -title = {{Infall of substructures onto a milky way-like dark halo}}, -volume = {385}, -year = {2007} -} -@article{Hopkins2010, -abstract = {Observations have shown that massive galaxies at high redshift have much smaller effective radii than galaxies of similar mass today; however, recent work has shown that they have similar central densities. The primary growth of size, therefore, relates to the apparent relative abundance of low-density material at low redshifts. But various models have been proposed to accomplish this, and the exact contribution of these mechanisms, relative to others that would, for example, lower the density of the system uniformly, or relate to possible observational misestimates of the stellar mass distribution, remain uncertain, as does the degree to which this evolution is driven by processes of initial spheroid formation versus subsequent 'dry' assembly of spheroids. These different possibilities also yield dramatically different constraints on any possible evolution in the MBH-$\sigma$ relation. Here, we compile observations of spheroid properties as a function of redshift and use them to test the different proposed models, each of which we have calibrated and studied in a suite of high-resolution hydrodynamic simulations. We show that the evolution in progenitor disc gas fractions with redshift gives rise to the initial formation of smaller spheroids at high redshift. We then consider how these early-forming systems must evolve to be consistent with the larger sizes of old spheroids today. We consider (1) equal-density 'dry' mergers, (2) later major or minor 'dry' mergers with less dense galaxies, (3) adiabatic expansion, after significant gas mass loss, (4) gradients in stellar mass-to-light ratios from young nuclear stellar populations (yielding smaller Re at early times, which vanish as the system fades), (5) biases in the stellar mass estimation of high-redshift (young) systems (from e.g. uncertain asymptotic giant branch starlight contributions) and (6) observational effects (possible biases in fitting or missed light from surface brightness dimming, or the effects of different definitions of effective radii). In principle, any of these models could be tuned to explain any observed effective radius evolution. However, the predicted evolution in velocity dispersions, central stellar mass surface densities and profile shape are very distinct. Comparing with observations, only model (2), later or minor 'dry' mergers with less dense systems, is consistent with the constraints as an explanation of the entire effect. Moreover, it is the only model which allows for any evolution in M BH-$\sigma$ towards more massive black holes (BHs) at high redshift. Still, the amount of merging needed for this to explain the observed factor of ∼6 size evolution is larger than that predicted by hierarchical growth and clustering constraints. We, therefore, consider a cosmologically motivated model with high-resolution simulations, in which the initial galaxy forms in a gas rich merger and is observed at an appropriate age under representative conditions, then evolves undergoing a 'typical' level of dry merging and mass loss. We show that this case is consistent with all the observational constraints without tension with cosmological expectations. Effect (2), which builds up an extended, low-density envelope, dominates the evolution (giving factors ∼2-3 size evolution), but effects (1), (3), (4) and (possibly) (6) each contribute an additional ∼20 per cent size evolution (net factor of ∼2), together bringing the natural cosmological predictions into good agreement with the combination of observational constraints. We discuss implications for the evolution in correlations between BH and host bulge properties and show that this naturally predicts some evolution similar to that observed; better observations of BH masses could also constrain host galaxy merger histories. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0909.2039}, -author = {Hopkins, Philip F. and Bundy, Kevin and Hernquist, Lars and Wuyts, Stijn and Cox, Thomas J.}, -doi = {10.1111/j.1365-2966.2009.15699.x}, -eprint = {0909.2039}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Quasars: general}, -month = {jan}, -number = {2}, -pages = {1099--1117}, -title = {{Discriminating between the physical processes that drive spheroid size evolution}}, -volume = {401}, -year = {2010} -} -@article{Klypin2001, -abstract = {We study the effects of mass and force resolution on the density profiles of galaxy-size Cold Dark Matter (CDM) halos in a flat, low-density cosmological model with vacuum energy. We show thatalthough increasing the mass and force resolution allows us to probe deeper into the inner halo regions, it does not lead to steeper inner density profiles. Instead, the halo profiles converge at scales larger than four times the formal resolution or the radius containing more than 200 particles, whichever is larger. In the simulations presented in this paper, we are able to probe density profile of a relaxed isolated galaxy-size halo at scales r=(0.005-1)r_vir. We find that the density distribution can be well approximated by the profile suggested by Moore etal (1998): rho= x^{-1.5}(1+x^{1.5})^-1, where x=r/r_s and r_s is the characteristic radius. The analytical profile proposed by Navarro et al. (1996) rho= x^{-1}(1+x)^-2, also provides a good fit, with the same relative errors of about 10% for radii larger than 1% of the virial radius. Both analytical profiles fit equally well because for high-concentration galaxy-size halos the differences between these profiles become significant only at scales well below 0.01r_vir. We also find that halos of similar mass may have somewhat different parameters (characteristic radius, maximum rotation velocity, etc.) and shapes of their density profiles. We associate this scatter in properties with differences in halo merger histories and the amount of substructure present in the analyzed halos.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0006343}, -author = {Klypin, Anatoly and Kravtsov, Andrey V. and Bullock, James S. and Primack, Joel R.}, -doi = {10.1086/321400}, -eprint = {0006343}, -file = {:C\:/Users/Jammy/Documents/Papers/DarkMatterModels/Navarro1996StructureCDMHalos.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -number = {2}, -pages = {903--915}, -primaryClass = {astro-ph}, -title = {{Resolving the Structure of Cold Dark Matter Halos}}, -volume = {554}, -year = {2001} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular it demands highly efficient machine learning and image analysis algorithms. But scalability is not the only challenge: Astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. We argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. In the following, we will present this exciting application area for data scientists. We will focus on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Walcher2011, -abstract = {Fitting the spectral energy distributions (SEDs) of galaxies is an almost universally used technique that has matured significantly in the last decade. Model predictions and fitting procedures have improved significantly over this time, attempting to keep up with the vastly increased volume and quality of available data. We review here the field of SED fitting, describing the modelling of ultraviolet to infrared galaxy SEDs, the creation of multiwavelength data sets, and the methods used to fit model SEDs to observed galaxy data sets. We touch upon the achievements and challenges in the major ingredients of SED fitting, with a special emphasis on describing the interplay between the quality of the available data, the quality of the available models, and the best fitting technique to use in order to obtain a realistic measurement as well as realistic uncertainties. We conclude that SED fitting can be used effectively to derive a range of physical properties of galaxies, such as redshift, stellar masses, star formation rates, dust masses, and metallicities, with care taken not to over-interpret the available data. Yet there still exist many issues such as estimating the age of the oldest stars in a galaxy, finer details of dust properties and dust-star geometry, and the influences of poorly understood, luminous stellar types and phases. The challenge for the coming years will be to improve both the models and the observational data sets to resolve these uncertainties. The present review will be made available on an interactive, moderated web page (sedfitting. org), where the community can access and change the text. The intention is to expand the text and keep it up to date over the coming years. {\textcopyright} 2010 Springer Science+Business Media B.V.}, -archivePrefix = {arXiv}, -arxivId = {1008.0395}, -author = {Walcher, Jakob and Groves, Brent and Budav{\'{a}}ri, Tam{\'{a}}s and Dale, Daniel}, -doi = {10.1007/s10509-010-0458-z}, -eprint = {1008.0395}, -isbn = {0-7803-8416-4}, -issn = {1572946X}, -journal = {Astrophysics and Space Science}, -keywords = {Galaxies: ISM,Galaxies: stellar content,Methods: data analysis,Radiation mechanisms: general,Techniques: photometric,Techniques: spectroscopic}, -month = {jan}, -number = {1}, -pages = {1--51}, -pmid = {21278243}, -title = {{Fitting the integrated spectral energy distributions of galaxies}}, -volume = {331}, -year = {2011} -} -@article{Ackermann2011, -abstract = {Satellite galaxies of the Milky Way are among the most promising targets for dark matter searches in gamma rays. We present a search for dark matter consisting of weakly interacting massive particles, applying a joint likelihood analysis to 10 satellite galaxies with 24 months of data of the Fermi Large Area Telescope. No dark matter signal is detected. Including the uncertainty in the dark matter distribution, robust upper limits are placed on dark matter annihilation cross sections. The 95% confidence level upper limits range from about 10-26cmm3s-1 at 5 GeV to about 5×10-23cm3s-1 at 1 TeV, depending on the dark matter annihilation final state. For the first time, using gamma rays, we are able to rule out models with the most generic cross section (∼3×10-26cm3s-1 for a purely s-wave cross section), without assuming additional boost factors. {\textcopyright} 2011 American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {1108.3546}, -author = {Ackermann, M. and Ajello, M. and Albert, A. and Atwood, W. B. and Baldini, L. and Ballet, J. and Barbiellini, G. and Bastieri, D. and Bechtol, K. and Bellazzini, R. and Berenji, B. and Blandford, R. D. and Bloom, E. D. and Bonamente, E. and Borgland, A. W. and Bregeon, J. and Brigida, M. and Bruel, P. and Buehler, R. and Burnett, T. H. and Buson, S. and Caliandro, G. A. and Cameron, R. A. and Ca{\~{n}}adas, B. and Caraveo, P. A. and Casandjian, J. M. and Cecchi, C. and Charles, E. and Chekhtman, A. and Chiang, J. and Ciprini, S. and Claus, R. and Cohen-Tanugi, J. and Conrad, J. and Cutini, S. and {De Angelis}, A. and {De Palma}, F. and Dermer, C. D. and Digel, S. W. and {Do Couto E Silva}, E. and Drell, P. S. and Drlica-Wagner, A. and Falletti, L. and Favuzzi, C. and Fegan, S. J. and Ferrara, E. C. and Fukazawa, Y. and Funk, S. and Fusco, P. and Gargano, F. and Gasparrini, D. and Gehrels, N. and Germani, S. and Giglietto, N. and Giordano, F. and Giroletti, M. and Glanzman, T. and Godfrey, G. and Grenier, I. A. and Guiriec, S. and Gustafsson, M. and Hadasch, D. and Hayashida, M. and Hays, E. and Hughes, R. E. and Jeltema, T. E. and J{\'{o}}hannesson, G. and Johnson, R. P. and Johnson, A. S. and Kamae, T. and Katagiri, H. and Kataoka, J. and Kn{\"{o}}dlseder, J. and Kuss, M. and Lande, J. and Latronico, L. and Lionetto, A. M. and {Llena Garde}, M. and Longo, F. and Loparco, F. and Lott, B. and Lovellette, M. N. and Lubrano, P. and Madejski, G. M. and Mazziotta, M. N. and McEnery, J. E. and Mehault, J. and Michelson, P. F. and Mitthumsiri, W. and Mizuno, T. and Monte, C. and Monzani, M. E. and Morselli, A. and Moskalenko, I. V. and Murgia, S. and Naumann-Godo, M. and Norris, J. P. and Nuss, E. and Ohsugi, T. and Okumura, A. and Omodei, N. and Orlando, E. and Ormes, J. F. and Ozaki, M. and Paneque, D. and Parent, D. and Pesce-Rollins, M. and Pierbattista, M. and Piron, F. and Pivato, G. and Porter, T. A. and Profumo, S. and Rain{\`{o}}, S. and Razzano, M. and Reimer, A. and Reimer, O. and Ritz, S. and Roth, M. and Sadrozinski, H. F.W. and Sbarra, C. and Scargle, J. D. and Schalk, T. L. and Sgr{\`{o}}, C. and Siskind, E. J. and Spandre, G. and Spinelli, P. and Strigari, L. and Suson, D. J. and Tajima, H. and Takahashi, H. and Tanaka, T. and Thayer, J. G. and Thayer, J. B. and Thompson, D. J. and Tibaldo, L. and Tinivella, M. and Torres, D. F. and Troja, E. and Uchiyama, Y. and Vandenbroucke, J. and Vasileiou, V. and Vianello, G. and Vitale, V. and Waite, A. P. and Wang, P. and Winer, B. L. and Wood, K. S. and Wood, M. and Yang, Z. and Zimmer, S. and Kaplinghat, M. and Martinez, G. D.}, -doi = {10.1103/PhysRevLett.107.241302}, -eprint = {1108.3546}, -isbn = {1079-7114 (Electronic)\r0031-9007 (Linking)}, -issn = {10797114}, -journal = {Physical Review Letters}, -number = {24}, -pages = {1--6}, -pmid = {22242987}, -title = {{Constraining dark matter models from a combined analysis of Milky Way satellites with the Fermi Large Area Telescope}}, -volume = {107}, -year = {2011} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless} $\sigma$∗ {\textless} 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Shi2015, -abstract = {We study how halo intrinsic dynamical properties are linked to their formation processes for halos in two mass ranges, 1012-1012.5 h-1M⊙ and ≥1013 h-1M⊙, and how both are correlated with the large-scale tidal field within which the halos reside at present. We identify infall halos that are about to merge with their hosts. We find that the tangential infall velocity increases significantly with the strength of the tidal field, but no strong correlation is found for the radial component. These results can be used to explain the environmental dependence of internal velocity anisotropy and spin of halos. The position vectors and velocities of infall halos are aligned with the principal axes of the tidal field, and the alignment depends on the strength of the tidal field. Opposite accretion patterns are found in weak and strong tidal fields, showing that in a weak field the accretion flow is dominated by radial motion within the local structure, while a large tangential component is present in a strong field. These findings can be used to understand the strong alignments we find between the principal axes of the internal velocity ellipsoids of halos and the tidal field, and their dependence on the strength of the tidal field. We further find that only in weak tidal fields does the spin-tidal field alignment follow the prediction of the tidal torque theory. We discuss how our results may be used to understand the spins of disk galaxies and velocity structures of elliptical galaxies and their correlations with large-scale structure.}, -archivePrefix = {arXiv}, -arxivId = {1501.07764}, -author = {Shi, Jingjing and Wang, Huiyuan and Mo, H J}, -doi = {10.1088/0004-637X/807/1/37}, -eprint = {1501.07764}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: halos,large-scale structure of universe,methods: statistical}, -number = {1}, -title = {{Flow Patterns Around Dark Matter Halos: the Link Between Halo Dynamical Properties and Large-Scale Tidal Field}}, -volume = {807}, -year = {2015} -} -@article{Lanusse2017a, -abstract = {Galaxy-scale strong gravitational lensing can not only provide a valuable probe of the dark matter distribution of massive galaxies, but also provide valuable cosmological constraints, either by studying the population of strong lenses or by measuring time delays in lensed quasars. Due to the rarity of galaxy-scale strongly lensed systems, fast and reliable automated lens finding methods will be essential in the era of large surveys such as Large Synoptic Survey Telescope, Euclid and Wide-Field Infrared Survey Telescope. To tackle this challenge, we introduce CMU DeepLens, a new fully automated galaxy-galaxy lens finding method based on deep learning. This supervised machine learning approach does not require any tuning after the training step which only requires realistic image simulations of strongly lensed systems. We train and validate our model on a set of 20 000 LSST-like mock observations including a range of lensed systems of various sizes and signal-to-noise ratios (S/N).We find on our simulated data set that for a rejection rate of non-lenses of 99 per cent, a completeness of 90 per cent can be achieved for lenses with Einstein radii larger than 1.4 arcsec and S/N larger than 20 on individual g-band LSST exposures. Finally, we emphasize the importance of realistically complex simulations for training such machine learning methods by demonstrating that the performance of models of significantly different complexities cannot be distinguished on simpler simulations.}, -archivePrefix = {arXiv}, -arxivId = {1703.02642}, -author = {Lanusse, Fran{\c{c}}ois and Ma, Quanbin and Li, Nan and Collett, Thomas E and Li, Chun Liang and Ravanbakhsh, Siamak and Mandelbaum, Rachel and P{\'{o}}czos, Barnab{\'{a}}s}, -doi = {10.1093/mnras/stx1665}, -eprint = {1703.02642}, -isbn = {0021-9258 (Print){\$}\backslash{\$}r0021-9258 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: statistical,gravitational lensing: strong}, -number = {3}, -pages = {3895--3906}, -pmid = {10913147}, -title = {{CMU DeepLens: Deep learning for automatic image-based galaxy-galaxy strong lens finding}}, -url = {http://arxiv.org/abs/1703.02642}, -volume = {473}, -year = {2018} -} -@article{Messias2019, -abstract = {Follow-up observations of (sub-)mm-selected gravitationally lensed systems have allowed a more detailed study of the dust-enshrouded phase of star formation up to very early cosmic times. Here, the case of the gravitationally lensed merger in HATLAS J142935.3-002836 (also known as H1429-0028; zlens = 0.218, zbkg = 1.027) is revisited following recent developments in the literature and new Atacama Pathfinder EXperiment (APEX) observations targeting two carbon monoxide (CO) rotational transitions Jup = 3 and 6. We show that the line profiles comprise three distinct velocity components, where the fainter high velocity one is less magnified and more compact. The modelling of the observed spectral line energy distribution of CO Jup = 2-6 and [C I] 3P1-3P0 assumes a large velocity gradient scenario, where the analysis is based on four statistical approaches. Since the detected gas and dust emission comes exclusively from only one of the two merging components (the one oriented north-south, NS), we are only able to determine upper limits for the companion. The molecular gas in the NS component in H1429-0028 is found to have a temperature of ∼70 K, a volume density of log (n[cm-3]) ∼ 3.7, to be expanding at ∼10 km s-1 pc-1, and amounts to MH2 = 4+3 -2 × 109M$\theta$. The CO to H2 conversion factor is estimated to be $\alpha$CO = 0.4+0.3 -0.2 M$\theta$/(K km s-1 pc2). The NS galaxy is expected to have a factor of ≳10× more gas than its companion (MH2 ≲ 3 × 108 M$\theta$). Nevertheless, the total amount of molecular gas in the system comprises only up to 15 per cent (1$\sigma$ upper limit) of the total (dynamical) mass.}, -archivePrefix = {arXiv}, -arxivId = {1904.00307}, -author = {Messias, Hugo and Nagar, Neil and Zhang, Zhi Yu and Oteo, Iv{\'{a}}n and Dye, Simon and Ibar, Eduardo and Timmons, Nicholas and {Van Der Werf}, Paul and Riechers, Dominik and Eales, Stephen and Ivison, Rob and Maresca, Jacob and Micha{\l}owski, Micha{\l} J. and Yang, Chentao}, -doi = {10.1093/mnras/stz945}, -eprint = {1904.00307}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Messias et al. - 2019 - The molecular gas properties in the gravitationally lensed merger HATLAS J142935.3-002836.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {ISM: abundances,galaxies: interactions,gravitational lensing: strong,submillimetre: ISM.,submillimetre: galaxies}, -number = {2}, -pages = {2366--2378}, -title = {{The molecular gas properties in the gravitationally lensed merger HATLAS J142935.3-002836}}, -url = {http://arxiv.org/abs/1904.00307%0Ahttp://dx.doi.org/10.1093/mnras/stz945}, -volume = {486}, -year = {2019} -} -@article{Wood2014, -abstract = {? 2014 IOP Publishing Ltd and Sissa Medialab srl.The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D and Hall, D J and Murray, N J and Gow, J P D and Holland, A and Turner, P and Burt, D}, -doi = {10.1088/1748-0221/9/12/C12028}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv,visible and ir photons (s}, -number = {12}, -pages = {C12028----C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{VanDeVoort2011, -abstract = {We study the rate at which gas accretes on to galaxies and haloes and investigate whether the accreted gas was shocked to high temperatures before reaching a galaxy. For this purpose, we use a suite of large cosmological, hydrodynamical simulations from the OverWhelmingly Large Simulations project, which uses a modified version of the smoothed particle hydrodynamics code gadget-3. We improve on previous work by considering a wider range of halo masses and redshifts, by distinguishing between accretion on to haloes and accretion on to galaxies, by including important feedback processes and by comparing simulations with different physics. Gas accretion is mostly smooth, with mergers only becoming important for groups and clusters. The specific rate of the gas accretion on to haloes is, like that for dark matter, only weakly dependent on the halo mass. For halo masses Mhalo≫ 1011M⊙, it is relatively insensitive to feedback processes. In contrast, accretion rates on to galaxies are determined by radiative cooling and by outflows driven by supernovae and active galactic nuclei. Galactic winds increase the halo mass at which the central galaxies grow the fastest by about two orders of magnitude to Mhalo$\sim$ 1012M⊙. Gas accretion is bimodal, with maximum past temperatures either of the order of the virial temperature or ≲105K. The fraction of the gas accreted on to haloes in the hot mode is insensitive to feedback and metal-line cooling. It increases with decreasing redshift, but is mostly determined by the halo mass, increasing gradually from less than 10 per cent for $\sim$1011M⊙ to greater than 90 per cent at $\sim$1013M⊙. In contrast, for accretion on to galaxies, the cold mode is always significant and the relative contributions of the two accretion modes are more sensitive to feedback and metal-line cooling. On average, the majority of stars present in any mass halo at any redshift were formed from the gas accreted in the cold mode, although the hot mode contributes typically over 10 per cent for Mhalo≳ 1011M⊙. Thus, while gas accretion on to haloes can be robustly predicted, the rate of accretion on to galaxies is sensitive to uncertain feedback processes. Nevertheless, it is clear that galaxies, but not necessarily their gaseous haloes, are predominantly fed by the gas that did not experience an accretion shock when it entered the host halo. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1011.2491}, -author = {van de Voort, Freeke and Schaye, Joop and Booth, C. M. and Haas, Marcel R. and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2011.18565.x}, -eprint = {1011.2491}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Intergalactic medium}, -month = {jul}, -number = {3}, -pages = {2458--2478}, -title = {{The rates and modes of gas accretion on to galaxies and their gaseous haloes}}, -volume = {414}, -year = {2011} -} -@book{Sersic1968, -abstract = {Not Available}, -author = {Sersic, J L}, -booktitle = {Cordoba}, -keywords = {GALAXIES,GROUPS OF GALAXIES,atlases}, -title = {{Atlas de galaxias australes}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1968adga.book.....S&link_type=CITATIONS%5Cnpapers://dcc533b5-8613-47b7-b88c-2b0c0d39c33f/Paper/p10728}, -year = {1968} -} -@article{Wong2016, -abstract = {Strong gravitational lenses with measured time delays between the multiple images allow a direct measurement of the time-delay distance to the lens, and thus a measure of cosmological parameters, particularly the Hubble constant, H0. We present a blind lens model analysis of the quadruply imaged quasar lens HE 0435-1223 using deep Hubble Space Telescope imaging, updated time-delay measurements from the COSmological MOnitoring of GRAvItational Lenses (COSMOGRAIL), a measurement of the velocity dispersion of the lens galaxy based on Keck data, and a characterization of the mass distribution along the line of sight. HE 0435-1223 is the third lens analysed as a part of the H0 Lenses in COSMOGRAIL's Wellspring (H0LiCOW) project. We account for various sources of systematic uncertainty, including the detailed treatment of nearby perturbers, the parametrization of the galaxy light and mass profile, and the regions used for lens modelling. We constrain the effective timedelay distance to be D$\Delta$t = 2612+208-191 Mpc, a precision of 7.6 per cent. From HE 0435-1223 alone, we infer a Hubble constant of H0 = 73.1+5.7-6.0 km s-1 Mpc-1 assuming a flat $\Lambda$CDM cosmology. The cosmographic inference based on the three lenses analysed by H0LiCOW to date is presented in a companion paper (H0LiCOW Paper V).}, -archivePrefix = {arXiv}, -arxivId = {1607.01403}, -author = {Wong, Kenneth C. and Suyu, Sherry H. and Auger, Matthew W. and Bonvin, Vivien and Courbin, Frederic and Fassnacht, Christopher D. and Halkola, Aleksi and Rusu, Cristian E. and Sluse, Dominique and Sonnenfeld, Alessandro and Treu, Tommaso and Collett, Thomas E. and Hilbert, Stefan and Koopmans, Leon V.E. and Marshall, Philip J. and Rumbaugh, Nicholas}, -doi = {10.1093/mnras/stw3077}, -eprint = {1607.01403}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Distance scale,Gravitational lensing: strong}, -number = {4}, -pages = {4895--4913}, -title = {{H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology}}, -volume = {465}, -year = {2017} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2013} -} -@article{Chirivi2017, -abstract = {Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we present the first attempt at modelling line-of-sight mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We focus on the Hubble Frontier Field cluster MACS J0416.1-2403, and our multi-plane model reproduces the observed image positions with a rms offset of {\$\sim${}}0.53". Starting from this best-fitting model, we simulate a mock cluster that resembles MACS J0416.1-2403 in order to explore the effects of line-of-sight structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms {\$\sim${}}0.3"); accounting for line-of-sight galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factors of the lensed multiple images are recovered within {\$\sim${}}10{\%} for {\$\sim${}}95{\%} of them, those {\$\sim${}}5{\%} that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models (up to a factor of {\$\sim${}}200). In addition, line-of-sight galaxies cannot explain the apparent discrepancy in the properties of massive subhalos between MACS J0416.1-2403 and N-body simulated clusters. Since our model of MACS J0416.1-2403 with line-of-sight galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities, such as more flexible halo shapes, would be needed in future models of MACS J0416.1-2403.}, -archivePrefix = {arXiv}, -arxivId = {1706.07815}, -author = {Chiriv{\`{i}}, G and Suyu, S H and Grillo, C and Halkola, A and Balestra, I and Caminha, G B and Mercurio, A and Rosati, P}, -doi = {10.1051/0004-6361/201731433}, -eprint = {1706.07815}, -issn = {14320746}, -keywords = {1,2403,cluster galaxies,dark matter,general,gravitational lensing,individual,macs j0416,strong}, -pages = {1--29}, -title = {{MACS J0416.1-2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters}}, -url = {http://arxiv.org/abs/1706.07815}, -year = {2017} -} -@article{Lipnicky2018, -abstract = {We report HI observations of eight spiral galaxies that are strongly lensing background sources. Our targets were selected from the Sloan WFC (Wide Field Camera) Edge-on Late-type Lens Survey (SWELLS) using the Arecibo, Karl G. Jansky Very Large Array, and Green Bank telescopes. We securely detect J1703+2451 at z=0.063 with a signal-to-noise of 6.7 and W50=79+/-13 km/s, obtaining the first detection of HI emission in a strong spiral lens. We measure a mass of M(HI)= 1.77+/-0.06(+0.35/-0.75) x 10{\^{}}9 M{\_}(sol) for this source. We find that this lens is a normal spiral, with observable properties that are fairly typical of spiral galaxies. For three other sources we did not secure a detection; however, we are able to place strong constraints on the HI masses of those galaxies. The observations for four of our sources were rendered unusable due to strong radio frequency interference.}, -archivePrefix = {arXiv}, -arxivId = {1802.01588}, -author = {Lipnicky, Andrew and Chakrabarti, Sukanya and Wright, Melvyn C H and Blitz, Leo and Heiles, Carl and Cotton, William and Frayer, David and Blandford, Roger and Shu, Yiping and Bolton, Adam S}, -doi = {10.1093/mnras/sty326}, -eprint = {1802.01588}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Radio lines: galaxies}, -number = {3}, -pages = {3097--3105}, -title = {{The first detection of neutral hydrogen in emission in a strong spiral lens}}, -url = {http://arxiv.org/abs/1802.01588%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty326}, -volume = {476}, -year = {2018} -} -@article{Eisenstein2001, -abstract = {We describe the target selection and resulting properties of a spectroscopic sample of luminous, red galaxies (LRG) from the imaging data of the Sloan Digital Sky Survey (SDSS). These galaxies are selected on the basis of color and magnitude to yield a sample of luminous, intrinsically red galaxies that extends fainter and further than the main flux-limited portion of the SDSS galaxy spectroscopic sample. The sample is designed to impose a passively-evolving luminosity and rest-frame color cut to a redshift of 0.38. Additional, yet more luminous, red galaxies are included to a redshift of 0.5. Approximately 12 of these galaxies per square degree are targeted for spectroscopy, so the sample will number over 100,000 with the full survey. SDSS commissioning data indicate that the algorithm efficiently selects luminous (M{\_}g=-21.4), red galaxies, that the spectroscopic success rate is very high, and that the resulting set of galaxies is approximately volume-limited out to z=0.38. When the SDSS is complete, the LRG spectroscopic sample will fill over 1h{\^{}}-3 Gpc{\^{}}3 with an approximately homogeneous population of galaxies and will therefore be well suited to studies of large-scale structure and clusters out to z=0.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108153}, -author = {Eisenstein, D J and Annis, J and Gunn, J E and Szalay, A S and Connolly, A J and Nichol, R C and Bahcall, N A and Bernardi, M and Burles, S and Castander, F J and Fukugita, M and Hogg, D W and Ivezic, Z and Knapp, G R and Lupton, R H and Narayanan, V and Postman, M and Riechart, D E and Richmond, M and Schneider, D P and Schlegel, D J and Strauss, M A and SubbaRao, M and Tucker, D L and Berk, D Vanden and Vogeley, M S and Weinberg, D H and Yanny, B}, -doi = {10.1086/323717}, -eprint = {0108153}, -isbn = {0004-6256}, -issn = {00046256}, -pages = {1--30}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample}}, -url = {http://arxiv.org/abs/astro-ph/0108153%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/323717}, -year = {2001} -} -@article{Shockley1952, -abstract = {The statistics of the recombination of holes and electrons in semiconductors is analyzed on the basis of a model in which the recombination occurs through the mechanism of trapping. A trap is assumed to have an energy level in the energy gap so that its charge may have either of two values differing by one electronic charge. The dependence of lifetime of injected carriers upon initial conductivity and upon injected carrier density is discussed. {\textcopyright}1952 The American Physical Society.}, -author = {Shockley, W and Read, W T}, -doi = {10.1103/PhysRev.87.835}, -issn = {0031899X}, -journal = {Physical Review}, -keywords = {Shockley1952}, -mendeley-tags = {Shockley1952}, -number = {5}, -pages = {835--842}, -title = {{Statistics of the recombinations of holes and electrons}}, -volume = {87}, -year = {1952} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo {\textgreater} 1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from {\$\sim${}}30° to 10° for M {\$\sim${}} 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles. {\textcopyright}2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@article{Governato2010, -abstract = {For almost two decades the properties of 'dwarf' galaxies have challenged the cold dark matter (CDM) model of galaxy formation. Most observed dwarf galaxies consist of a rotating stellar disk embedded in a massive dark-matter halo with a near-constant-density core. Models based on the dominance of CDM, however, invariably form galaxies with dense spheroidal stellar bulges and steep central dark-matter profiles, because low-angular-momentum baryons and dark matter sink to the centres of galaxies through accretion and repeated mergers. Processes that decrease the central density of CDM halos have been identified, but have not yet reconciled theory with observations of present-day dwarfs. This failure is potentially catastrophic for the CDM model, possibly requiring a different dark-matter particle candidate. Here we report hydrodynamical simulations (in a framework assuming the presence of CDM and a cosmological constant) in which the inhomogeneous interstellar medium is resolved. Strong outflows from supernovae remove low-angular-momentum gas, which inhibits the formation of bulges and decreases the dark-matter density to less than half of what it would otherwise be within the central kiloparsec. The analogues of dwarf galaxies-bulgeless and with shallow central dark-matter profiles-arise naturally in these simulations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/0911.2237}, -author = {Governato, F and Brook, C and Mayer, L and Brooks, A and Rhee, G and Wadsley, J and Jonsson, P and Willman, B and Stinson, G and Quinn, T and Madau, P}, -doi = {10.1038/nature08640}, -eprint = {0911.2237}, -isbn = {0028-0836}, -issn = {0028-0836}, -journal = {\Nat}, -number = {7278}, -pages = {203--206}, -pmid = {20075915}, -primaryClass = {astro-ph.CO}, -title = {{Bulgeless dwarf galaxies and dark matter cores from supernova-driven outflows}}, -volume = {463}, -year = {2010} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z ∼ 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u - g color profiles for these galaxies and show that most z ∼ 2galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z ∼ 2galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: ($\Delta$(u - g rest)/$\Delta$(log r))median = -0.47, -0.33, and -0.46 for z ∼ 2, z ∼ 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z ∼ 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u - g colors, and lower S{\'{e}}rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch. {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J. and {Van Dokkum}, Pieter G. and Labb{\'{e}}, Ivo and Illingworth, Garth D. and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Szomoru et al. - 2011 - Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging The hubbl.pdf:pdf}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Gomer2018, -abstract = {The positions of multiple images in galaxy lenses are related to the galaxy mass distribution. Smooth elliptical mass profiles were previously shown to be inadequate in reproducing the quad population. In this paper, we explore the deviations from such smooth elliptical mass distributions. Unlike most other work, we use a model-free approach based on the relative polar image angles of quads, and their position in 3D space with respect to the Fundamental Surface of Quads. The FSQ is defined by quads produced by elliptical lenses. We have generated thousands of quads from synthetic populations of lenses with substructure consistent with {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM simulations, and found that such perturbations are not sufficient to match the observed distribution of quads relative to the FSQ. The result is unchanged even when subhalo masses are increased by a factor of ten, and the most optimistic lensing selection bias is applied. We then produce quads from galaxies created using two components, representing baryons and dark matter. The transition from the mass being dominated by baryons in inner radii to being dominated by dark matter in outer radii can carry with it asymmetries, which would affect relative image angles. We run preliminary experiments using lenses with two elliptical mass components with nonidentical axis ratios and position angles, perturbations from ellipticity in the form of nonzero Fourier coefficients {\$}a{\_}4{\$} and {\$}a{\_}6{\$}, and artificially offset ellipse centers as a proxy for asymmetry at image radii. We show that combination of these effects is a promising way of accounting for quad population properties. We conclude that the quad population provides a unique and sensitive tool for constraining detailed mass distribution in the centers of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1712.07665}, -author = {Gomer, Matthew R and Williams, Liliya L R}, -doi = {10.1093/mnras/stx3294}, -eprint = {1712.07665}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1987--2002}, -title = {{The impact of {\$}\Lambda{\$}CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses}}, -volume = {475}, -year = {2018} -} -@article{Rana2017, -abstract = {The construction of the cosmic distance-duality relation (CDDR) has been widely studied. However, its consistency with various new observables remains a topic of interest. We present a new way to constrain the CDDR $\eta$(z) using different dynamic and geometric properties of strong gravitational lenses (SGL) along with SNe Ia observations. We use a sample of 102 SGL with the measurement of corresponding velocity dispersion $\sigma$0 and Einstein radius $\theta$E. In addition, we also use a dataset of 12 two image lensing systems containing the measure of time delay $\Delta$ t between source images. Jointly these two datasets give us the angular diameter distance DAol of the lens. Further, for luminosity distance, we use the 740 observations from JLA compilation of SNe Ia. To study the combined behavior of these datasets we use a model independent method, Gaussian Process (GP). We also check the efficiency of GP by applying it on simulated datasets, which are generated in a phenomenological way by using realistic cosmological error bars. Finally, we conclude that the combined bounds from the SGL and SNe Ia observation do not favor any deviation of CDDR and are in concordance with the standard value ($\eta$=1) within 2$\sigma$ confidence region, which further strengthens the theoretical acceptance of CDDR.}, -archivePrefix = {arXiv}, -arxivId = {1705.04549}, -author = {Rana, Akshay and Jain, Deepak and Mahajan, Shobhit and Mukherjee, Amitabha and Holanda, R. F.L.}, -doi = {10.1088/1475-7516/2017/07/010}, -eprint = {1705.04549}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rana et al. - 2017 - Probing the cosmic distance duality relation using time delay lenses(2).pdf:pdf}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,dark energy theory,gravitational lensing,supernova type Ia - standard candles}, -number = {7}, -title = {{Probing the cosmic distance duality relation using time delay lenses}}, -volume = {2017}, -year = {2017} -} -@article{Gadotti2011, -abstract = {I present results from the modelling of stellar bars in nearly 300 barred galaxies in the local universe through parametric multicomponent multiband image fitting. The surface brightness radial profile of bars is described using a S{\'{e}}rsic function and parameters, such as the bar effective radius, ellipticity, boxiness, length and mass, and bar-to-total luminosity and mass ratios, are determined, which is unprecedented for a sample of this size. The properties of bars in galaxies with classical bulges and pseudo-bulges are compared. For a fixed bar-to-total mass ratio, pseudo-bulges are on average significantly less massive than classical bulges, indicating that, if pseudo-bulges are formed through bars, further processes are necessary to build a classical bulge. I find a correlation between bar ellipticity and boxiness, and define a new parameter as the product of these two quantities. I also find correlations between this product and the normalized bar size, between the sizes of bars and bulges, and between the normalized bar size and bulge-to-total ratio. Bars with different ellipticities follow parallel lines in the latter two correlations. These correlations can arise if, starting off with different normalized sizes and ellipticities, bars grow longer and stronger with dynamical age, as a result of angular momentum exchange between the inner and outer parts of galaxies, consistent with previous theoretical predictions. A plausible consequence is that bar pattern speeds should become lower with bar dynamical age and towards galaxies with more prominent bulges. {\textcopyright} 2011 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1003.1719}, -author = {Gadotti, Dimitri A.}, -doi = {10.1111/j.1365-2966.2011.18945.x}, -eprint = {1003.1719}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gadotti - 2011 - Secular evolution and structural properties of stellar bars in galaxies(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {3308--3318}, -title = {{Secular evolution and structural properties of stellar bars in galaxies}}, -volume = {415}, -year = {2011} -} -@article{Brehmer2019, -abstract = {The subtle and unique imprint of dark matter substructure on extended arcs in strong lensing systems contains a wealth of information about the properties and distribution of dark matter on small scales and, consequently, about the underlying particle physics. However, teasing out this effect poses a significant challenge since the likelihood function for realistic simulations of population-level parameters is intractable. We apply recently-developed simulation-based inference techniques to the problem of substructure inference in galaxy-galaxy strong lenses. By leveraging additional information extracted from the simulator, neural networks are efficiently trained to estimate likelihood ratios associated with population-level parameters characterizing substructure. Through proof-of-principle application to simulated data, we show that these methods can provide an efficient and principled way to simultaneously analyze an ensemble of strong lenses, and can be used to mine the large sample of lensing images deliverable by near-future surveys for signatures of dark matter substructure.}, -archivePrefix = {arXiv}, -arxivId = {1909.02005}, -author = {Brehmer, Johann and Mishra-Sharma, Siddharth and Hermans, Joeri and Louppe, Gilles and Cranmer, Kyle}, -doi = {10.3847/1538-4357/ab4c41}, -eprint = {1909.02005}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brehmer et al. - 2019 - Mining for Dark Matter Substructure Inferring Subhalo Population Properties from Strong Lenses with Machine Lear.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {1643,1886,1903,343,353,670,astrostatistics techniques,cosmology,dark matter,gravitational,lensing,nonparametric inference,strong gravitational lensing}, -number = {1}, -pages = {49}, -title = {{Mining for Dark Matter Substructure: Inferring Subhalo Population Properties from Strong Lenses with Machine Learning}}, -volume = {886}, -year = {2019} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10^12.5 h^-1 M_sun < M_200b < 10^15 h^-1 M_sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that $\sim$ 70% of galaxies with stellar mass M_* > 10^11 h^-2 M_sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The $\sim$ 30% of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20\% level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J. E. and Leauthaud, A. and Emsellem, E. and Ge, J. and Arag{\'{o}}n-Salamanca, A. and Greco, J. and Lin, Y.-T. and Mao, S. and Masters, K. and Merrifield, M. and More, S. and Okabe, N. and Schneider, D. P. and Thomas, D. and Wake, D. A. and Pan, K. and Bizyaev, D. and Oravetz, D. and Simmons, A. and Yan, R. and van den Bosch, F.}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2018 - SDSS-IV MaNGA Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Xia2017, -abstract = {In this paper we use high-resolution cosmological simulations to study halo intrinsic alignment and its dependence on mass, formation time and large-scale environment. In agreement with previous studies using N-body simulations, it is found that massive halos have stronger alignment. For given mass, older halos have stronger alignment than younger ones. By identifying the cosmic environment of halo using Hessian matrix, we find that for given mass, halos in cluster regions also have stronger alignment than those in filament. The existing theory has not addressed these dependencies explicitly. In this work we extend the linear alignment model with inclusion of halo bias and find that the halo alignment with its mass and formation time dependence can be explained by halo bias. However, the model can not account for the environment dependence, as it is found that halo bias is lower in cluster and higher in filament. Our results suggest that halo bias and environment are independent factors in determining halo alignment. We also study the halo alignment correlation function and find that halos are strongly clustered along their major axes and less clustered along the minor axes. The correlated halo alignment can extend to scale as large as $100h^{-1}$Mpc where its feature is mainly driven by the baryon acoustic oscillation effect.}, -archivePrefix = {arXiv}, -arxivId = {1706.07814}, -author = {Xia, Qianli and Kang, Xi and Wang, Peng and Luo, Yu and Yang, Xiaohu and Jing, Yipeng and Wang, Huiyuan and Mo, Houjun}, -doi = {10.3847/1538-4357/aa8d17}, -eprint = {1706.07814}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xia et al. - 2017 - Halo Intrinsic Alignment Dependence on Mass, Formation Time, and Environment.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {22}, -title = {{Halo Intrinsic Alignment: Dependence on Mass, Formation Time, and Environment}}, -url = {http://arxiv.org/abs/1706.07814%0Ahttp://dx.doi.org/10.3847/1538-4357/aa8d17}, -volume = {848}, -year = {2017} -} -@article{Geometryek, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Atek2015, -abstract = {Exploiting the power of gravitational lensing, the Hubble Frontier Fields (HFF) program aims at observing six massive galaxy clusters to explore the distant universe far beyond the limits of blank field surveys. Using the complete Hubble Space Telescope observations of the first HFF cluster A2744, we report the detection of 50 galaxy candidates at z ∼ 7 and eight candidates at z ∼ 8 in a total survey area of 0.96 arcmin2 in the source plane. Three of these galaxies are multiply imaged by the lensing cluster. Using an updated model of the mass distribution in the cluster we were able to calculate the magnification factor and the effective survey volume for each galaxy in order to compute the ultraviolet galaxy luminosity function (LF) at both redshifts 7 and 8. Our new measurements reliably extend the z ∼ 7 UV LF down to an absolute magnitude of MUV ∼ -15.5. We find a characteristic magnitude of M∗UV = -20.90-0.73+0.90 mag and a faint-end slope $\alpha$ = -2.01-0.28+0.20,close to previous determinations in blank fields. We show here for the first time that this slope remains steep down to very faint luminosities of 0.01 L∗. Although prone to large uncertainties, our results at z ∼ 8 also seem to confirm a steep faint-end slope below 0.1 L∗. The HFF program is therefore providing an extremely efficient way to study the faintest galaxy populations at z > 7 that would otherwise be inaccessible with current instrumentation. The full sample of six galaxy clusters will provide even better constraints on the buildup of galaxies at early epochs and their contribution to cosmic reionization.}, -archivePrefix = {arXiv}, -arxivId = {1409.0512}, -author = {Atek, Hakim and Richard, Johan and Kneib, Jean Paul and Jauzac, Mathilde and Schaerer, Daniel and Clement, Benjamin and Limousin, Marceau and Jullo, Eric and Natarajan, Priyamvada and Egami, Eiichi and Ebeling, Harald}, -doi = {10.1088/0004-637X/800/1/18}, -eprint = {1409.0512}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Atek et al. - 2015 - New constraints on the faint end of the UV luminosity function at z ∼ 7-8 using the gravitational lensing of the hu.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: luminosity function, mass function,Gravitational lensing: strong}, -number = {1}, -title = {{New constraints on the faint end of the UV luminosity function at z ∼ 7-8 using the gravitational lensing of the hubble frontier fields cluster A2744}}, -volume = {800}, -year = {2015} -} -@article{Chirivi2017, -abstract = {Exploiting the powerful tool of strong gravitational lensing by galaxy clusters to study the highest-redshift Universe and cluster mass distributions relies on precise lens mass modelling. In this work, we present the first attempt at modelling line-of-sight mass distribution in addition to that of the cluster, extending previous modelling techniques that assume mass distributions to be on a single lens plane. We focus on the Hubble Frontier Field cluster MACS J0416.1-2403, and our multi-plane model reproduces the observed image positions with a rms offset of {\$\sim${}}0.53". Starting from this best-fitting model, we simulate a mock cluster that resembles MACS J0416.1-2403 in order to explore the effects of line-of-sight structures on cluster mass modelling. By systematically analysing the mock cluster under different model assumptions, we find that neglecting the lensing environment has a significant impact on the reconstruction of image positions (rms {\$\sim${}}0.3"); accounting for line-of-sight galaxies as if they were at the cluster redshift can partially reduce this offset. Moreover, foreground galaxies are more important to include into the model than the background ones. While the magnification factors of the lensed multiple images are recovered within {\$\sim${}}10{\%} for {\$\sim${}}95{\%} of them, those {\$\sim${}}5{\%} that lie near critical curves can be significantly affected by the exclusion of the lensing environment in the models (up to a factor of {\$\sim${}}200). In addition, line-of-sight galaxies cannot explain the apparent discrepancy in the properties of massive subhalos between MACS J0416.1-2403 and N-body simulated clusters. Since our model of MACS J0416.1-2403 with line-of-sight galaxies only reduced modestly the rms offset in the image positions, we conclude that additional complexities, such as more flexible halo shapes, would be needed in future models of MACS J0416.1-2403.}, -archivePrefix = {arXiv}, -arxivId = {1706.07815}, -author = {Chiriv{\`{i}}, G and Suyu, S H and Grillo, C and Halkola, A and Balestra, I and Caminha, G B and Mercurio, A and Rosati, P}, -doi = {10.1051/0004-6361/201731433}, -eprint = {1706.07815}, -issn = {14320746}, -keywords = {1,2403,cluster galaxies,dark matter,general,gravitational lensing,individual,macs j0416,strong}, -pages = {1--29}, -title = {{MACS J0416.1-2403: Impact of line-of-sight structures on strong gravitational lensing modelling of galaxy clusters}}, -url = {http://arxiv.org/abs/1706.07815%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201731433}, -year = {2017} -} -@article{Report2011, -abstract = {Euclid is a space-based survey mission from the European Space Agency designed to understand the origin of the Universe's accelerating expansion. It will use cosmological probes to investigate the nature of dark energy, dark matter and gravity by tracking their observational signatures on the geometry of the universe and on the cosmic history of structure formation. The mission is optimised for two independent primary cosmological probes: Weak gravitational Lensing (WL) and Baryonic Acoustic Oscillations (BAO). The Euclid payload consists of a 1.2 m Korsch telescope designed to provide a large field of view. It carries two instruments with a common field-of-view of {\$\sim${}}0.54 deg2: the visual imager (VIS) and the near infrared instrument (NISP) which contains a slitless spectrometer and a three bands photometer. The Euclid wide survey will cover 15,000 deg2 of the extragalactic sky and is complemented by two 20 deg2 deep fields. For WL, Euclid measures the shapes of 30-40 resolved galaxies per arcmin2 in one broad visible R+I+Z band (550-920 nm). The photometric redshifts for these galaxies reach a precision of dz/(1+z) {\textless} 0.05. They are derived from three additional Euclid NIR bands (Y, J, H in the range 0.92-2.0 micron), complemented by ground based photometry in visible bands derived from public data or through engaged collaborations. The BAO are determined from a spectroscopic survey with a redshift accuracy dz/(1+z) =0.001. The slitless spectrometer, with spectral resolution {\$\sim${}}250, predominantly detects Ha emission line galaxies. Euclid is a Medium Class mission of the ESA Cosmic Vision 2015-2025 programme, with a foreseen launch date in 2019. This report (also known as the Euclid Red Book) describes the outcome of the Phase A study.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the 'Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a (100 cMpc)3 and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts 0 and 1, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar 'downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Li2008, -abstract = {We analyze properties of subhalos/substructures resolved in a dark matter simulation of a Milky Way-like halo in a $\Lambda$CDM cosmology. We explore possible links between subhalos and the Galactic satellites and find: 1) The infall patterns of subhalos are slightly elongated along the major axis of the galaxy halo and are clumpy on smaller scales. 2) The Great disk defined by MW satellites (Kroupa et al. 2005) is easily reproduced in our simulations without recurring to sophisticated galaxy formation recipes and is purely due to their highly centrally concentrated distribution around the Galaxy.}, -archivePrefix = {arXiv}, -arxivId = {0807.2780}, -author = {Li, Yang Shyang and Helmi, Amina}, -doi = {10.1007/978-1-4020-5573-7_53}, -eprint = {0807.2780}, -isbn = {0000000000000}, -issn = {15706605}, -journal = {Astrophysics and Space Science Proceedings}, -keywords = {Dark matter,Galaxies: Dwarf,Galaxies: Kinematics and dynamics,Galaxy: Formation,Methods: Numerical}, -number = {202409}, -pages = {311--314}, -title = {{Infall of substructures onto a milky way-like dark halo}}, -volume = {385}, -year = {2007} -} -@article{Wang2018, -abstract = {We explore the isothermal total density profiles of early-type galaxies (ETGs) in the IllustrisTNG simulation. For the selected 559 ETGs at z = 0 with stellar masses {\$}10{\^{}}{\{}10.7{\}}\backslash, \backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot {\}} \backslashleqslant M{\_}{\{}\backslashast {\}} \backslashleqslant 10{\^{}}{\{}11.9{\}}\backslash, \backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot {\}}{\$}, the total power-law slope has a mean of 〈$\gamma$′〉 = 2.011 ± 0.007 and a scatter of {\$}\backslashsigma {\_}{\{}\backslashgamma {\^{}}{\{}\backslashprime {\}}{\}} = 0.171{\$} over the radial range 0.4–4 times the stellar half-mass radius. Several correlations between $\gamma$′ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction, and in situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduces many correlation trends, and in particular, $\gamma$′ is almost constant with redshift below z = 2. Through analysing IllustrisTNG model variations, we show that black hole kinetic winds are crucial to lowering $\gamma$′ and matching observed galaxy correlations. The effects of stellar winds on $\gamma$′ are subdominant compared to active galactic nucleus (AGN) feedback, and differ due to the presence of AGN feedback from previous works. The density profiles of the ETG dark matter haloes are well described by steeper than NFW profiles, and they are steeper in the full physics (FP) run than their counterparts in the dark matter-only (DMO) run. Their inner density slopes anticorrelate (remain constant) with the halo mass in the FP (DMO) run, and anticorrelate with the halo concentration parameter c200 in both the types of runs. The dark matter haloes of low-mass ETGs are contracted whereas high-mass ETGs are expanded, suggesting that variations in the total density profile occur through the different halo responses to baryons.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -doi = {10.1093/mnras/stz3348}, -eprint = {1811.06545}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology,dark,formation,galaxies,matter,methods,numerical,structure,theory}, -number = {4}, -pages = {5188--5215}, -title = {{Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {491}, -year = {2020} -} -@article{Jackson2015, -abstract = {We present Very Large Array detections of radio emission in 4 four-image gravitational lens systems with quasar sources: HS 0810+2554, RX J0911+0511, HE 0435-1223 and SDSS J0924+0219, and extended Multi-Element Remote Linked Interferometer (e-MERLIN) observations of two of the systems. The first three are detected at a high level of significance, and SDSS J0924+0219 is detected. HS 0810+2554 is resolved, allowing us for the first time to achieve 10-mas resolution of the source frame in the structure of a radio-quiet quasar. The others are unresolved or marginally resolved. All four objects are among the faintest radio sources yet detected, with intrinsic flux densities in the range 1-5 $\mu$Jy; such radio objects, if unlensed, will only be observable routinely with the Square Kilometre Array. The observations of HS 0810+2554, which is also detected with e-MERLIN, strongly suggest the presence of a mini active galactic nucleus, with a radio core and milliarcsecond scale jet. The flux densities of the lensed images in all but HE 0435-1223 are consistent with smooth galaxy lens models without the requirement for smaller scale substructure in the model, although some interesting anomalies are seen between optical and radio flux densities. These are probably due to microlensing effects in the optical.}, -archivePrefix = {arXiv}, -arxivId = {1508.05842}, -author = {Jackson, Neal and Tagore, Amitpal S. and Roberts, Carl and Sluse, Dominique and Stacey, Hannah and Vives-Arias, Hector and Wucknitz, Olaf and Volino, Filomena}, -doi = {10.1093/mnras/stv1982}, -eprint = {1508.05842}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Jackson2015SLRadioMaseMerlin.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Gravitational lensing: strong,Quasars: general,Radio continuum: galaxies}, -number = {1}, -pages = {287--298}, -title = {{Observations of radio-quiet quasars at 10-mas resolution by use of gravitational lensing}}, -volume = {454}, -year = {2015} -} -@article{Peng2010, -abstract = {We present a two-dimensional (2D) fitting algorithm (GALFIT, ver. 3) with new capabilities to study the structural components of galaxies and other astronomical objects in digital images. Our technique improves on previous 2D fitting algorithms by allowing for irregular, curved, logarithmic and power-law spirals, ring, and truncated shapes in otherwise traditional parametric functions like the S{\'{e}}rsic, Moffat, King, Ferrer, etc., profiles. One can mix and match these new shape features freely, with or without constraints, and apply them to an arbitrary number of model components of numerous profile types, so as to produce realistic-looking galaxy model images. Yet, despite the potential for extreme complexity, the meaning of the key parameters like the S{\'{e}}rsic index, effective radius, or luminosity remains intuitive and essentially unchanged. The new features have an interesting potential for use to quantify the degree of asymmetry of galaxies, to quantify low surface brightness tidal features beneath and beyond luminous galaxies, to allow more realistic decompositions of galaxy subcomponents in the presence of strong rings and spiral arms, and to enable ways to gauge the uncertainties when decomposing galaxy subcomponents. We illustrate these new features by way of several case studies that display various levels of complexity. {\textcopyright}2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0912.0731}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans Walter}, -doi = {10.1088/0004-6256/139/6/2097}, -eprint = {0912.0731}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Galaxies: bulges,Galaxies: fundamental parameters,Galaxies: structure,Techniques: image processing,Techniques: photometric}, -number = {6}, -pages = {2097--2129}, -title = {{Detailed decomposition of galaxy images. II. beyond axisymmetric models}}, -volume = {139}, -year = {2010} -} -@article{Geometryep, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Rest2001, -author = {Rest, Armin and Bosch, Frank C V A N D E N and Tran, Hien and Tsvetanov, Zlatan and Ford, Holland C and Davies, James and Schafer, Joanna}, -journal = {Database}, -keywords = {cd {\`{e}} galaxies,elliptical and lenticular,galaxies,nuclei {\`{e}} galaxies,structure}, -number = {1995}, -title = {{WFPC2 IMAGES OF THE CENTRAL REGIONS OF EARLY-TYPE GALAXIES . I . THE DATA AND We present high-resolution R-band images of the central regions of 67 early-type galaxies obtained with the Wide Field and Planetary Camera 2 ( WFPC2 ) aboard the Hubble Space T}}, -year = {2001} -} -@article{2001ez, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Oriordan2024, -abstract = {Strong gravitational lensing can be used to find otherwise invisible dark matter subhaloes. In such an analysis, the lens galaxy mass model is a significant source of systematic uncertainty. In this paper, we analyse the effect of angular complexity in the lens model. We use multipole perturbations that introduce low-order deviations from pure ellipticity in the isodensity contours, keeping the radial density profile fixed. We find that, in Hubble Space Telescope-like data, multipole perturbations consistent with those seen in galaxy isophotes are very effective at causing false positive substructure detections. We show that the effectiveness of this degeneracy depends on the deviation from a pure ellipse and the lensing configuration. We find that, when multipoles of 1 per cent are allowed in the lens model, the area in the observation where a subhalo could be detected drops by a factor of 3. Sensitivity away from the lensed images is mostly lost. However, the mass limit of detectable objects on or close to the lensed images does not change. We do not expect the addition of multipole perturbations to lens models to have a significant effect on the ability of strong lensing to constrain the underlying dark matter model. However, given the high rate of false positive detections, angular complexity beyond the elliptical power law should be included for such studies to be reliable. We discuss implications for previous detections and future work.}, -archivePrefix = {arXiv}, -arxivId = {2310.10714}, -author = {O'riordan, Conor M. and Vegetti, Simona}, -doi = {10.1093/mnras/stae153}, -eprint = {2310.10714}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/ORiodan2024Angularcomplexity.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {dark matter,gravitational lensing: strong}, -number = {2}, -pages = {1757--1768}, -title = {{Angular complexity in strong lens substructure detection}}, -volume = {528}, -year = {2024} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kremer et al. - 2017 - Big Universe, Big Data Machine Learning and Image Analysis for Astronomy.pdf:pdf}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Moore1999, -abstract = {We use numerical simulations to examine the substructure within galactic and cluster mass halos that form within a hierarchical universe. Clusters are easily reproduced with a steep mass spectrum of thousands of substructure clumps that closely matches observations. However, the survival of dark matter substructure also occurs on galactic scales, leading to the remarkable result that galaxy halos appear as scaled versions of galaxy clusters. The model predicts that the virialised extent of the Milky Way's halo should contain about 500 satellites with circular velocities larger than Draco and Ursa-Minor i.e. bound masses > 10^8Mo and tidally limited sizes > kpc. The substructure clumps are on orbits that take a large fraction of them through the stellar disk leading to significant resonant and impulsive heating. Their abundance and singular density profiles has important implications for the existence of old thin disks, cold stellar streams, gravitational lensing and indirect/direct detection experiments.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9907411}, -author = {Moore, Ben and Ghigna, Sebastiano and Governato, Fabio and Lake, George and Quinn, Thomas and Stadel, Joachim and Tozzi, Paolo}, -doi = {10.1086/312287}, -eprint = {9907411}, -isbn = {1538-4357}, -issn = {0004637X}, -journal = {ApJ}, -keywords = {COSMOLOGY: DARK MATTER,COSMOLOGY: OBSERVATIONS,COSMOLOGY: THEORY,Cosmology: Dark Matter,Cosmology: Observations,Cosmology: Theory,GALAXIES: CLUSTERS: GENERAL,GALAXIES: FORMATION,Galaxies: Clusters: General,Galaxies: Formation}, -month = {oct}, -number = {1}, -pages = {L19--L22}, -primaryClass = {astro-ph}, -title = {{Dark Matter Substructure within Galactic Halos}}, -url = {http://arxiv.org/abs/astro-ph/9907411%0Ahttp://dx.doi.org/10.1086/312287}, -volume = {524}, -year = {1999} -} -@article{Brewer2012a, -abstract = {We present gravitational lens models for 20 strong gravitational lens systems observed as part of the Sloan WFC Edge-on Late-type Lens Survey (SWELLS) project. 15 of the lenses are taken from Paper I, while five are newly discovered systems. The systems are galaxy-galaxy lenses where the foreground deflector has an inclined disc, with a wide range of morphological types, from late-type spiral to lenticular. For each system, we compare the total mass inside the critical curve inferred from gravitational lens modelling to the stellar mass inferred from stellar population synthesis (SPS) models, computing the stellar mass fraction f*≡M SPS/M lens. We find that, for the lower mass SWELLS systems, adoption of a Salpeter stellar initial mass function (IMF) leads to estimates of f* that exceed 1. This is unphysical and provides strong evidence against the Salpeter IMF being valid for these systems. Taking the lower mass end of the SWELLS sample ($\sigma$ SIE < 230kms -1), we find that the IMF is lighter (in terms of stellar mass-to-light ratio) than Salpeter with 98 percent probability, and consistent with the Chabrier IMF and IMFs between the two. This result is consistent with previous studies of spiral galaxies based on independent techniques. In combination with recent studies of massive early-type galaxies that have favoured a heavier Salpeter-like IMF, this result strengthens the evidence against a universal stellar IMF. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.1677}, -author = {Brewer, Brendon J. and Dutton, Aaron A. and Treu, Tommaso and Auger, Matthew W. and Marshall, Philip J. and Barnab{\`{e}}, Matteo and Bolton, Adam S. and Koo, David C. and Koopmans, L{\'{e}}on V.E.}, -doi = {10.1111/j.1365-2966.2012.20870.x}, -eprint = {1201.1677}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Brewer et al. - 2012 - The SWELLS survey - III. Disfavouring 'heavy' initial mass functions for spiral lens galaxies.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Stars: luminosity function, mass function}, -number = {4}, -pages = {3574--3590}, -title = {{The SWELLS survey - III. Disfavouring 'heavy' initial mass functions for spiral lens galaxies}}, -volume = {422}, -year = {2012} -} -@article{VanderTol2019, -abstract = {In radio astronomy obtaining a high dynamic range in synthesis imaging of wide fields requires a correction for time and direction-dependent effects. Applying direction-dependent correction can be done by either partitioning the image in facets and applying a direction-independent correction per facet, or by including the correction in the gridding kernel (AW-projection). An advantage of AW-projection over faceting is that the effectively applied beam is a sinc interpolation of the sampled beam, where the correction applied in the faceting approach is a discontinuous piece wise constant beam. However, AW-projection quickly becomes prohibitively expensive when the corrections vary over short time scales. This occurs for example when ionospheric effects are included in the correction. The cost of the frequent recomputation of the oversampled convolution kernels then dominates the total cost of gridding. Image domain gridding is a new approach that avoids the costly step of computing oversampled convolution kernels. Instead low-resolution images are made directly for small groups of visibilities which are then transformed and added to the large uv grid. The computations have a simple, highly parallel structure that maps very well onto massively parallel hardware such as graphical processing units (GPUs). Despite being more expensive in pure computation count, the throughput is comparable to classical W-projection. The accuracy is close to classical gridding with a continuous convolution kernel. Compared to gridding methods that use a sampled convolution function, the new method is more accurate. Hence the new method is at least as fast and accurate as classical W-projection, while allowing for the correction for quickly varying direction-dependent effects.}, -archivePrefix = {arXiv}, -arxivId = {1909.07226}, -author = {van der Tol, Sebastiaan and Veenboer, Bram and Offringa, Andr{\'{e}} R.}, -doi = {10.1051/0004-6361/201832858}, -eprint = {1909.07226}, -file = {:C\:/Users/Jammy/Documents/Papers/uvplane/ImagePlaneGridding.pdf:pdf}, -issn = {23318422}, -journal = {arXiv}, -keywords = {Instrumentation: interferometers,Methods: numerical,Techniques: image processing}, -number = {2015}, -pages = {1--14}, -title = {{Image Domain Gridding: a fast method for convolutional resampling of visibilities}}, -year = {2019} -} -@article{Boylan2011, -abstract = {We show that dissipationless $\Lambda$ cold dark matter simulations predict that the majority of the most massive subhaloes of the Milky Way are too dense to host any of its bright satellites (LV> 105L⊙). These dark subhaloes have peak circular velocities at infall ofVinfall= 30-70kms-1 and infall masses of (0.2-4) × 1010M⊙. Unless the Milky Way is a statistical anomaly, this implies that galaxy formation becomes effectively stochastic at these masses. This is in marked contrast to the well-established monotonic relation between galaxy luminosity and halo circular velocity (or halo mass) for more massive haloes. We show that at least two (and typically four) of these massive dark subhaloes are expected to produce a larger dark matter annihilation flux than Draco. It may be possible to circumvent these conclusions if baryonic feedback in dwarf satellites or different dark matter physics can reduce the central densities of massive subhaloes by order unity on a scale of 0.3-1 kpc. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1103.0007}, -author = {Boylan-Kolchin, Michael and Bullock, James S. and Kaplinghat, Manoj}, -doi = {10.1111/j.1745-3933.2011.01074.x}, -eprint = {1103.0007}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Dark matter,Galaxies: abundances,Galaxy: halo}, -number = {1}, -pages = {40--44}, -title = {{Too big to fail? The puzzling darkness of massive Milky Way subhaloes}}, -volume = {415}, -year = {2011} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Sonnenfeld2013a, -abstract = {We describe the goals of the CASTLES (CfA-Arizona-Space-Telescope-LEns-Survey) 1 project including a sample of NICMOS images of gravitational lenses and a brief list of the preliminary findings.}, -annote = {From Duplicate 14 (Supermassive black holes and their host spheroids I. Galaxy vivisection - Savorgnan, Giulia A. D.; Graham, Alister W.) - -NULL}, -archivePrefix = {arXiv}, -arxivId = {1211.0310}, -author = {Mu{\~{n}}oz, J. A. and Falco, E. E. and Kochanek, C. S. and Leh{\'{a}}r, J. and Mcleod, B. A. and Impey, C. D. and Rix, H. W. and Peng, C. Y.}, -doi = {10.1023/a:1002120921330}, -eprint = {1211.0310}, -isbn = {doi:10.1088/0004-637X/786/2/89}, -issn = {0004640X}, -journal = {Astrophysics and Space Science}, -keywords = {Astrophysics - Cosmology and Extragalactic Astroph,Black hole physics,Data analysis,Galaxies: active,Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure,Gravitational lensing: strong-methods,High Energy Physics - Experiment,Methods: numerical,Methods: statistical,Techniques: image processing,active,cD,catalogs,ccd,cte,cti,dwarf,evolution,formation,fundamental parameters,galaxies,galaxies: elliptical and lenticular,galaxies: formation,galaxies: high-redshift,galaxies: photometry,galaxies: statistics,galaxies: structure,galaxies: structure surveys,general,gravitational lensing,hxmt,interactions,irregular,ism,keyword1,keyword2,keyword3,le,proton-irradiated,quasars,scd,star formation,strong - galaxies,struc-,structure}, -month = {jun}, -number = {1-4}, -pages = {51--54}, -title = {{The castles project}}, -url = {http://arxiv.org/abs/1211.0310}, -volume = {263}, -year = {1998} -} -@article{Madau2014, -abstract = {Over the past two decades, an avalanche of new data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Here we review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch. A consistent picture is emerging, whereby the star-formation rate density peaked approximately 3.5 Gyr after the Big Bang, at z≈1.9, and declined exponentially at later times, with an e-folding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before a redshift z = 1.3. About 25% formed before the peak of the cosmic star-formation rate density, and another 25% formed after z = 0.7. Less than ∼1% of today's stars formed during the epoch of reionization. Under the assumption of a universal initial mass function, the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding star-formation activity. The comoving rates of star formation and central black hole accretion follow a similar rise and fall, offering evidence for coevolution of black holes and their host galaxies. The rise of the mean metallicity of the Universe to about 0.001 solar by z = 6, one Gyr after the Big Bang, appears to have been accompanied by the production of fewer than ten hydrogen Lyman-continuum photons per baryon, a rather tight budget for cosmological reionization. Copyright {\textcopyright} 2014 by Annual Reviews.}, -archivePrefix = {arXiv}, -arxivId = {1403.0007}, -author = {Madau, Piero and Dickinson, Mark}, -doi = {10.1146/annurev-astro-081811-125615}, -eprint = {1403.0007}, -isbn = {1539-3704 (Electronic)\r0003-4819 (Linking)}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {cosmology,evolution,galaxy formation,star formation,stellar populations}, -month = {aug}, -number = {1}, -pages = {415--486}, -pmid = {23856689}, -title = {{Cosmic star-formation history}}, -url = {http://arxiv.org/abs/1403.0007%0Ahttp://dx.doi.org/10.1146/annurev-astro-081811-125615}, -volume = {52}, -year = {2014} -} -@article{Wong2011, -abstract = {Using new photometric and spectroscopic data in the fields of nine strong gravitational lenses that lie in galaxy groups, we analyze the effects of both the local group environment and line-of-sight (LOS) galaxies on the lens potential. We use Monte Carlo simulations to derive the shear directly from measurements of the complex lens environment, providing the first detailed independent check of the shear obtained from lens modeling. We account for possible tidal stripping of the group galaxies by varying the fraction of total mass apportioned between the group dark matter halo and individual group galaxies. The environment produces an average shear of $\gamma$ = 0.08 (ranging from 0.02 to 0.17), significant enough to affect quantities derived from lens observables. However, the direction and magnitude of the shears do not match those obtained from lens modeling in three of the six four-image systems in our sample (B1422, RXJ1131, and WFI2033). The source of this disagreement is not clear, implying that the assumptions inherent in both the environment and lens model approaches must be reconsidered. If only the local group environment of the lens is included, the average shear is $\gamma$ = 0.05 (ranging from 0.01 to 0.14), indicating that LOS contributions to the lens potential are not negligible.We isolate the effects of various theoretical and observational uncertainties on our results. Of those uncertainties, the scatter in the Faber-Jackson relation and error in the group centroid position dominate. Future surveys of lens environments should prioritize spectroscopic sampling of both the local lens environment and objects along the LOS, particularly those bright (I <21.5) galaxies projected within 5' of the lens. {\textcopyright} 2011 The American Astronomical Society. All rights reserved.}, -author = {Wong, Kenneth C. and Keeton, Charles R. and Williams, Kurtis A. and Momcheva, Ivelina G. and Zabludoff, Ann I.}, -doi = {10.1088/0004-637X/726/2/84}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Wong2011ShearEnvironment.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {Gravitational lensing: strong}, -number = {2}, -title = {{The effect of environment on shear in strong gravitational lenses}}, -volume = {726}, -year = {2011} -} -@article{Bezanson2009, -abstract = {Recent studies have shown that massive quiescent galaxies at high redshift are much more compact than present-day galaxies of the same mass. Here we compare the radial stellar density profiles and the number density of a sample of massive galaxies at z 2.3 to nearby massive elliptical galaxies. We confirm that the average stellar densities of the z 2.3 galaxies within the effective radius, $\rho$(28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of $\sim$7000 massive galaxies at z $\sim$ 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E. and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2018 - Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 z 0.5 using Hyper Suprime-Cam(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 < z < 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Greene2013, -abstract = {We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions $\sigma$* ≳ 150 km s-1. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼ 10 Gyr), relatively metal-poor ([Fe/H] ≈ -0.5), and $\alpha$-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z ≈ 1.5-2). {\textcopyright}2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1308.2682}, -author = {Greene, Jenny E and Murphy, Jeremy D and Graves, Genevieve J and Gunn, James E and Raskutti, Sudhir and Comerford, Julia M and Gebhardt, Karl}, -doi = {10.1088/0004-637X/776/2/64}, -eprint = {1308.2682}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: abundances,galaxies: elliptical and lenticular,galaxies: evolution}, -number = {2}, -title = {{The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius}}, -volume = {776}, -year = {2013} -} -@article{Thomas2014, -abstract = {The most massive elliptical galaxies have low-density centers or cores that differ dramatically from the high-density centers of less massive ellipticals and bulges of disk galaxies. These cores have been interpreted as the result of mergers of supermassive black hole binaries, which depopulate galaxy centers by gravitationally slingshotting central stars toward large radii. Such binaries naturally form in mergers of luminous galaxies. Here, we analyze the population of central stellar orbits in 11 massive elliptical galaxies that we observed with the integral field spectrograph SINFONI at the European Southern Observatory Very Large Telescope. Our dynamical analysis is orbit-based and includes the effects of a central black hole, the mass distribution of the stars, and a dark matter halo. We show that the use of integral field kinematics and the inclusion of dark matter is important to conclude on the distribution of stellar orbits in galaxy centers. Six of our galaxies are core galaxies. In these six galaxies, but not in the galaxies without cores, we detect a coherent lack of stars on radial orbits in the core region and a uniform excess of radial orbits outside of it: when scaled by the core radius rb , the radial profiles of the classical anisotropy parameter $\beta$(r) are nearly identical in core galaxies. Moreover, they quantitatively match the predictions of black hole binary simulations, providing the first convincing dynamical evidence for core scouring in the most massive elliptical galaxies. {\textcopyright} 2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1311.3783}, -author = {Thomas, J. and Saglia, R. P. and Bender, R. and Erwin, P. and Fabricius, M.}, -doi = {10.1088/0004-637X/782/1/39}, -eprint = {1311.3783}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Thomas2013DynamicalFootprintCoreScouring.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {39}, -title = {{The dynamical fingerprint of core scouring in massive elliptical galaxies}}, -volume = {782}, -year = {2014} -} -@article{Greene2012, -abstract = {We use the Mitchell Spectrograph (formerly VIRUS-P) on the McDonald Observatory 2.7m Harlan J. Smith Telescope to search for the chemical signatures of massive elliptical galaxy assembly. The Mitchell Spectrograph is an integral-field spectrograph with a uniquely wide field of view (107x107 sq arcsec), allowing us to achieve remarkably high signal-to-noise ratios of {\$\sim${}}20-70 per pixel in radial bins of 2-2.5 times the effective radii of the eight galaxies in our sample. Focusing on a sample of massive elliptical galaxies with stellar velocity dispersions sigma* {\textgreater} 150 km/s, we study the radial dependence in the equivalent widths (EWs) of key metal absorption lines. By twice the effective radius, the Mgb EWs have dropped by {\$\sim${}}50{\%}, and only a weak correlation between sigma* and Mgb EW remains. The Mgb EWs at large radii are comparable to those seen in the centers of elliptical galaxies that are approximately an order of magnitude less massive. We find that the well-known metallicity gradients often observed within an effective radius continue smoothly to 2.5R{\_}e, while the abundance ratio gradients remain flat. Much like the halo of the Milky Way, the stellar halos of our galaxies have low metallicities and high alpha-abundance ratios, as expected for very old stars formed in small stellar systems. Our observations support a picture in which the outer parts of massive elliptical galaxies are built by the accretion of much smaller systems whose star formation history was truncated at early times.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -volume = {786}, -year = {2014} -} -@article{Feroz2007, -abstract = {In performing a Bayesian analysis of astronomical data, two difficult problems often emerge. First, in estimating the parameters of some model for the data, the resulting posterior distribution may be multimodal or exhibit pronounced (curving) degeneracies, which can cause problems for traditional Markov Chain Monte Carlo (MCMC) sampling methods. Secondly, in selecting between a set of competing models, calculation of the Bayesian evidence for each model is computationally expensive using existing methods such as thermodynamic integration. The nested sampling method introduced by Skilling, has greatly reduced the computational expense of calculating evidence and also produces posterior inferences as a by-product. This method has been applied successfully in cosmological applications by Mukherjee, Parkinson & Liddle, but their implementation was efficient only for unimodal distributions without pronounced degeneracies. Shaw, Bridges & Hobson recently introduced a clustered nested sampling method which is significantly more efficient in sampling from multimodal posteriors and also determines the expectation and variance of the final evidence from a single run of the algorithm, hence providing a further increase in efficiency. In this paper, we build on the work of Shaw et al. and present three new methods for sampling and evidence evaluation from distributions that may contain multiple modes and significant degeneracies in very high dimensions; we also present an even more efficient technique for estimating the uncertainty on the evaluated evidence. These methods lead to a further substantial improvement in sampling efficiency and robustness, and are applied to two toy problems to demonstrate the accuracy and economy of the evidence calculation and parameter estimation. Finally, we discuss the use of these methods in performing Bayesian object detection in astronomical data sets, and show that they significantly outperform existing MCMC techniques. An implementation of our methods will be publicly released shortly. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0704.3704}, -author = {Feroz, F. and Hobson, M. P.}, -doi = {10.1111/j.1365-2966.2007.12353.x}, -eprint = {0704.3704}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {2}, -pages = {449--463}, -pmid = {358711}, -title = {{Multimodal nested sampling: An efficient and robust alternative to Markov Chain Monte Carlo methods for astronomical data analyses}}, -volume = {384}, -year = {2008} -} -@article{Spindler2017, -abstract = {We study the spatially resolved star formation of 1494 galaxies in the SDSS-IV MaNGA Survey. Star formation rates (SFRs) are calculated using a two-step process, using H$\alpha$ in starforming regions and Dn4000 in regions identified as active galactic nucleus/low-ionization (nuclear) emission region [AGN/LI(N)ER] or lineless. The roles of secular and environmental quenching processes are investigated by studying the dependence of the radial profiles of specific star formation rate on stellar mass, galaxy structure, and environment. We report on the existence of 'centrally suppressed' galaxies, which have suppressed Specific Star Formation Rate (SSFR) in their cores compared to their discs. The profiles of centrally suppressed and unsuppressed galaxies are distributed in a bimodal way. Galaxies with high stellar mass and core velocity dispersion are found to be much more likely to be centrally suppressed than low-mass galaxies, and we show that this is related to morphology and the presence of AGN/LI(N)ER like emission. Centrally suppressed galaxies also display lower star formation at all radii compared to unsuppressed galaxies. The profiles of central and satellite galaxies are also compared, and we find that satellite galaxies experience lower specific star formation rates at all radii than central galaxies. This uniform suppression could be a signal of the stripping of hot halo gas in the process known as strangulation. We find that satellites are not more likely to be suppressed in their cores than centrals, indicating that the core suppression is an entirely internal process. We find no correlation between the local environment density and the profiles of star formation rate surface density.}, -archivePrefix = {arXiv}, -arxivId = {1710.05049}, -author = {Spindler, Ashley and Wake, David and Belfiore, Francesco and Bershady, Matthew and Bundy, Kevin and Drory, Niv and Masters, Karen and Thomas, Daniel and Westfall, Kyle and Wild, Vivienne}, -doi = {10.1093/mnras/sty247}, -eprint = {1710.05049}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Bulges,Galaxies: Clusters: General,Galaxies: Evolution,Galaxies: Groups: General,Galaxies: Star formation,Galaxies: Structure}, -number = {1}, -pages = {580--600}, -title = {{SDSS-IV MaNGA: The spatial distribution of star formation and its dependence on mass, structure, and environment}}, -url = {http://arxiv.org/abs/1710.05049}, -volume = {476}, -year = {2018} -} -@article{Calanog2014, -abstract = {We present Keck-Adaptive Optics and Hubble Space Telescope high resolution near-infrared (IR) imaging for 500 $\mu$m bright candidate lensing systems identified by the Herschel Multi-tiered Extragalactic Survey and Herschel Astrophysical Terahertz Large Area Survey. Out of 87 candidates with near-IR imaging, 15 (∼17%) display clear near-IR lensing morphologies. We present near-IR lens models to reconstruct and recover basic rest-frame optical morphological properties of the background galaxies from 12 new systems. Sources with the largest near-IR magnification factors also tend to be the most compact, consistent with the size bias predicted from simulations and previous lensing models for submillimeter galaxies (SMGs). For four new sources that also have high-resolution submillimeter maps, we test for differential lensing between the stellar and dust components and find that the 880 $\mu$m magnification factor ($\mu$880) is ∼1.5 times higher than the near-IR magnification factor ($\mu$NIR), on average. We also find that the stellar emission is ∼2 times more extended in size than dust. The rest-frame optical properties of our sample of Herschel-selected lensed SMGs are consistent with those of unlensed SMGs, which suggests that the two populations are similar.}, -archivePrefix = {arXiv}, -arxivId = {1406.1487}, -author = {Calanog, J. A. and Fu, Hai and Cooray, A. and Wardlow, J. and Ma, B. and Amber, S. and Baker, A. J. and Baes, M. and Bock, J. and Bourne, N. and Bussmann, R. S. and Casey, C. M. and Chapman, S. C. and Clements, D. L. and Conley, A. and Dannerbauer, H. and {De Zotti}, G. and Dunne, L. and Dye, S. and Eales, S. and Farrah, D. and Furlanetto, C. and Harris, A. I. and Ivison, R. J. and Kim, S. and Maddox, S. J. and Magdis, G. and Messias, H. and Micha{\l}lowski, M. J. and Negrello, M. and Nightingale, J. and O'Bryan, J. M. and Oliver, S. J. and Riechers, D. and Scott, D. and Serjeant, S. and Simpson, J. and Smith, M. and Timmons, N. and Thacker, C. and Valiante, E. and Vieira, J. D.}, -doi = {10.1088/0004-637X/797/2/138}, -eprint = {1406.1487}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: star formation,Gravitational lensing: strong,Submillimeter: galaxies}, -number = {2}, -pages = {126--138}, -title = {{Lens models of herschel-selected galaxies from high-resolution near-IR observations}}, -url = {http://stacks.iop.org/0004-637X/797/i=2/a=138?key=crossref.4244e3e383c14bc754f84ba66e968d77%5Cnpapers3://publication/doi/10.1088/0004-637X/797/2/138}, -volume = {797}, -year = {2014} -} -@article{Powell2023, -abstract = {Using a single gravitational lens system observed at ≲ 5 mas resolution with very long baseline interferometry, we place a lower bound on the mass of the fuzzy dark matter (FDM) particle, ruling out m$\chi$ ≤ 4.4 × 10−21 eV with a 20:1 posterior odds ratio relative to a smooth lens model. We generalize our result to non-scalar and multiple-field models, such as vector FDM, with m$\chi$,vec > 1.4 × 10−21 eV. Due to the extended source structure and high angular resolution of the observation, our analysis is directly sensitive to the presence of granule structures in the main dark matter halo of the lens, which is the most generic prediction of FDM theories. A model based on well-understood physics of ultra-light dark matter fields in a gravitational potential well makes our result robust to a wide range of assumed dark matter fractions and velocity dispersions in the lens galaxy. Our result is competitive with other lower bounds on m$\chi$ from past analyses, which rely on intermediate modelling of structure formation and/or baryonic effects. Higher resolution observations taken at 10–100 GHz could improve our constraints by up to two orders of magnitude in the future.}, -archivePrefix = {arXiv}, -arxivId = {2302.10941}, -author = {Powell, Devon M and Vegetti, Simona and McKean, J P and White, Simon D M and Ferreira, Elisa G M and May, Simon and Spingola, Cristiana}, -doi = {10.1093/mnrasl/slad074}, -eprint = {2302.10941}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Powell et al. - 2023 - A lensed radio jet at milli-arcsecond resolution – II. Constraints on fuzzy dark matter from an extended gravitat.pdf:pdf}, -issn = {1745-3925}, -journal = {MNRAS Letters}, -keywords = {2716,cosmology,dark matter,galaxies,general,gravitational lensing,haloes,individual,mg j0751,quasars,radio continuum,strong}, -number = {1}, -pages = {L84--L88}, -title = {{A lensed radio jet at milli-arcsecond resolution – II. Constraints on fuzzy dark matter from an extended gravitational arc}}, -volume = {524}, -year = {2023} -} -@article{Cohen2018, -abstract = {We present HST/ACS imaging of twenty-three very low surface brightness ({\$}\backslashmu{\_}{\{}e,V{\}}{\$}=25-27.5) galaxies detected in the fields of four nearby galaxy groups. These objects were selected from deep optical imaging obtained with the Dragonfly Telephoto Array. Seven are new discoveries, while most of the others had been identified previously in visual surveys of deep photographic plates and more recent surveys. Few have previously been studied in detail. From the ACS images, we measure distances to the galaxies using both the tip of the red giant branch method and the surface brightness fluctuations method. We demonstrate that the two methods are consistent with each other in the regime where both can be applied. The distances to 15 out of 20 galaxies with stable measurements are consistent with that of the targeted group within errors. This suggests that assuming group membership based solely on projected proximity is {\$\sim${}}75{\%} successful in this regime. The galaxies are nearly round, with a median axis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The objects have a range of sizes, from {\$}R{\_}e{\$}=0.4 kpc to {\$}R{\_}e{\$}=1.8 kpc, with a median of 1.0 kpc. They range in luminosity from {\$}M{\_}V{\$}=-11.4 to {\$}M{\_}V{\$}=-15.6, with a median of -12.4. Galaxies with {\$}R{\_}e{\$}{\$\sim${}}1 kpc and {\$}M{\_}V{\$}{\$\sim${}}-12 are fairly rare in the Local Group but we find many of them in this relatively small sample. Four of the objects fall in the class of ultra diffuse galaxies (UDGs), with {\$}R{\_}e{\$}{\textgreater}1.5 kpc and {\$}\backslashmu{\_}{\{}0,V{\}}{\$}{\textgreater}24 mag/arcsec{\^{}}2, including the recently identified dark matter deficient galaxy NGC1052-DF2.}, -archivePrefix = {arXiv}, -arxivId = {1807.06016}, -author = {Cohen, Yotam and van Dokkum, Pieter and Danieli, Shany and Romanowsky, Aaron J and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Mowla, Lamiya and Kruijssen, J M Diederik and Conroy, Charlie and Wasserman, Asher}, -doi = {10.3847/1538-4357/aae7c8}, -eprint = {1807.06016}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {Astrophysics,Astrophysics of Galaxies}, -number = {2}, -pages = {96}, -title = {{ The Dragonfly Nearby Galaxies Survey. V. HST /ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC 1052, NGC 1084, M96, and NGC 4258 }}, -url = {http://arxiv.org/abs/1807.06016%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aae7c8}, -volume = {868}, -year = {2018} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M* > 1011M⊙ galaxies at 1 < z < 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 < z < 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V. A. and Dunlop, J. S. and McLure, R. J. and Cirasuolo, M. and Buitrago, F. and Bowler, R. A.A. and Targett, T. A. and Bell, E. F. and McIntosh, D. H. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Hartley, W. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and McGrath, E. J.}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure}, -month = {oct}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 < z < 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.5221}, -volume = {444}, -year = {2014} -} -@article{Hilz2013, -abstract = {There is observational evidence for inside-out growth of giant elliptical galaxies since z≳ 2-3, which is - in contrast to disc galaxies - not driven by in situ star formation. Many of the $\sim$1011M⊙ systems at high redshift have small sizes $\sim$1 kpc and surface brightness profiles with low-{\'{S}}ersic indices n. The most likely descendants at z = 0 have, on average, grown by a factor of 2 in mass and a factor of 4 in size, indicating r$\alpha$ M$\alpha$ with $\alpha$ ≳2. They also have surface brightness profiles with n ≳ 5. This evolution can be qualitatively explained on the basis of two assumptions: compact ellipticals predominantly grow by collisionless minor (mass-ratio 1:10) or intermediate (mass-ratio 1:5) 'dry' mergers, and they are embedded in massive dark matter haloes which support the stripping of merging satellite stars at large radii. We draw these conclusions from idealized collisionless mergers spheroidal galaxies - with and without dark matter - with mass ratios of 1:1, 1:5 and 1:10. The sizes evolve as r$\alpha$ M$\alpha$ with$\alpha$ <2 for mass-ratios of 1:1 (and 1:5 without dark matter haloes) and, while doubling the stellar mass, the {\'{S}}ersic index increases from n $\sim$ 4 to n $\sim$ 5. For minor mergers of galaxies embedded in dark matter haloes, the sizes grow significantly faster and the profile shapes change more rapidly. Surprisingly, already mergers with moderate mass-ratios of 1:5, well motivated by recent cosmological simulations, give $\alpha$ $\sim$ 2.3 and after only two merger generations ($\sim$40 per cent added stellar mass) the {\'{S}}ersic index has increased to n > 8 (n $\sim$ 5.5 without dark matter), reaching a final value of n = 9.5 after doubling the stellar mass. This is accompanied by a significant increase of the dark matter fraction (from $\sim$40 to ≳70 per cent) within the stellar half-mass radius, driven by the strong size increase probing larger, dark matter-dominated regions. For equal-mass mergers the effect is much weaker. We conclude that only a few intermediate mass-ratio mergers ($\sim$3-5 with initial mass-ratios of 1:5) of galaxies embedded in massive dark matter haloes can result in the observed concurrent inside-out growth and the rapid evolution in profile shapes. This process might explain the existence of present-day giant ellipticals with sizes, r > 4 kpc, high {\'{S}}ersic indices, n > 5, and a significant amount of dark matter within the half-light radius. Apart from negative stellar metallicity gradients such a 'minor' merger scenario also predicts significantly lower dark matter fractions for z $\sim$ 2 compact quiescent galaxies and their rare present-day analogues. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1206.5004}, -author = {Hilz, Michael and Naab, Thorsten and Ostriker, J. P.}, -doi = {10.1093/mnras/sts501}, -eprint = {1206.5004}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cd-Galaxies,Galaxies,ellipticals and lenticular,evolution-Galaxies,fundamental parameters-Galaxies,haloes-galaxies,photometry-Galaxies,structure}, -month = {mar}, -number = {4}, -pages = {2924--2933}, -title = {{How do minor mergers promote inside-out growth of ellipticals, transforming the size, density profile and dark matter fraction?}}, -volume = {429}, -year = {2013} -} -@article{Birrer2017, -abstract = {We present a simple method to accurately infer line of sight (LOS) integrated lensing effects for galaxy scale strong lens systems through image reconstruction. Our approach enables us to separate weak lensing LOS effects from the main strong lens deflector. We test our method using mock data and show that strong lens systems can be accurate probes of cosmic shear with a precision on the shear terms of ± 0.003 (statistical error) for an HST-like dataset. We apply our formalism to reconstruct the lens COSMOS 0038+4133 and its LOS. In addition, we estimate the LOS properties with a halo-rendering estimate based on the COSMOS field galaxies and a galaxy-halo connection. The two approaches are independent and complementary in their information content. We find that when estimating the convergence at the strong lens system, performing a joint analysis improves the measure by a factor of two compared to a halo model only analysis. Furthermore the constraints of the strong lens reconstruction lead to tighter constraints on the halo masses of the LOS galaxies. Joint constraints of multiple strong lens systems may add valuable information to the galaxy-halo connection and may allow independent weak lensing shear measurement calibrations.}, -archivePrefix = {arXiv}, -arxivId = {1610.01599}, -author = {Birrer, Simon and Welschen, Cyril and Amara, Adam and Refregier, Alexandre}, -doi = {10.1088/1475-7516/2017/04/049}, -eprint = {1610.01599}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Birrer2019ShearWLSL.pdf:pdf}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {gravitational lensing,weak gravitational lensing}, -number = {4}, -title = {{Line-of-sight effects in strong lensing: Putting theory into practice}}, -volume = {2017}, -year = {2017} -} -@article{Morishita2018, -abstract = {Observations have revealed log M*/Msun {\textgreater}11 galaxies that were already dead when the universe was only {\$\sim${}}2Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interests. In this paper, we study star formation and metallicity enrichment histories of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple HST surveys allows robust determination of their SEDs. Our new SED modeling provides mass accumulation/stellar metallicity enrichment histories of those galaxies over the past {\$\sim${}}3Gyr, with no functional assumptions on their star formation histories. We find that most of our massive galaxies have formed {\textgreater}50{\%} of their extant masses by {\$\sim${}}1.5Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Most of our galaxies already have stellar metallicities compatible with, or even higher than, those of local early-type galaxies, with a median value of log Z*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. By using reconstructed star formation history, we reveal their rapid metallicity enrichment history from z{\$\sim${}}5.5 to 2.2 at a rate of {\$\sim${}}0.2dex/Gyr in logZ*/Zsun. The inferred metallicities are on average {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies at the time of formation. This supports a view where quenched galaxies continue to form stars at low-level until recently, rather than abrupt termination of star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -eprint = {1812.06980}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {February}, -pages = {1--13}, -title = {{Massive Dead Galaxies at z{\$\sim${}}2 with HST Grism Spectroscopy I. Star Formation and Metallicity Enrichment Histories}}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {13}, -year = {2018} -} -@article{Geometryeh, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(12).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ > 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright} 2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E. and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Raskutti, Greene, Murphy - 2014 - The stellar halos of massive elliptical galaxies. III. Kinematics at large radius.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{Massey2013, -abstract = {The first half of this paper explores the origin of systematic biases in the measurement of weak gravitational lensing. Compared to previous work, we expand the investigation of point spread function instability and fold in for the first time the effects of non-idealities in electronic imaging detectors and imperfect galaxy shape measurement algorithms. Together, these now explain the additive A(l) and multiplicative M(l) systematics typically reported in current lensing measurements. We find that overall performance is driven by a product of a telescope/camera's absolute performance, and our knowledge about its performance. The second half of this paper propagates any residual shear measurement biases through to their effect on cosmological parameter constraints. Fully exploiting the statistical power of Stage IV weak lensing surveys will require additive biasesA 1.8 × 10-12 and multiplicative biases M 4.0 × -3. These can be allocated between individual budgets in hardware, calibration data and software, using results from the first half of the paper. If instrumentation is stable and well calibrated, we find extant shear measurement software from Gravitational Lensing Accuracy Testing 2010 (GREAT10) already meet requirements on galaxies detected at signal-to-noise ratio = 40. Averaging over a population of galaxies with a realistic distribution of sizes, it also meets requirements for a 2D cosmic shear analysis from space. If used on fainter galaxies or for 3D cosmic shear tomography, existing algorithms would need calibration on simulations to avoid introducing bias at a level similar to the statistical error. Requirements on hardware and calibration data are discussed in more detail in a companion paper. Our analysis is intentionally general, but is specifically being used to drive the hardware and ground segment performance budget for the design of the European Space Agency's recently selected Euclid mission. {\textcopyright}2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1210.7690}, -author = {Massey, Richard and Hoekstra, Henk and Kitching, Thomas and Rhodes, Jason and Cropper, Mark and Amiaux, J{\'{e}}r{\^{o}}me and Harvey, David and Mellier, Yannick and Meneghetti, Massimo and Miller, Lance and Paulin-Henriksson, St{\'{e}}phane and Pires, Sandrine and Scaramella, Roberto and Schrabback, Tim}, -doi = {10.1093/mnras/sts371}, -eprint = {1210.7690}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Gravitational lensing: weak,Instrumentation: detectors,Methods: data analysis,Space vehicles: instruments,Telescopes}, -month = {feb}, -number = {1}, -pages = {661--678}, -title = {{Origins of weak lensing systematics, and requirements on future instrumentation (or knowledge of instrumentation)}}, -volume = {429}, -year = {2013} -} -@article{Naab2007, -abstract = {We describe high-resolution smoothed particle hydrodynamics (SPH) simulations of three approximately M* field galaxies starting from $\Lambda$CDM initial conditions. The simulations are made intentionally simple, and include photoionization, cooling of the intergalactic medium, and star formation, but not feedback from AGNs or supernovae. All of the galaxies undergo an initial burst of star formation at z$\sim$5, accompanied by the formation of a bubble of heated gas. Two out of three galaxies show early-type properties at present, whereas only one of them experienced a major merger. Heating from shocks and PdV work dominates over cooling so that for most of the gas the temperature is an increasing function of time. By z$\sim$1 a significant fraction of the final stellar system is in place and the spectral energy distribution resembles those of observed massive red galaxies. The galaxies have grown from z=1-->0 on average by 25% in mass and in size by gas-poor (dry) stellar mergers. By the present day the simulated galaxies are old ($\sim$10 Gyr), kinematically hot stellar systems surrounded by hot gaseous haloes. Stars dominate the mass of the galaxies up to $\sim$4 effective radii ($\sim$10 kpc). Kinematic and most photometric properties are in good agreement with those of observed elliptical galaxies. The galaxy with a major merger develops a counter-rotating core. Our simulations show that realistic intermediate-mass giant elliptical galaxies with plausible formation histories can be formed from $\Lambda$CDM initial conditions even without requiring recent major mergers or feedback from supernovae or AGNs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0512235}, -author = {Naab, Thorsten and Johansson, Peter H. and Ostriker, Jeremiah P. and Efstathiou, George}, -doi = {10.1086/510841}, -eprint = {0512235}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Naab et al. - 2007 - Formation of Early‐Type Galaxies from Cosmological Initial Conditions(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {710--720}, -primaryClass = {astro-ph}, -title = {{Formation of Early‐Type Galaxies from Cosmological Initial Conditions}}, -url = {http://stacks.iop.org/0004-637X/658/i=2/a=710}, -volume = {658}, -year = {2007} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as 'notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude ({\textless}50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 {\textless} G {\textless} 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G M and Prod'homme, T and Murray, N J and Crowley, C and Hopkinson, G and Brown, A G A and Kohley, R and Holland, A}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within {\$\sim${}}30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M sun and a factor of 3 at 107 M sun. The most massive subhalos with 1010 M sun survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://stacks.iop.org/0004-637X/709/i=2/a=1138?key=crossref.6ebb2a01dc7b45f1fa5c66089a37542b}, -volume = {709}, -year = {2010} -} -@article{Deason2011, -abstract = {We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the gimic suite of simulations. gimic consists of resimulations of five cosmologically representative regions from the Millennium Simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r∼ 0.1r200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r∼r200). Misalignments of {\textgreater}45° are seen in ∼30 per cent of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20 per cent of the satellite systems with 10 bright galaxies within r200 exhibit a polar spatial alignment with respect to the galaxy - an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction (∼10 per cent) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z= 0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation - the memory of their accretion history can remain intact to z= 0. Understanding the phase-space distribution of the z= 0 satellite population is key for studies that estimate the host halo mass from the line-of-sight velocities and projected positions of satellite galaxies. We quantify the effects of such systematics in estimates of the host halo mass from the satellite population. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A J and Mccarthy, I G and Font, A S and Evans, N W and Frenk, C S and Belokurov, V and Libeskind, N I and Crain, R A and Theuns, T}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, $M_{BH}$, that had been imaged at $3.6\sim\mu m$ with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between $M_{ BH}$ and the host spheroid (and galaxy) luminosity, $L_{sph}$ (and $L_{gal}$), and also stellar mass, $M_{*,sph}$. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have $M_{BH} < 10^7\simM_\odot$, and allows us to better investigate the poorly studied low-mass end of the $M_{BH} - M_{*,sph}$ correlation. The bulges of early-type galaxies follow $M_{BH} \propto M_{*,sph}^{1.04 \pm 0.10}$ and define a tight red sequence with intrinsic scatter $\epsilon = 0.43 \pm 0.06\simdex$ and a median $M_{BH}/M_{*,sph}$ ratio of $0.68 \pm 0.04\%$, i.e.$\sim$a $\pm 2\sigma$ range of 0.1-5%. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with $M_{BH} \propto M_{*,sph}^{2-3}$, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index $n<2$, argued by some to be pseudo-bulges, are not offset to lower $M_{BH}$ from the correlation defined by the current bulge sample with $n>2$; and iii) $L_{sph}$ and $L_{gal}$ correlate equally well with $M_{BH}$, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with $L_{ sph}$ is better than that with $L_{gal}$.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A. D. and Graham, Alister W. and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Savorgnan et al. - 2016 - Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M ,Sph Diagr(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Bentabol2016, -abstract = {We examine a sample of 1495 galaxies in the CANDELS fields to determine the evolution of two component galaxies, including bulges and discs, within massive galaxies at the epoch 1 {\textless}z {\textless}3 when the Hubble sequence forms. We fit all of our galaxies' light profiles with a single S{\$}\backslash{\$}'ersic fit, as well as with a combination of exponential and S{\$}\backslash{\$}'ersic profiles. The latter is done in order to describe a galaxy with an inner and an outer component, or bulge and disc component. We develop and use three classification methods (visual, F-test and the RFF) to separate our sample into 1-component galaxies (disc/spheroids-like galaxies) and 2-component galaxies (galaxies formed by an 'inner part' or bulge and an 'outer part' or disc). We then compare the results from using these three different ways to classify our galaxies. We find that the fraction of galaxies selected as 2-component galaxies increases on average 50 per cent from the lowest mass bin to the most massive galaxies, and decreases with redshift by a factor of four from z = 1 to z = 3. We find that single S{\$}\backslash{\$}'ersic 'disc-like' galaxies have the highest relative number densities at all redshifts, and that 2-component galaxies have the greatest increase and become at par with S{\$}\backslash{\$}'ersic discs by z = 1. We also find that the systems we classify as 2-component galaxies have an increase in the sizes of their outer components, or 'discs', by about a factor of three from z = 3 to z = 1.5, while the inner components or 'bulges' stay roughly the same size. This suggests that these systems are growing from the inside out, whilst the bulges or protobulges are in place early in the history of these galaxies. This is also seen to a lesser degree in the growth of single 'disc-like' galaxies vs. 'spheroid-like' galaxies over the same epoch.}, -archivePrefix = {arXiv}, -arxivId = {1606.07405}, -author = {Margalef-Bentabol, Berta and Conselice, Christopher J and Mortlock, Alice and Hartley, Will and Duncan, Kenneth and Ferguson, Harry C and Dekel, Avishai and Primack, Joel R}, -doi = {10.1093/mnras/stw1451}, -eprint = {1606.07405}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure}, -number = {3}, -pages = {1--21}, -title = {{The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z {\textless}3}}, -volume = {461}, -year = {2016} -} -@techreport{Cawley2001, -abstract = {The Charge Transfer Efficiency (CTE) Working Group at STScI was created as a forum to study and discuss the effects of CTE loss on HST CCDs. This report is the first publication detailing our progress. It represents the Institute's current (as of early 2001) understanding of the effects of CTE degradation due to radiation damage. We review the causes of CTE loss, present the results of monitoring of the WFPC2 and STIS CCDs and discuss the means by which future CCD instruments, ACS and WFC3 will address CTE. We also look at the scientific impacts of CTE degradation, presenting several examples from WFPC2 and STIS.}, -author = {Cawley, Laura and Goudfrooij, Paul and Whitmore, Brad and Stiavelli, M and Group, Working}, -booktitle = {Space Telescope WFC Instrument Science Report}, -keywords = {HST,Hubble Space Telescope,Space Telescope Science Institute,WFC3,Wide Field Camera 3}, -month = {apr}, -pages = {1--41}, -title = {{HST CCD Performance in the Second Decade : Charge Transfer Efficiency}}, -year = {2002} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. with the particletagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of $\sim$1900 massive dark matter haloes (1012-1014M⊙) from the Millennium II $\lambda$ cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of MilkyWay-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a S{\`{e}}rsic profile, the radial scale and amplitude of which vary systematically with halo mass (M200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M* and M200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z ≈ 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P. and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S. and White, Simon D.M.}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cooper et al. - 2013 - Galactic accretion and the outer structure of galaxies in the CDM model(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Inada2012, -abstract = {We present the final statistical sample of lensed quasars from the Sloan Digital Sky Survey (SDSS) Quasar Lens Search (SQLS). The well-defined statistical lens sample consists of 26 lensed quasars brighter than i = 19.1 and in the redshift range of 0.6 < z < 2.2 selected from 50,826 spectroscopically confirmed quasars in the SDSS Data Release 7 (DR7), where we restrict the image separation range to 1″ < $\theta$ < 20″ and the i-band magnitude differences in two images to be smaller than 1.25mag. The SDSS DR7 quasar catalog also contains 36additional lenses identified with various techniques. In addition to these lensed quasars, we have identified 81 pairs of quasars from follow-up spectroscopy, 26 of which are physically associated binary quasars. The statistical lens sample covers a wide range of image separations, redshifts, and magnitudes, and therefore is suitable for systematic studies of cosmological parameters and surveys of the structure and evolution of galaxies and quasars. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1203.1087}, -author = {Inada, Naohisa and Oguri, Masamune and Shin, Min Su and Kayo, Issha and Strauss, Michael A. and Morokuma, Tomoki and Rusu, Cristian E. and Fukugita, Masataka and Kochanek, Christopher S. and Richards, Gordon T. and Schneider, Donald P. and York, Donald G. and Bahcall, Neta A. and Frieman, Joshua A. and Hall, Patrick B. and White, Richard L.}, -doi = {10.1088/0004-6256/143/5/119}, -eprint = {1203.1087}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {cosmology: observations,gravitational lensing: strong,quasars: general}, -month = {may}, -number = {5}, -pages = {119}, -primaryClass = {astro-ph.CO}, -title = {{The Sloan Digital Sky Survey Quasar Lens Search. V. Final catalog from the seventh data release}}, -url = {http://stacks.iop.org/1538-3881/143/i=5/a=119%5Cnhttp://stacks.iop.org/1538-3881/143/i=5/a=119?key=crossref.528eb90f68b4962e086445b2ff987968}, -volume = {143}, -year = {2012} -} -@article{Planck2018, -abstract = {The European Space Agency's Planck satellite, which was dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013, producing deep, high-resolution, all-sky maps in nine frequency bands from 30 to 857GHz. This paper presents the cosmological legacy of Planck, which currently provides our strongest constraints on the parameters of the standard cosmological model and some of the tightest limits available on deviations from that model. The 6-parameter LCDM model continues to provide an excellent fit to the cosmic microwave background data at high and low redshift, describing the cosmological information in over a billion map pixels with just six parameters. With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the six parameters to better than 1% (simultaneously), with the best-determined parameter (theta_*) now known to 0.03%. We describe the multi-component sky as seen by Planck, the success of the LCDM model, and the connection to lower-redshift probes of structure formation. We also give a comprehensive summary of the major changes introduced in this 2018 release. The Planck data, alone and in combination with other probes, provide stringent constraints on our models of the early Universe and the large-scale structure within which all astrophysical objects form and evolve. We discuss some lessons learned from the Planck mission, and highlight areas ripe for further experimental advances.}, -archivePrefix = {arXiv}, -arxivId = {1807.06205}, -author = {Aghanim, N. and Akrami, Y. and Arroja, F. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Ballardini, M. and Banday, A. J. and Barreiro, R. B. and Bartolo, N. and Basak, S. and Battye, R. and Benabed, K. and Bernard, J.-P. and Bersanelli, M. and Bielewicz, P. and Bock, J. J. and Bond, J. R.}, -doi = {10.1051/0004-6361/201833880}, -eprint = {1807.06205}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Aghanim et al. - 2019 - Planck 2018 results. I. Overview and the cosmological legacy of Planck.pdf:pdf}, -issn = {0004-6361}, -journal = {A\&A}, -keywords = {Planck2018,cosmic background radiation,cosmology,observations,surveys,theory}, -mendeley-tags = {Planck2018}, -title = {{Planck 2018 results. I. Overview and the cosmological legacy of Planck}}, -year = {2019} -} -@article{Thater2019, -abstract = {We present our ongoing work of using two independent tracers to estimate the supermassive black hole mass in the nearby early-type galaxy NGC 6958; namely integrated stellar and molecular gas kinematics. We used data from the Atacama Large Millimeter/submillimeter Array (ALMA), and the adaptive-optics assisted Multi-Unit Spectroscopic Explorer (MUSE) and constructed state-of-the-art dynamical models. The different methods provide black hole masses of (2.89±2.05)×108M{\^{a}}S™ from stellar kinematics and (1.35±0.09)×108M{\^{a}}S™ from molecular gas kinematics which are consistent within their 3$\sigma$ uncertainties. Compared to recent MBH-$\sigma$e scaling relations, we derive a slightly over-massive black hole. Our results also confirm previous findings that gas-based methods tend to provide lower black hole masses than stellar-based methods. More black hole mass measurements and an extensive analysis of the method-dependent systematics are needed in the future to understand this noticeable discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1911.11491}, -author = {Thater, Sabine and Krajnovi{\'{c}}, Davor and Nguyen, Dieu D. and Iguchi, Satoru and Weilbacher, Peter M.}, -doi = {10.1017/S1743921319008445}, -eprint = {1911.11491}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Thater et al. - 2019 - Testing the robustness of black hole mass measurements with ALMA and MUSE.pdf:pdf}, -isbn = {0000000000000}, -issn = {17439221}, -journal = {Proceedings of the International Astronomical Union}, -keywords = {galaxies: individual (NGC6958),galaxies: kinematics and dynamics,galaxies: nuclei}, -number = {S353}, -pages = {199--202}, -title = {{Testing the robustness of black hole mass measurements with ALMA and MUSE}}, -url = {http://arxiv.org/abs/1911.11491}, -volume = {14}, -year = {2019} -} -@article{Report2011, -abstract = {Euclid is a space-based survey mission from the European Space Agency designed to understand the origin of the Universe's accelerating expansion. It will use cosmological probes to investigate the nature of dark energy, dark matter and gravity by tracking their observational signatures on the geometry of the universe and on the cosmic history of structure formation. The mission is optimised for two independent primary cosmological probes: Weak gravitational Lensing (WL) and Baryonic Acoustic Oscillations (BAO). The Euclid payload consists of a 1.2 m Korsch telescope designed to provide a large field of view. It carries two instruments with a common field-of-view of {\$\sim${}}0.54 deg2: the visual imager (VIS) and the near infrared instrument (NISP) which contains a slitless spectrometer and a three bands photometer. The Euclid wide survey will cover 15,000 deg2 of the extragalactic sky and is complemented by two 20 deg2 deep fields. For WL, Euclid measures the shapes of 30-40 resolved galaxies per arcmin2 in one broad visible R+I+Z band (550-920 nm). The photometric redshifts for these galaxies reach a precision of dz/(1+z) {\textless}0.05. They are derived from three additional Euclid NIR bands (Y, J, H in the range 0.92-2.0 micron), complemented by ground based photometry in visible bands derived from public data or through engaged collaborations. The BAO are determined from a spectroscopic survey with a redshift accuracy dz/(1+z) =0.001. The slitless spectrometer, with spectral resolution {\$\sim${}}250, predominantly detects Ha emission line galaxies. Euclid is a Medium Class mission of the ESA Cosmic Vision 2015-2025 programme, with a foreseen launch date in 2019. This report (also known as the Euclid Red Book) describes the outcome of the Phase A study.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1110.3193}, -author = {Flacher, David and Harari-Kermadec, Hugo}, -doi = {10.1080/09645292.2011.561630}, -eprint = {1110.3193}, -issn = {09645292}, -journal = {Education Economics}, -keywords = {asymmetric information,equity,higher education,social bias,tuition fees}, -number = {2}, -pages = {191--210}, -primaryClass = {astro-ph.CO}, -title = {{Tuition fees, self-esteem and social heterogeneity}}, -volume = {21}, -year = {2013} -} -@article{Jin2017, -abstract = {We report the results from a recent 133 ks XMM-Newton observation of a highly super- Eddington narrow-line Type-1 quasi-stellar object RX J0439.6-5311. This source has one of the steepest active galactic nuclei hard X-ray slopes, in addition to a prominent and smooth soft X-ray excess. Strong variations are found throughout the 0.3-10 keV energy range on all time-scales covered by the observation, with the soft excess mainly showing low-frequency (LF) variations below 0.1 mHz while the hard X-rays show stronger variability at higher frequencies. We perform a full set of spectral-timing analysis on the X-ray data, including a simultaneous modelling of the time-averaged spectra, frequency-dependent root-mean-square and covariance spectra, lag-frequency and lag-energy spectra. Especially, we find a significant time-lag signal in the LF band, which indicates that the soft X-rays lead the hard by $\sim$4 ks, with a broad continuum-like profile in the lag spectrum. Our analysis strongly supports the model where the soft X-ray excess is dominated by a separate low temperature, optically thick Comptonization component rather than relativistic reflection or a jet. This soft X-ray emitting region is several tens or hundreds of Rg away from the hot corona emitting hard X-rays, and is probably associated with a geometrically thick ('puffed-up') inner disc region.}, -archivePrefix = {arXiv}, -arxivId = {1703.07118}, -author = {Jin, Chichuan and Done, Chris and Ward, Martin}, -doi = {10.1093/mnras/stx718}, -eprint = {1703.07118}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Jin, Done, Ward - 2017 - Super-Eddington QSO RX J0439.6-5311 - I. Origin of the soft X-ray excess and structure of the inner accretion f.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Accretion,Accretion discs,Galaxies: active,Galaxies: nuclei}, -number = {3}, -pages = {3663--3681}, -title = {{Super-Eddington QSO RX J0439.6-5311 - I. Origin of the soft X-ray excess and structure of the inner accretion flow}}, -url = {http://arxiv.org/abs/1703.07118%0Ahttp://dx.doi.org/10.1093/mnras/stx718}, -volume = {468}, -year = {2017} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified {\$\sim${}}17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M {\textless}10{\^{}}9 M*), low-metallicity (Z{\$\sim${}}1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He $\backslash$ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A and Erb, Dawn K and Auger, Matthew W and Pettini, Max and Brammer, Gabriel B}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -isbn = {0004-637X}, -issn = {15384357}, -pages = {1--28}, -title = {{A Window On The Earliest Star Formation: Extreme Photoionization Conditions of a High-Ionization, Low-Metallicity Lensed Galaxy at z{\$\sim${}}2}}, -url = {http://arxiv.org/abs/1803.02340}, -year = {2018} -} -@article{Hopkins2012, -abstract = {Feedback from massive stars is believed to play a critical role in driving galactic super-winds that enrich the IGM and shape the galaxy mass function and mass-metallicity relation. In previous papers, we introduced new numerical methods for implementing stellar feedback on sub-GMC through galactic scales in galaxy simulations. This includes radiation pressure (UV through IR), SNe (Type-I {\&} II), stellar winds ('fast' O-star through 'slow' AGB winds), and HII photoionization. Here, we show that these feedback mechanisms drive galactic winds with outflow rates as high as {\$\sim${}}10-20 times the galaxy SFR. The mass-loading efficiency (wind mass loss rate divided by SFR) scales inversely with circular velocity, consistent with momentum-conservation expectations. We study the contributions of each feedback mechanism to galactic winds in a range of galaxy models, from SMC-like dwarfs {\&} MW-analogues to z{\$\sim${}}2 clumpy disks. In massive, gas-rich systems (local starbursts and high-z galaxies), radiation pressure dominates the wind generation. For MW-like spirals and dwarf galaxies the gas densities are much lower, and shock-heated gas from SNe and stellar winds dominates production of large-scale outflows. In all models, however, winds have a multi-phase structure that depends on interactions between multiple feedback mechanisms operating on different spatial {\&} time scales: any single mechanism fails to reproduce the winds observed. We provide fitting functions for wind mass-loading and velocities as a function of galaxy properties, for use in cosmological simulations and semi-analytic models. These differ from typically-adopted formulae with explicit dependence on gas surface density that can be very important in both low-density dwarf galaxies and high-density gas-rich galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1110.4638}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2012.20593.x}, -eprint = {1110.4638}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Stars: formation}, -number = {4}, -pages = {3522--3537}, -title = {{Stellar feedback in galaxies and the origin of galaxy-scale winds}}, -volume = {421}, -year = {2012} -} -@article{Zentner2005, -abstract = {We present a study of the spatial distribution of subhalos in galactic dark matter halos using dissipationless cosmological simulations of the concordance LCDM model. We find that subhalos are distributed anisotropically and are preferentially located along the major axes of the triaxial mass distributions of their hosts. The Kolmogorov-Smirnov probability for drawing our simulated subhalo sample from an isotropic distribution is P{\_}KS {\$}\backslash{\$}simeq 1.5 {\$}\backslash{\$}times 10{\^{}}{\{}-4{\}}. An isotropic distribution of subhalos is thus not the correct null hypothesis for testing the CDM paradigm. The nearly planar distribution of observed Milky Way (MW) satellites is marginally consistent (probability {\$}\backslash{\$}simeq 0.02) with being drawn randomly from the subhalo distribution in our simulations. Furthermore, if we select the subhalos likely to be luminous, we find a distribution that is consistent with the observed MW satellites. In fact, we show that subsamples of the subhalo population with a centrally-concentrated radial distribution, similar to that of the MW dwarfs, typically exhibit a comparable degree of planarity. We explore the origin of the observed subhalo anisotropy and conclude that it is likely due to (1) preferential accretion of subhalos along filaments, often closely aligned with the major axis of the host halo, and (2) evolution of satellite orbits within the prolate, triaxial potentials typical of CDM halos. Agreement between predictions and observations requires the major axis of the outer dark matter halo of the Milky Way to be nearly perpendicular to the disk. We discuss possible observational tests of such disk-halo alignment with current large galaxy surveys.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0502496}, -author = {Zentner, Andrew R and Kravtsov, Andrey V and Gnedin, Oleg Y and Klypin, Anatoly A}, -doi = {10.1086/431355}, -eprint = {0502496}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {219--232}, -primaryClass = {astro-ph}, -title = {{The Anisotropic Distribution of Galactic Satellites}}, -url = {http://arxiv.org/abs/astro-ph/0502496%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/431355}, -volume = {629}, -year = {2005} -} -@article{Birrer2015a, -abstract = {We present extended modelling of the strong lens system RXJ1131-1231 with archival data in two HST bands in combination with existing line-of-sight contribution and velocity dispersion estimates. Our focus is on source size and its influence on time-delay cosmography. We therefore examine the impact of mass-sheet degeneracy and especially the degeneracy pointed out by Schneider & Sluse (2013) [1] using the source reconstruction scale. We also extend on previous work by further exploring the effects of priors on the kinematics of the lens and the external convergence in the environment of the lensing system. Our results coming from RXJ1131-1231 are given in a simple analytic form so that they can be easily combined with constraints coming from other cosmological probes. We find that the choice of priors on lens model parameters and source size are subdominant for the statistical errors for H0 measurements of this systems. The choice of prior for the source is sub-dominant at present (2% uncertainty on H0) but may be relevant for future studies. More importantly, we find that the priors on the kinematic anisotropy of the lens galaxy have a significant impact on our cosmological inference. When incorporating all the above modeling uncertainties, we find H0 = 86.6+6.8-6.9 km s-1 Mpc-1, when using kinematic priors similar to other studies. When we use a different kinematic prior motivated by Barnab{\`{e}} et al. (2012) [2] but covering the same anisotropic range, we find H0 = 74.5+8.0-7.8 km s-1 Mpc-1. This means that the choice of kinematic modeling and priors have a significant impact on cosmographic inferences. The way forward is either to get better velocity dispersion measures which would down weight the impact of the priors or to construct physically motivated priors for the velocity dispersion model.}, -archivePrefix = {arXiv}, -arxivId = {1511.03662}, -author = {Birrer, Simon and Amara, Adam and Refregier, Alexandre}, -doi = {10.1088/1475-7516/2016/08/020}, -eprint = {1511.03662}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {dark energy experiments,gravitational lensing}, -number = {8}, -pages = {020--020}, -title = {{The mass-sheet degeneracy and time-delay cosmography: Analysis of the strong lens RXJ1131-1231}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2015arXiv151103662B&link_type=ABSTRACT%255Cnpapers://dcc533b5-8613-47b7-b88c-2b0c0d39c33f/Paper/p11560%255Cnhttp://stacks.iop.org/1475-7516/2016/i=08/a=020?key=crossref.b617a3265830727594854b2ee1144}, -volume = {2016}, -year = {2016} -} -@article{Chevance2012, -abstract = {Recent deep Hubble Space Telescope WFC3 imaging suggests that a majority of compact quiescent massive galaxies at z 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and S{\'{e}}rsic index distributions obtained from two-dimensional structural fits to 40, 000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of S{\'{e}}rsic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. {\textcopyright} 2012. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1206.3579}, -author = {Chevance, M{\'{e}}lanie and Weijmans, Anne Marie and Damjanov, Ivana and Abraham, Roberto G. and Simard, Luc and {Van Den Bergh}, Sidney and Caris, Evelyn and Glazebrook, Karl}, -doi = {10.1088/2041-8205/754/2/L24}, -eprint = {1206.3579}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Chevance et al. - 2012 - On the shapes and structures of high-redshift compact galaxies.pdf:pdf}, -isbn = {9781617289422}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: statistics,galaxies: structure}, -number = {2}, -title = {{On the shapes and structures of high-redshift compact galaxies}}, -volume = {754}, -year = {2012} -} -@article{Hlavacek-Larrondo2012, -abstract = {We investigate where brightest cluster galaxies (BCGs) sit on the Fundamental Plane of black hole (BH) activity, an established relation between the X-ray luminosity, the radio luminosity and the mass of a BH. Our sample mostly consists of BCGs that lie at the centres of massive, strong cooling flow clusters, therefore requiring extreme mechanical feedback from their central active galactic nucleus (AGN) to offset cooling of the intracluster plasma (L mech>10 44 -10 45 ergs -1). Based on the BH masses derived from the and M BH - M K correlations, we find that all of our objects are offset from the plane such that they appear to be less massive than predicted from their X-ray and radio luminosities (to more than a 99per cent confidence level). For these objects to be consistent with the Fundamental Plane, the and M BH - M K correlations therefore seem to underestimate the BH masses of BCGs, on average by a factor of 10. Our results suggest that the standard relationships between BH mass and host galaxy properties no longer hold for these extreme galaxies. Furthermore, our results imply that if these BHs follow the Fundamental Plane, then many of those that lie in massive, strong cool core clusters must be ultramassive with M BH > 10 10M ⊙. This rivals the largest BH masses known and has important ramifications for our understanding of the formation and evolution of BHs. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -author = {Hlavacek-Larrondo, J. and Fabian, A. C. and Edge, A. C. and Hogan, M. T.}, -doi = {10.1111/j.1365-2966.2012.21187.x}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Hlavacak2021SMBHsinBCGClusters.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Accretion,Black hole physics,Galaxies: active,Galaxies: clusters: general,Galaxies: jets,X-rays: galaxies: clusters,accretion discs}, -number = {1}, -pages = {224--231}, -title = {{On the hunt for ultramassive black holes in brightest cluster galaxies}}, -volume = {424}, -year = {2012} -} -@article{Siverd2009, -abstract = {We identify, categorize, and quantify alignment effects among host and satellite galaxies using a spectroscopically-confirmed, low-redshift (z{\textless}0.23) galaxy sample from the Sloan Digital Sky Survey Data Release 6. Consistent with other recent findings, we find that satellite galaxies (SGs) of red, centrally concentrated (elliptical) host galaxies (HGs) with radial velocity separation |Delta{\_}V|{\textless}600 km/s preferentially reside near the projected major axes of their HGs. Among these, this preference is strongest for highly concentrated, red SGs. We find that fractional anisotropy increases with decreasing $\backslash$Delta{\_}V and Delta{\_}R and is nearly 40{\%} greater among the closest SGs (Delta{\_}R{\textless}250 kpc/h) relative to more distant (Delta{\_}R{\textgreater}500 kpc/h) SGs. For highly concentrated SGs at small ({\textless}300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to {\textless}15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby ({\textless}40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ({\$\sim${}}3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R J and Ryden, B S and Gaudi, B S}, -eprint = {0903.2264}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@article{Eisenstein2001, -abstract = {We describe the target selection and resulting properties of a spectroscopic sample of luminous, red galaxies (LRG) from the imaging data of the Sloan Digital Sky Survey (SDSS). These galaxies are selected on the basis of color and magnitude to yield a sample of luminous, intrinsically red galaxies that extends fainter and further than the main flux-limited portion of the SDSS galaxy spectroscopic sample. The sample is designed to impose a passively-evolving luminosity and rest-frame color cut to a redshift of 0.38. Additional, yet more luminous, red galaxies are included to a redshift of 0.5. Approximately 12 of these galaxies per square degree are targeted for spectroscopy, so the sample will number over 100,000 with the full survey. SDSS commissioning data indicate that the algorithm efficiently selects luminous (M_g=-21.4), red galaxies, that the spectroscopic success rate is very high, and that the resulting set of galaxies is approximately volume-limited out to z=0.38. When the SDSS is complete, the LRG spectroscopic sample will fill over 1h^-3 Gpc^3 with an approximately homogeneous population of galaxies and will therefore be well suited to studies of large-scale structure and clusters out to z=0.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108153}, -author = {Eisenstein, Daniel J. and Annis, James and Gunn, James E. and Szalay, Alexander S. and Connolly, Andrew J. and Nichol, R. C. and Bahcall, Neta A. and Bernardi, Mariangela and Burles, Scott and Castander, Francisco J. and Fukugita, Masataka and Hogg, David W. and Ivezi{\'{c}}, {\v{Z}}eljko and Knapp, G. R. and Lupton, Robert H. and Narayanan, Vijay and Postman, Marc and Reichart, Daniel E. and Richmond, Michael and Schneider, Donald P. and Schlegel, David J. and Strauss, Michael A. and SubbaRao, Mark and Tucker, Douglas L. and {Vanden Berk}, Daniel and Vogeley, Michael S. and Weinberg, David H. and Yanny, Brian}, -doi = {10.1086/323717}, -eprint = {0108153}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Eisenstein et al. - 2001 - Spectroscopic Target Selection for the Sloan Digital Sky Survey The Luminous Red Galaxy Sample.pdf:pdf}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2267--2280}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample}}, -url = {http://arxiv.org/abs/astro-ph/0108153%0Ahttp://dx.doi.org/10.1086/323717}, -volume = {122}, -year = {2001} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ({\$}z = 1.489{\$}), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5{\$}+{\$}2223 ({\$}z = 0.542{\$}), published by Grillo et al. (2016), and explore different {\$}\backslashLambda{\$}CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of {\$}H{\_}{\{}0{\}}{\$} and {\$}\backslashOmega{\_}{\{}\backslashrm m{\}}{\$} with relative (1{\$}\backslashsigma{\$}) statistical errors of, respectively, 6{\%} (7{\%}) and 31{\%} (26{\%}) in flat (general) cosmological models, assuming a conservative 3{\%} uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of {\$}H{\_}{\{}0{\}}{\$}, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C and Rosati, P and Suyu, S H and Balestra, I and Caminha, G B and Halkola, A and Kelly, P L and Lombardi, M and Mercurio, A and Rodney, S A and Treu, T}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -issn = {15384357}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -title = {{Measuring the value of the Hubble constant "$\backslash$`a la Refsdal"}}, -url = {http://arxiv.org/abs/1802.01584}, -year = {2018} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M_*/M_sun) > 11.5 (M_K < -25.3 mag) and distance D < 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38\pm6% down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80\pm10% and 28\pm6%, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R_e), and the gas morphologies are diverse, with 17/28 = 61\pm9% being centrally concentrated, 8/28 = 29\pm9% exhibiting clear rotation out to several kpc, and 3/28 = 11\pm6% being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly $\sim$10^5M_sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E. and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A. and Blakeslee, John P. and Goulding, Andy D. and McConnell, Nicholas J. and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pandya et al. - 2017 - The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Ear.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{YuSa2013, -abstract = {Charged Coupled Devices (CCDs) have been successfully used in several low energy X-ray astronomical satellites over the past two decades. Their high energy resolution and high spatial resolution make them a perfect tool for low energy astronomy, such as observing the formation of galaxy clusters and the environment around black holes. The Low Energy X-ray Telescope (LE) group is developing a Swept Charge Device (SCD) for the Hard X-ray Modulation Telescope (HXMT) satellite. A SCD is a special low energy X-ray CCD, which can be read out a thousand times faster than traditional CCDs, simultaneously keeping excellent energy resolution. A test method for measuring the charge transfer efficiency (CTE) of a prototype SCD has been set up. Studies of the charge transfer inefficiency (CTI) with a proton-irradiated SCD have been performed at a range of operating temperatures. The SCD is irradiated by 3 × 10 8cm-2 10 MeV protons. {\textcopyright} 2014 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1308.1698}, -author = {Wang, Yu Sa and Yang, Yan Ji and Chen, Yong and Liu, Xiao Yan and Cui, Wei Wei and Xu, Yu Peng and Li, Cheng Kui and Li, Mao Shun and Han, Da Wei and Chen, Tian Xiang and Huo, Jia and Wang, Juan and Li, Wei and Hu, Wei and Zhang, Yi and Lu, Bo and Yin, Guo He and Zhu, Yue and Zhang, Zi Liang}, -doi = {10.1088/1674-1137/38/6/066001}, -eprint = {1308.1698}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2014 - Measurements of charge transfer efficiency in a proton-irradiated swept charge device(2).pdf:pdf}, -issn = {16741137}, -journal = {Chinese Physics C}, -keywords = {CCD,CTE,CTI,HXMT,LE,SCD,proton-irradiated}, -number = {6}, -pages = {1--5}, -title = {{Measurements of charge transfer efficiency in a proton-irradiated swept charge device}}, -url = {http://arxiv.org/abs/1308.1698}, -volume = {38}, -year = {2014} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T < 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim & Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H. and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{VanDeVen2009, -abstract = {Studies of strong gravitational lensing in current and upcoming wide and deep photometric surveys, and of stellar kinematics from (integral-field) spectroscopy at increasing redshifts, promise to provide valuable constraints on galaxy density profiles and shapes. However, both methods are affected by various selection and modelling biases, which we aim to investigate in a consistent way. In this first paper in a series, we develop a flexible but efficient pipeline to simulate lensing by realistic galaxy models. These galaxy models have separate stellar and dark matter components, each with a range of density profiles and shapes representative of early-type, central galaxies without significant contributions from other nearby galaxies. We use Fourier methods to calculate the lensing properties of galaxies with arbitrary surface density distributions, and Monte Carlo methods to compute lensing statistics such as point-source lensing cross-sections. Incorporating a variety of magnification bias modes lets us examine different survey limitations in image resolution and flux. We rigorously test the numerical methods for systematic errors and sensitivity to basic assumptions. We also determine the minimum number of viewing angles that must be sampled in order to recover accurate orientation-averaged lensing quantities. We find that for a range of non-isothermal stellar and dark matter density profiles typical of elliptical galaxies, the combined density profile and corresponding lensing properties are surprisingly close to isothermal around the Einstein radius. The converse implication is that constraints from strong lensing and/or stellar kinematics, which are indeed consistent with isothermal models near the Einstein radius, cannot trivially be extrapolated to smaller and larger radii. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:0808.2493v1}, -author = {{Van De Ven}, Glenn and Mandelbaum, Rachel and Keeton, Charles R.}, -doi = {10.1111/j.1365-2966.2009.15167.x}, -eprint = {arXiv:0808.2493v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: kinematics and dynamics,Galaxies: photometry,Galaxies: structure,Gravitational lensing,Methods: numerical,Stellar dynamics}, -number = {2}, -pages = {607--634}, -title = {{Galaxy density profiles and shapes - I. Simulation pipeline for lensing by realistic galaxy models}}, -volume = {398}, -year = {2009} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of {\$\sim${}}1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Dutton2014, -abstract = {Recent studies have shown that massive elliptical galaxies have total mass density profiles within an effective radius that can be approximated as . $\rho$tot ∝ r -$\gamma$' with mean slope 〈$\gamma$'〉 = 2.08 ± 0.03 and scatter $\sigma$$\gamma$' =0.16 ± 0.02. The small scatter of the slope (known as the bulge-halo conspiracy) is not generic in $\Lambda$ cold dark matter ($\Lambda$CDM) based models and therefore contains information about the galaxy formation process. We compute the distribution of $\gamma$' for $\Lambda$CDM-based models that reproduce the observed correlations between stellar mass, velocity dispersion, and effective radius of early-type galaxies in the Sloan Digital Sky Survey. The models have a range of stellar initial mass functions (IMFs) and dark halo responses to galaxy formation. The observed distribution of $\gamma$' is well reproduced by a model with cosmologically motivated but uncontracted dark matter haloes, and a Salpeter-type IMF. Other models are on average ruled out by the data, even though they may happen in individual cases. Models with adiabatic halo contraction (and lighter IMFs) predict too small values of $\gamma$'. Models with halo expansion, or mass-follows-light predict too high values of $\gamma$'. Our study shows that the non-homologous structure of massive early-type galaxies can be precisely reproduced by $\Lambda$CDM models if the IMF is not universal and if mechanisms, such as feedback from active galactic nuclei, or dynamical friction, effectively on average counterbalance the contraction of the halo expected as a result of baryonic cooling. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.4389}, -author = {Dutton, Aaron A. and Treu, Tommaso}, -doi = {10.1093/mnras/stt2489}, -eprint = {1303.4389}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular, cD,Galaxies: formation,Galaxies: fundamental parameters,Stars: luminosity function, mass function}, -number = {4}, -pages = {3594--3602}, -title = {{The bulge-halo conspiracy in massive elliptical galaxies: Implications for the stellar initial mass function and halo response to baryonic processes}}, -volume = {438}, -year = {2014} -} -@article{Shajib2019, -abstract = {We demonstrate an efficient method to compute the strong-gravitational-lensing deflection angle and magnification for any elliptical surface density profile. This method solves a numerical hurdle in lens modelling that has lacked a general solution for nearly three decades. The hurdle emerges because it is prohibitive to derive analytic expressions of the lensing quantities for most elliptical mass profiles. In our method, we first decompose an elliptical mass profile into concentric Gaussian components. We introduce an integral transform that provides us with a fast and accurate algorithm for this Gaussian decomposition. We derive analytic expressions of the lensing quantities for a Gaussian component. As a result, we can compute these quantities for the total mass profile by adding up the contributions from the individual components. This lensing analysis self-consistently completes the kinematic description in terms of Gaussian components presented by Cappellari (2008). Our method is general without extra computational burden unlike other methods currently in use.}, -archivePrefix = {arXiv}, -arxivId = {1906.08263}, -author = {Shajib, Anowar J.}, -doi = {10.1093/mnras/stz1796}, -eprint = {1906.08263}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Shajib2020GaussianDecomp].pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dynamics,Galaxies: kinematics,Gravitational lensing: strong,Methods: analytical,Methods: data analysis,Methods: numerical}, -number = {1}, -pages = {1387--1400}, -title = {{Unified lensing and kinematic analysis for any elliptical mass profile}}, -volume = {14}, -year = {2019} -} -@article{Fergus2014, -abstract = {High dynamic range imagers aim to block or eliminate light from a very bright primary star in order to make it possible to detect and measure far fainter companions; in real systems, a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronagraph. The model uses principal components analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles, but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of the order of a percent of the brightness of the speckles, or up to 10-7 times the brightness of the primary star. This outperforms existing methods by a factor of two to three and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W. and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Fergus et al. - 2014 - S4 A spatial-spectral model for speckle suppression.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Zehavi2017, -abstract = {We study the dependence of the galaxy content of dark matter halos on large-scale environment and halo formation time using semi-analytic galaxy models applied to the Millennium simulation. We analyze subsamples of halos at the extremes of these distributions and measure the occupation functions for the galaxies they host. We find distinct differences in these occupation functions. The main effect with environment is that central galaxies (and in one model also the satellites) in denser regions start populating lower-mass halos. A similar, but significantly stronger, trend exists with halo age, where early-forming halos are more likely to host central galaxies at lower halo mass. We discuss the origin of these trends and the connection to the stellar mass -- halo mass relation. We find that, at fixed halo mass, older halos and to some extent also halos in dense environments tend to host more massive galaxies. Additionally, we see a reverse trend for the satellite galaxies occupation where early-forming halos have fewer satellites, likely due to having more time for them to merge with the central galaxy. We describe these occupancy variations also in terms of the changes in the occupation function parameters, which can aid in constructing realistic mock galaxy catalogs. Finally, we study the corresponding galaxy auto- and cross-correlation functions of the different samples and elucidate the impact of assembly bias on galaxy clustering. Our results can inform theoretical models of assembly bias and attempts to detect it in the real universe.}, -archivePrefix = {arXiv}, -arxivId = {1706.07871}, -author = {Zehavi, Idit and Contreras, Sergio and Padilla, Nelson and Smith, Nicholas J and Baugh, Carlton M and Norberg, Peder}, -doi = {10.3847/1538-4357/aaa54a}, -eprint = {1706.07871}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {clustering,cosmology,evolution,galaxies,halos,large-scale structure of universe,statistics,theory}, -number = {1}, -pages = {84}, -title = {{The Impact of Assembly Bias on the Galaxy Content of Dark Matter Halos}}, -url = {http://arxiv.org/abs/1706.07871%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaa54a}, -volume = {853}, -year = {2018} -} -@article{Yang2006, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd, but inconsistent with several previous studies who detected a preferential minor-axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Nightingale2015, -abstract = {We present a new pixelized method for the inversion of gravitationally lensed extended source images which we term adaptive semi-linear inversion (SLI). At the heart of the method is an h-means clustering algorithm which is used to derive a source plane pixelization that adapts to the lens model magnification. The distinguishing feature of adaptive SLI is that every pixelization is derived from a random initialization, ensuring that data discretization is performed in a completely different and unique way for every lens model parameter set. We compare standard SLI on a fixed source pixel grid with the new method and demonstrate the shortcomings of the former when modelling singular power-law ellipsoid (SPLE) lens profiles. In particular, we demonstrate the superior reliability and efficiency of adaptive SLI which, by design, fixes the number of degrees of freedom (NDOF) of the optimization and thereby removes biases present with other methods that allow the NDOF to vary. In addition, we highlight the importance of data discretization in pixel-based inversion methods, showing that adaptive SLI averages over significant systematics that are present when a fixed source pixel grid is used. In the case of the SPLE lens profile, we show how the method successfully samples its highly degenerate posterior probability distribution function with a single nonlinear search. The robustness of adaptive SLI provides a firm foundation for the development of a strong lens modelling pipeline, which will become necessary in the short-term future to cope with the increasing rate of discovery of new strong lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1412.7436}, -author = {Nightingale, J. W. and Dye, S.}, -doi = {10.1093/mnras/stv1455}, -eprint = {1412.7436}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: evolution,Galaxies: structure,Methods: observational}, -month = {sep}, -number = {3}, -pages = {2940--2959}, -title = {{Adaptive semi-linear inversion of strong gravitational lens imaging}}, -volume = {452}, -year = {2015} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L. Gabriel and Arg{\"{u}}elles, C. R. and Perlick, Volker and Rueda, J. A. and Ruffini, R.}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/G{\'{o}}mez et al. - 2016 - Strong lensing by fermionic dark matter in galaxies(2).pdf:pdf}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Tan2024, -abstract = {The mass distribution in massive elliptical galaxies encodes their evolutionary history, thus providing an avenue to constrain the baryonic astrophysics in their evolution. The power-law assumption for the radial mass profile in ellipticals has been sufficient to describe several observables to the noise level, including strong lensing and stellar dynamics. In this paper, we quantitatively constrained any deviation, or the lack thereof, from the power-law mass profile in massive ellipticals through joint lensing-dynamics analysis of a large statistical sample with 77 galaxy-galaxy lens systems. We performed an improved and uniform lens modelling of these systems from archival Hubble Space Telescope imaging using the automated lens modelling pipeline dolphin. We combined the lens model posteriors with the stellar dynamics to constrain the deviation from the power law after accounting for the line-of-sight lensing effects, a first for analyses on galaxy-galaxy lenses. We find that the Sloan Lens ACS Survey lens galaxies with a mean redshift of 0.2 are consistent with the power-law profile within 1.1$\sigma$ (2.8$\sigma$) and the Strong Lensing Legacy Survey lens galaxies with a mean redshift of 0.6 are consistent within 0.8$\sigma$ (2.1$\sigma$), for a spatially constant (Osipkov-Merritt) stellar anisotropy profile. We adopted the spatially constant anisotropy profile as our baseline choice based on previous dynamical observables of local ellipticals. However, spatially resolved stellar kinematics of lens galaxies are necessary to differentiate between the two anisotropy models. Future studies will use our lens models to constrain the mass distribution individually in the dark matter and baryonic components.}, -archivePrefix = {arXiv}, -arxivId = {2311.09307}, -author = {Tan, Chin Yi and Shajib, Anowar J. and Birrer, Simon and Sonnenfeld, Alessandro and Treu, Tommaso and Wells, Patrick and Williams, Devon and Buckley-Geer, Elizabeth J. and Drlica-Wagner, Alex and Frieman, Joshua}, -doi = {10.1093/mnras/stae884}, -eprint = {2311.09307}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Tan2024StrongLensSlope.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cD,galaxies: elliptical and lenticular,gravitational lensing: strong}, -number = {2}, -pages = {1474--1505}, -title = {{Project Dinos I: A joint lensing-dynamics constraint on the deviation from the power law in the mass profile of massive ellipticals}}, -volume = {530}, -year = {2024} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Distribution of Satellite Galaxies in a Lambda-CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2005} -} -@article{Haussler2013, -abstract = {In this paper, we demonstrate a new method for fitting galaxy profiles which makes use of the full multiwavelength data provided by modern large optical-near-infrared imaging surveys. We present a new version of GALAPAGOS, which utilizes a recently developed multiwavelength version of GALFIT, and enables the automated measurement of wavelength-dependent S{\'{e}}rsic profile parameters for very large samples of galaxies. Our newtechnique is extensively tested to assess the reliability of both pieces of software, GALFIT and GALAPAGOS on both real ugrizY JHK imaging data from the Galaxy And Mass Assembly survey and simulated data made to the same specifications. We find that fitting galaxy light profiles with multiwavelength data increases the stability and accuracy of the measured parameters, and hence produces more complete and meaningful multiwavelength photometry than has been available previously. The improvement is particularly significant for magnitudes in low-S/N bands and for structural parameters like half-light radius re and S{\'{e}}rsic index n for which a prior is used by constraining these parameters to a polynomial as a function of wavelength. This allows the fitting routines to push the magnitude of galaxies for which sensible values can be derived to fainter limits. The technique utilizes a smooth transition of galaxy parameters with wavelength, creating more physically meaningful transitions than single-band fitting and allows accurate interpolation between passbands, perfect for derivation of rest-frame values. {\textcopyright} 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1212.3332}, -author = {H{\"{a}}u{\ss}ler, Boris and Bamford, Steven P. and Vika, Marina and Rojas, Alex L. and Barden, Marco and Kelvin, Lee S. and Alpaslan, Mehmet and Robotham, Aaron S.G. and Driver, Simon P. and Baldry, I. K. and Brough, Sarah and Hopkins, Andrew M. and Liske, Jochen and Nichol, Robert C. and Popescu, Cristina C. and Tuffs, Richard J.}, -doi = {10.1093/mnras/sts633}, -eprint = {1212.3332}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: structure,Techniques: image processing,methods: data analysis}, -month = {mar}, -number = {1}, -pages = {330--369}, -title = {{Megamorph - multiwavelength measurement of galaxy structure: Complete S{\'{e}}rsic profile information from modern surveys}}, -volume = {430}, -year = {2013} -} -@article{Er2020, -abstract = {Radio signals are delayed when propagating through plasma. This type of delay is frequencydependent and is usually used for estimating the projected number density of electrons along the line of sight, called the dispersion measure. The dense and clumpy distribution of plasma can cause refractive deflections of radio signals, analogous to lensing effects. Similar to gravitational lensing, there are two contributions to the time delay effect in plasma lensing: A geometric delay, due to increased path length of the signal, and a dispersive delay due to the change of speed of light in a plasma medium. We show the delay time for two models of the plasma distribution, and point out that the estimated dispersion measure can be biased. Since the contribution of the geometric effect can be comparable to that of the dispersive delay, the bias in the measured dispersion measure can be dramatically large if plasma lensing lensing effects are not taken into account when signals propagate through a high-density gradient clump of plasma.}, -archivePrefix = {arXiv}, -arxivId = {2001.02100}, -author = {Er, Xinzhong and Yang, Yuan Pei and Rogers, Adam}, -doi = {10.3847/1538-4357/ab66b1}, -eprint = {2001.02100}, -file = {:C\:/Users/Jammy/Documents/Papers/FRBLenses/Er2020.pdf:pdf}, -issn = {23318422}, -journal = {arXiv}, -keywords = {FRB,Galaxies: ISM,Strong lensing}, -title = {{The effects of plasma lensing on the inferred dispersion measures of fast radio bursts}}, -year = {2020} -} -@book{Buta2017, -abstract = {Rings are important and characteristic features of disc-shaped galaxies. This paper is the first in a series that re-visits galactic rings with the goals of further understanding the nature of the features and for examining their role in the secular evolution of galaxy structure. The series begins with a new sample of 3962 galaxies drawn from the Galaxy Zoo 2 citizen science data base, selected because zoo volunteers recognized a ring-shaped pattern in the morphology as seen in Sloan Digital Sky Survey colour images. The galaxies are classified within the framework of the Comprehensive de Vaucouleurs revised Hubble-Sandage system. It is found that zoo volunteers cued on the same kinds of ring-like features that were recognized in the 1995 Catalogue of Southern Ringed Galaxies. This paper presents the full catalogue of morphological classifications, comparisons with other sources of classifications and some histograms designed mainly to highlight the content of the catalogue. The advantages of the sample are its large size and the generally good quality of the images; the main disadvantage is the low physical resolution that limits the detectability of linearly small rings such as nuclear rings. The catalogue includes mainly inner and outer disc rings and lenses. Cataclysmic ('encounter-driven') rings (such as ring and polar ring galaxies) are recognized in less than 1 per cent of the sample.}, -archivePrefix = {arXiv}, -arxivId = {1707.06589}, -author = {Buta, Ronald J}, -booktitle = {Monthly Notices of the Royal Astronomical Society}, -doi = {10.1093/MNRAS/STX1829}, -eprint = {1707.06589}, -isbn = {4500050000}, -issn = {13652966}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: spiral,Galaxies: star formation,Galaxies: statistics,Galaxies: structure}, -number = {4}, -pages = {4027--4046}, -title = {{Galactic rings revisited - I. CVRHS classifications of 3962 ringed galaxies from the Galaxy Zoo 2 Database}}, -url = {http://arxiv.org/abs/1707.06589%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1829}, -volume = {471}, -year = {2017} -} -@article{Siverd2009, -abstract = {We identify, categorize, and quantify alignment effects among host and satellite galaxies using a spectroscopically-confirmed, low-redshift (z{\textless}0.23) galaxy sample from the Sloan Digital Sky Survey Data Release 6. Consistent with other recent findings, we find that satellite galaxies (SGs) of red, centrally concentrated (elliptical) host galaxies (HGs) with radial velocity separation |Delta{\_}V|{\textless}600 km/s preferentially reside near the projected major axes of their HGs. Among these, this preference is strongest for highly concentrated, red SGs. We find that fractional anisotropy increases with decreasing $\backslash$Delta{\_}V and Delta{\_}R and is nearly 40{\%} greater among the closest SGs (Delta{\_}R{\textless}250 kpc/h) relative to more distant (Delta{\_}R{\textgreater}500 kpc/h) SGs. For highly concentrated SGs at small ({\textless}300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to {\textless}15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby ({\textless}40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ({\$\sim${}}3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R J and Ryden, B S and Gaudi, B S}, -eprint = {0903.2264}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@article{Bett2010, -abstract = {We investigate the magnitude and internal alignment of the angular momentum of cold dark matter haloes in simulations with and without baryons. We analyse the cumulative angular momentum profiles of hundreds of thousands of well-resolved haloes in the Millennium Simulation of Springel et al. and in a smaller, but higher resolution, simulation, in total spanning 5 orders of magnitude in mass. For haloes of a given mass, the median specific angular momentum increases with radius as j(<=r) $\sim$ r. The direction of the vector varies considerably with radius: the median angle between the inner (<$\sim$0.25Rvir) and total (<=Rvir) angular momentum vectors is about 25°. To investigate how baryons affect halo spin, we use another high-resolution simulation, which includes gas cooling, star formation and feedback. This simulation produces a sample of galaxies with a realistic distribution of disc-to-total ratios, D/T: two-thirds of the galaxies have D/T > 0.5 in the B band. The formation of the galaxy spins up the dark matter within 0.1Rvir such that the specific halo angular momentum increases by $\sim$50 per cent in the median. The dark matter angular momentum becomes better aligned, but there remains a broad distribution of (mis-)alignments between the halo and the central galaxy, with a median angle between their angular momenta of $\sim$30°. Galaxies have a range of orientations relative to the shape of the halo: half of them have their minor axes misaligned by more than 45°, although only about 10 per cent of the galaxies lie within 30° of the plane perpendicular to the major axis of their halo. Finally, we align a sample of haloes according to the orientation of their galaxies and stack the projected mass distributions. Although the individual haloes are significantly aspherical, galaxy-halo misalignments produce a stacked mass distribution that cannot be distinguished from circular. If the lack of alignment found in our simulations is realistic, it will be extremely difficult for weak lensing studies to measure the ellipticity of cold dark matter haloes using this technique.}, -archivePrefix = {arXiv}, -arxivId = {0906.2785}, -author = {Bett, Philip and Eke, Vincent and Frenk, Carlos S. and Jenkins, Adrian and Okamoto, Takashi}, -doi = {10.1111/j.1365-2966.2010.16368.x}, -eprint = {0906.2785}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Methods: N-body simulations}, -number = {3}, -pages = {1137--1156}, -title = {{The angular momentum of cold dark matter haloes with and without baryons}}, -volume = {404}, -year = {2010} -} -@article{Harvey2015, -abstract = {Collisions between galaxy clusters provide a test of the non-gravitational forces acting on dark matter. Dark matter's lack of deceleration in the `bullet cluster collision' constrained its self-interaction cross-section $\backslash$sigma{\_}DM/m {\textless} 1.25cm2/g (68{\%} confidence limit) for long-ranged forces. Using the Chandra and Hubble Space Telescopes we have now observed 72 collisions, including both `major' and `minor' mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6$\backslash$sigma significance. The position of the dark mass has remained closely aligned within 5.8+/-8.2 kpc of associated stars: implying a self-interaction cross-section $\backslash$sigma{\_}DM/m {\textless} 0.47 cm2/g (95{\%} CL) and disfavoring some proposed extensions to the standard model.}, -archivePrefix = {arXiv}, -arxivId = {1503.07675}, -author = {Harvey, David and Massey, Richard and Kitching, Thomas and Taylor, Andy and Tittley, Eric}, -doi = {10.1126/science.1261381}, -eprint = {1503.07675}, -issn = {10959203}, -journal = {Science}, -number = {6229}, -pages = {1462--1465}, -pmid = {25814581}, -title = {{The nongravitational interactions of dark matter in colliding galaxy clusters}}, -volume = {347}, -year = {2015} -} -@article{Enia2018, -abstract = {We perform lens modelling and source reconstruction of Sub-millimetre Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500$\mu$m in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). A previous analysis of the same data set used a single S{\'{e}}rsic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from theH-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission.We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5s. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value reff $\sim$ 1.77 kpc and a median Gaussian full width at half-maximum $\sim$1.47 kpc. After correction for magnification, our sources have intrinsic star formation rates (SFR) $\sim$ 900-3500M⊙ yr-1, resulting in a median SFR surface density $\Sigma$SFR $\sim$ 132M⊙ yr-1 kpc-2 (or $\sim$218M⊙ yr-1 kpc-2 for the Gaussian fit). This is consistent with that observed for other star-forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst.}, -archivePrefix = {arXiv}, -arxivId = {1801.01831}, -author = {Enia, A. and Negrello, M. and Gurwell, M. and Dye, S. and Rodighiero, G. and Massardi, M. and {De Zotti}, G. and Franceschini, A. and Cooray, A. and van der Werf, P. and Birkinshaw, M. and Michalowski, M. J. and Oteo, I.}, -doi = {10.1093/mnras/sty021}, -eprint = {1801.01831}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Enia et al. - 2018 - The Herschel-ATLAS Magnifications and physical sizes of 500-$\mu$m-selected strongly lensed galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong,Instrumentation: interferometers}, -number = {3}, -pages = {3467--3484}, -title = {{The Herschel-ATLAS: Magnifications and physical sizes of 500-$\mu$m-selected strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1801.01831}, -volume = {475}, -year = {2018} -} -@article{Short2012, -abstract = {The identification of strong gravitational lenses in large surveys has historically been a rather time consuming exercise. Early data from the Herschel Astrophysical Terahertz Large Area Survey (Herschel-ATLAS) demonstrate that lenses can be identified efficiently at submillimetre wavelengths using a simple flux criteria. Motivated by that development, this work considers the statistical properties of strong gravitational lens systems which have been, and will be, found by the Herschel-ATLAS. Analytical models of lens statistics are tested with the current best estimates for the various model ingredients. These include the cosmological parameters, the mass function and the lens density profile, for which we consider the singular isothermal sphere (SIS) and the Navarro, Frenk & White (NFW) approximations. The five lenses identified in the Herschel-ATLAS Science Demonstration Phase suggest a SIS density profile is preferred, but cannot yet constrain \Omega_\Lambda to an accuracy comparable with other methods. The complete Herschel-ATLAS data set should be sufficient to yield competitive constraints on \Omega_\Lambda. Whilst this huge number of lenses has great potential for constraining cosmological parameters, they will be most powerful in constraining uncertainty in astrophysical processes. Further investigation is needed to fully exploit this unprecedented data set.}, -archivePrefix = {arXiv}, -arxivId = {1206.4919}, -author = {Short, Jo and Pearson, Elizabeth and Coles, Peter and Eales, Steve}, -eprint = {1206.4919}, -journal = {Mnras}, -number = {June}, -pages = {1--14}, -title = {{Strong Gravitational Lens Statistics using the Herschel-ATLAS}}, -url = {http://arxiv.org/abs/1206.4919}, -volume = {000}, -year = {2012} -} -@article{Huang2018, -abstract = {We use $\sim$100 deg2 of deep (> 28.5 mag arcsec-2 in i band), high-quality (median 0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) survey to reveal the halo mass dependence of the surface mass density profiles and outer stellar envelopes of massive galaxies. The i-band images from the HSC survey reach $\sim$4 mag deeper than Sloan Digital Sky Survey and enable us to directly trace stellar mass distributions to 100 kpc without requiring stacking. We conclusively show that, at fixed stellar mass, the stellar profiles of massive galaxies depend on the masses of their dark matter haloes. On average, massive central galaxies with log10(M*, 100 kpc/M⊙) > 11.6 in more massive haloes at 0.3 < z < 0.5 have shallower inner stellar mass density profiles (within $\sim$10-20 kpc) and more prominent outer envelopes. These differences translate into a halo mass dependence of the mass-size relation. Central galaxies in haloes with log10(M200b/M⊙) > 14.0 are $\sim$20 per cent larger in R50 at fixed M*, 100 kpc. Such dependence is also reflected in the relationship between the stellarmass within 10 and 100 kpc. Comparing to the mass-size relation, the M*, 100 kpc-M*, 10 kpc relation avoids the ambiguity in the definition of size, and can be straightforwardly compared with simulations. Our results demonstrate that, with deep images from HSC, we can quantify the connection between halo mass and the outer stellar halo, which may provide new constraints on the formation and assembly of massive central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1803.02824}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Mandelbaum, Rachel and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/sty1136}, -eprint = {1803.02824}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2018 - A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: haloes,Galaxies: photometry,Galaxies: structure}, -number = {1}, -pages = {521--537}, -title = {{A detection of the environmental dependence of the sizes and stellar haloes of massive central galaxies}}, -url = {http://arxiv.org/abs/1803.02824}, -volume = {480}, -year = {2018} -} -@article{Yan2016, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R$\sim$2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is $\sim$73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R. and Bershady, Matthew A. and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M. and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R. and Thomas, Daniel and Wake, David A. and Weijmans, Anne-Marie and Westfall, Kyle B. and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A. and Blanton, Michael R. and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T. and Goddard, Daniel and Gunn, James E. and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R. and Oravetz, Daniel and Pan, Kaike and Parejko, John K. and Sanchez, Sebastian F. and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yan et al. - 2016 - SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY.pdf:pdf}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {6}, -pages = {197}, -title = {{SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY}}, -url = {http://arxiv.org/abs/1607.08613%0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {152}, -year = {2016} -} -@article{Pontzen2017, -abstract = {We show how the interplay between active galactic nuclei (AGN) and merger history determines whether a galaxy quenches star formation at high redshift. We first simulate, in a full cosmological context, a galaxy of total dynamical mass {\$}10{\^{}}{\{}12{\}}\backslash,M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} at {\$}z=2{\$}. Then we systematically alter the accretion history of the galaxy by minimally changing the linear overdensity in the initial conditions. This "genetic modification" approach allows the generation of three sets of {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM initial conditions leading to maximum merger ratios of 1:10, 1:5 and 2:3 respectively. The changes leave the final halo mass, large scale structure and local environment unchanged, providing a controlled numerical experiment. Interaction between the AGN physics and mergers in the three cases lead respectively to a star-forming, temporarily-quenched and permanently-quenched galaxy. However the differences do not primarily lie in the black hole accretion rates, but in the kinetic effects of the merger: the galaxy is resilient against AGN feedback unless its gaseous disk is first disrupted. Typical accretion rates are comparable in the three cases, falling below {\$}0.1\backslash,M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} yr{\$}{\^{}}{\{}-1{\}}{\$}, equivalent to around {\$}2\backslashbackslash{\{}\backslash{\%}{\}}{\$} of the Eddington rate or {\$}10{\^{}}{\{}-3{\}}{\$} times the pre-quenching star formation rate, in agreement with observations. This low level of black hole accretion can be sustained even when there is insufficient dense cold gas for star formation. Conversely, supernova feedback is too distributed to generate outflows in high-mass systems, and cannot maintain quenching over periods longer than the halo gas cooling time.}, -archivePrefix = {arXiv}, -arxivId = {1607.02507}, -author = {Pontzen, Andrew and Tremmel, Michael and Roth, Nina and Peiris, Hiranya V and Saintonge, Am{\'{e}}lie and Volonteri, Marta and Quinn, Tom and Governato, Fabio}, -doi = {10.1093/mnras/stw2627}, -eprint = {1607.02507}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: star formation,Galaxies: stellar content}, -number = {1}, -pages = {547--558}, -title = {{How to quench a galaxy}}, -volume = {465}, -year = {2017} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the `Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a {\$}(100 \backslash,\backslashbackslashrm cMpc){\^{}}3{\$} and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts {\$}0{\$} and {\$}1{\$}, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar `downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Keeton2005, -abstract = {When the source in a four-image gravitational lens system lies sufficiently close to a fold caustic, two of the lensed images lie very close together. If the lens potential is smooth on the scale of the separation between the two close images, the difference between their fluxes should approximately vanish, Rfold ≡ (F+ - F-)/(F+ + F-) ≈ 0. (The subscript indicates the image parity.) Violations of this fold relation in observed lenses are thought to indicate the presence of structure on scales smaller than the separation between the close images. We present a detailed study of the fold relation in realistic smooth lenses, finding it to be more subtle and rich than was previously realized. The degree to which Rfold can differ from zero for smooth lenses depends not only on the distance of the source from the caustic, but also on its location along the caustic, and then on the angular structure of the lens potential (ellipticity, multipole modes, and external shear). Since the source position is unobservable, it is impossible to say from Rfold alone whether the flux ratios in an observed lens are anomalous or not. Instead, we must consider the full distribution of Rfold values that can be obtained from smooth lens potentials that reproduce the separation d1 between the two close images and the distance d2 to the next nearest image. (By reducing the image configuration to these two numbers, we limit our model dependence and obtain a generic analysis.) We show that the generic features of this distribution can be understood, which means that the fold relation provides a robust probe of small-scale structure in lens galaxies. We then compute the full distribution using Monte Carlo simulations of realistic smooth lenses. Comparing these predictions with the data, we find that five of the 12 known lenses with fold configurations have flux ratio anomalies: B0712+472, SDSS 0924+0219, PG 1115+080, B1555+375, and B1933+503. Combining this with our previous analysis revealing anomalies in three of the four known lenses with cusp configurations, we conclude that at least half (8/16) of all four-image lenses that admit generic, local analyses exhibit flux ratio anomalies. The fold and cusp relations do not reveal the nature of the implied small-scale structure, but do provide the formal foundation for substructure studies, and also indicate which lenses deserve further study. Although our focus is on close pairs of images, we show that the fold relation can be used—with great care—to analyze all image pairs in all 22 known four-image lenses and reveal lenses with some sort of interesting structure.}, -author = {Keeton, Charles R. and Gaudi, B. Scott and Petters, A. O.}, -doi = {10.1086/497324}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {Cosmology: Dark Matter,Cosmology: Gravitational Lensing,Cosmology: Large-Scale Structure of Universe,Cosmology: Theory,Galaxies: Formation}, -month = {dec}, -number = {1}, -pages = {35}, -title = {{Identifying Lenses with Small-Scale Structure. II. Fold Lenses}}, -url = {http://iopscience.iop.org/0004-637X/635/1/35/fulltext/}, -volume = {635}, -year = {2005} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Mendez-Abreu2010a, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Dominika2016, -abstract = {Spectral features introduced by instrumental chromaticity of radio interferometers have the potential to negatively impact the ability to perform Epoch of Reionisation (EoR) and Cosmic Dawn (CD) science using the redshifted neutral hydrogen emission line from the early Universe. We describe instrument calibration choices that influence the spectral characteristics of the science data, and assess their impact on EoR statistical and tomographic experiments. Principally, we consider the intrinsic spectral response of the receiving antennas, embedded within a complete frequency-dependent primary beam response, and frequency-dependent instrument sampling. We assess different options for bandpass calibration. The analysis is applied to the proposed SKA1-Low EoR/CD experiments. We provide tolerances on the smoothness of the SKA station primary beam bandpass, to meet the scientific goals of statistical and tomographic (imaging) EoR programs. Two calibration strategies are tested: (1) fitting of each fine channel independently, and (2) fitting of an nth-order polynomial for each {\$\sim${}}1{\$\sim${}}MHz coarse channel with (n+1)th-order residuals (n=2,3,4). Strategy (1) leads to uncorrelated power in the 2D power spectrum proportional to the thermal noise power, thereby reducing the overall array sensitivity. Strategy (2) leads to correlated residuals from the fitting, and residual signal power with (n+1)th-order curvature. For the residual power to be less than the thermal noise, the fractional amplitude of a fourth-order term in the bandpass across a single coarse channel must be {\textless}2.5{\%} (50{\$\sim${}}MHz), {\textless}0.5{\%} (150{\$\sim${}}MHz), {\textless}0.8{\%} (200{\$\sim${}}MHz). The tomographic experiment places stringent constraints on phase residuals in the bandpass. We find that the root-mean-square variability over all stations of the change in phase across any fine channel (4.578{\$\sim${}}kHz) should not exceed 0.2 degrees.}, -archivePrefix = {arXiv}, -arxivId = {1604.03273}, -author = {Trott, Cathryn M and Wayth, Randall B}, -doi = {10.1017/pas.2016.xxx}, -eprint = {1604.03273}, -issn = {14486083}, -journal = {arXiv preprint arXiv: {\ldots}}, -keywords = {aboriginal astronomy,ethnoastronomy,history of astronomy}, -number = {3}, -pages = {15}, -title = {{Australian Aboriginal Astronomy and Navigation arXiv:1607.02215v1}}, -url = {http://arxiv.org/abs/1604.03273}, -volume = {447}, -year = {2016} -} -@article{Mendez-Abreu2010, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A < 0.9). This fraction is 33%, 55%, and 43% if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C < (A + B)/2). Only 18% of the observed bulges have a probability >50% and none has a probability >90% of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n > 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T > 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n > 2 and B/T > 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n > 2 and with B/T > 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n > 2 and B/T > 0.3. {\textcopyright} 2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J. and Simonneau, E. and Aguerri, J. A.L. and Corsini, E. M.}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/M{\'{e}}ndez-Abreu et al. - 2010 - Structural properties of disk galaxies II. Intrinsic shape of bulges(3).pdf:pdf}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {galaxies: bulges,galaxies: elliptical and lenticular, cD,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ({\$}z = 1.489{\$}), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5{\$}+{\$}2223 ({\$}z = 0.542{\$}), published by Grillo et al. (2016), and explore different {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of {\$}H{\_}{\{}0{\}}{\$} and {\$}\backslashbackslashOmega{\{}\backslash{\_}{\}}{\{}\backslashbackslashrm m{\}}{\$} with relative (1{\$}\backslashbackslashsigma{\{}\backslash{\$}{\}}) statistical errors of, respectively, 6{\%} (7{\%}) and 31{\%} (26{\%}) in flat (general) cosmological models, assuming a conservative 3{\%} uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of {\$}H{\_}{\{}0{\}}{\$}, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C and Rosati, P and Suyu, S H and Balestra, I and Caminha, G B and Halkola, A and Kelly, P L and Lombardi, M and Mercurio, A and Rodney, S A and Treu, T}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -issn = {15384357}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -title = {{Measuring the value of the Hubble constant "{\$}\backslash{\$}`a la Refsdal"}}, -url = {http://arxiv.org/abs/1802.01584}, -year = {2018} -} -@article{Bolzonella2000, -abstract = {We report experimental results on the structure and melting behavior of ice confined in multi-walled carbon nanotubes and ordered mesoporous carbon CMK-3, which is the carbon replica of a SBA-15 silica template. The silica template has cylindrical mesopores with micropores connecting the walls of neighboring mesopores. The structure of the carbon replica material CMK-3 consists of carbon rods connected by smaller side-branches, with quasi-cylindrical mesopores of average pore size 4.9 nm and micropores of 0.6 nm. Neutron diffraction and differential scanning calorimetry have been used to determine the structure of the confined ice and the solid-liquid transition temperature. The results are compared with the behavior of water in multi-walled carbon nanotubes of inner diameters of 2.4 nm and 4 nm studied by the same methods. For D2O in CMK-3 we find evidence of the existence of nanocrystals of cubic ice and ice IX; the diffraction results also suggest the presence of ice VIII, although this is less conclusive. We find evidence of cubic ice in the case of the carbon nanotubes. For bulk water these crystal forms only occur at temperatures below 170 K in the case of cubic ice, and at pressures of hundreds or thousands of MPa in the case of ice VIII and IX. These phases appear to be stabilized by the confinement. {\textcopyright} 2011 the Owner Societies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0003380}, -author = {Jazdzewska, Monika and {\'{S}}liwinska-Bartkowiak, Ma{\l}gorzata M. and Beskrovnyy, Anatoly I. and Vasilovskiy, Sergey G. and Ting, Siu Wa and Chan, Kwong Yu and Huang, Liangliang and Gubbins, Keith E.}, -doi = {10.1039/c0cp02797a}, -eprint = {0003380}, -issn = {14639076}, -journal = {Physical Chemistry Chemical Physics}, -keywords = {GALAXIES: GENERAL,Galaxies: Distances and Redshifts,METHODS: DATA ANALYSIS,TECHNIQUES: PHOTOMETRIC}, -month = {nov}, -number = {19}, -pages = {9008--9013}, -pmid = {21451863}, -primaryClass = {astro-ph}, -title = {{Novel ice structures in carbon nanopores: Pressure enhancement effect of confinement}}, -url = {http://arxiv.org/abs/astro-ph/0003380}, -volume = {13}, -year = {2011} -} -@article{Oser2010a, -abstract = {Cosmological simulations of galaxy formation appear to show a "two-phase" character with a rapid early phase at z≳2 duringwhich "in situ" stars are formedwithin the galaxy from infalling cold gas followed by an extended phase since z≲3 duringwhich "ex situ" stars are primarily accreted. In the latter phase, massive systems growconsiderably in mass and radius by accretion of smaller satellite stellar systems formed at quite early times (z > 3) outside of the virial radius of the forming central galaxy. These tentative conclusions are obtained from high-resolution resimulations of 39 individual galaxies in a full cosmological context with present-day virial halomasses ranging from 7×10 11M⊙ h -1 ≲ Mvir ≲ 2.7×1013M⊙ h -1 (h = 0.72) and central galaxy masses between 4.5×1010M⊙ h -1 ≲ M* ≲ 3.6 × 1011M⊙ h -1. The simulations include the effects of a uniform UV background, radiative cooling, star formation, and energetic feedback from Type II supernova. The importance of stellar accretion increases with galaxy mass and toward lower redshift. In our simulations, lower mass galaxies (M* ≲ 9 × 10 10M⊙ h -1) accrete about 60% of their present-day stellar mass. High-mass galaxy (M* ≳ 1.7 × 10 11M⊙ h -1) assembly is dominated by accretion and merging with about 80% of the stars added by the present day. In general the simulated galaxies approximately double their mass since z = 1. For massive systems this mass growth is not accompanied by significant star formation. The majority of the in situ created stars are formed at z > 2, primarily out of cold gas flows. We recover the observational result of "archaeological downsizing," where the most massive galaxies harbor the oldest stars. We find that this is not in contradiction with hierarchical structure formation. Most stars in the massive galaxies are formed early on in smaller structures; the galaxies themselves are assembled late. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1010.1381}, -author = {Oser, Ludwig and Ostriker, Jeremiah P. and Naab, Thorsten and Johansson, Peter H. and Burkert, Andreas}, -doi = {10.1088/0004-637X/725/2/2312}, -eprint = {1010.1381}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oser et al. - 2010 - The two phases of galaxy formation(3).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Cosmology:theory,Dark matter,Galaxies:evolution,Galaxies:formation,Methods:numerical}, -number = {2}, -pages = {2312--2323}, -title = {{The two phases of galaxy formation}}, -volume = {725}, -year = {2010} -} -@article{Pontzen2017, -abstract = {We show how the interplay between active galactic nuclei (AGNs) and merger history determines whether a galaxy quenches star formation (SF) at high redshift. We first simulate, in a full cosmological context, a galaxy of total dynamical mass Mvir = 1012M⊙ at z = 2. Then we systematically alter the accretion history of the galaxy by minimally changing the linear overdensity in the initial conditions. This 'genetic modification' approach allows the generation of three sets of $\Lambda$ CDM initial conditions leading to maximum merger ratios of 1:10, 1:5 and 2:3, respectively. The changes leave the final halo mass, large-scale structure and local environment unchanged, providing a controlled numerical experiment. Interaction between the AGN physics and mergers in the three cases leads, respectively, to a star-forming, temporarily quenched and permanently quenched galaxy. However, the differences do not primarily lie in the black hole accretion rates, but in the kinetic effects of the merger: the galaxy is resilient against AGN feedback unless its gaseous disc is first disrupted. Typical accretion rates are comparable in the three cases, falling below 0.1M⊙ yr-1, equivalent to around 2 per cent of the Eddington rate or 10-3 times the pre-quenching star formation rate, in agreement with observations. This low level of black hole accretion can be sustained even when there is insufficient dense cold gas for SF. Conversely, supernova feedback is too distributed to generate outflows in high-mass systems, and cannot maintain quenching over periods longer than the halo gas cooling time.}, -archivePrefix = {arXiv}, -arxivId = {1607.02507}, -author = {Pontzen, Andrew and Tremmel, Michael and Roth, Nina and Peiris, Hiranya V and Saintonge, Am{\'{e}}lie and Volonteri, Marta and Quinn, Tom and Governato, Fabio}, -doi = {10.1093/mnras/stw2627}, -eprint = {1607.02507}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: star formation,Galaxies: stellar content}, -number = {1}, -pages = {547--558}, -title = {{How to quench a galaxy}}, -volume = {465}, -year = {2017} -} -@article{Press2001, -abstract = {The product of a unique collaboration among four leading scientists in academic research and industry, Numerical Recipes is a comprehensive text and reference work on scientific computing. Thoroughly self-contained, it proceeds from mathematical and theoretical considerations to actual, practical computer routines. This new version incorporates completely new C++ versions of the more than 300 Numerical Recipes Second Edition routines widely recognized as the most accessible and practical basis for scientific computing, in addition to including the full mathematical and explanatory contents of Numerical Recipes in C. Key Features: Includes linear algebra, interpolation, special functions, random numbers, nonlinear sets of equations, optimization, eigensystems, Fourier methods and wavelets, statistical tests, ODEs and PDEs, integral equations, and inverse theory. A wealth of tricks and tips for scientific computing in C++ The routines, in ANSI/ISO C++ source code, can be used with almost any existing C++ vector/matrix class library, according to user preference Includes a simple class library for stand-alone use Other new Numerical Recipes products for your library... Numerical Recipes Example Book C++ Numerical Recipes Code CDROM with Windows, DOS, or Macintosh Single Screen License-v2.10 including C++, Second Edition Numerical Recipes Code CDROM with LINUX or UNIX Single Screen License v2.10 including C++, Second Edition Numerical Recipes Code CDROM with Windows, DOS, or Macintosh Single Screen License}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {Seiler, Mary C. and Seiler, Fritz A.}, -doi = {10.1111/j.1539-6924.1989.tb01007.x}, -eprint = {arXiv:1011.1669v3}, -isbn = {2245-1919}, -issn = {15396924}, -journal = {Risk Analysis}, -number = {3}, -pages = {415--416}, -pmid = {25186536}, -title = {{Numerical Recipes in C: The Art of Scientific Computing}}, -url = {http://www.jstor.org/stable/1269484?origin=crossref}, -volume = {9}, -year = {1989} -} -@article{Xie2014, -abstract = {Recent work has suggested that the amplitude of the size mass relation of massive early type galaxies evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive early type galaxies. We find this model is able to reproduce the amplitude of present day amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark halos at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than {\$}10{\^{}}{\{}11.4{\}}M{\_}{\{}\backslashodot{\}}{\$}. At lower masses, low mass ratio mergers play a more important role. In situ star formation contribute more to the size growth than it does to stellar mass growth. We also find that, for ETGs identified at {\$}z=2{\$}, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stu2487}, -volume = {447}, -year = {2015} -} -@article{Dubois2013, -abstract = {In order to understand the physical mechanisms at work during the formation of massive early-type galaxies, we performed six zoomed hydrodynamical cosmological simulations of haloes in the mass range 4.3×1012 ≤Mvir ≤8.0×1013M at z=0, using the AdaptiveMesh Refinement code RAMSES. These simulations explore the role of active galactic nuclei (AGN), through jets powered by the accretion on to supermassive black holes on the formation of massive elliptical galaxies. In the absence of AGN feedback, large amounts of stars accumulate in the central galaxies to form overly massive, blue, compact and rotation-dominated galaxies. Powerful AGN jets transform the central galaxies into red extended and dispersion-dominated galaxies. This morphological transformation of disc galaxies into elliptical galaxies is driven by the efficient quenching of the in situ star formation due to AGN feedback, which transform these galaxies into systems built up by accretion. For galaxies mainly formed by accretion, the proportion of stars deposited farther away from the centre increases, and galaxies have larger sizes. The accretion is also directly responsible for randomizing the stellar orbits, increasing the amount of dispersion over rotation of stars as a function of time. Finally, we find that our galaxies simulated with AGN feedback better match the observed scaling laws, such as the size-mass, velocity dispersion-mass, Fundamental Plane relations and slope of the total density profiles at z 0, from dynamical and strong lensing constraints.{\textcopyright} 2013 The Authors.}, -archivePrefix = {arXiv}, -arxivId = {1301.3092}, -author = {Dubois, Yohan and Gavazzi, Rapha{\"{e}}l and Peirani, S{\'{e}}bastien and Silk, Joseph}, -doi = {10.1093/mnras/stt997}, -eprint = {1301.3092}, -isbn = {0197-3851 (Print)\n0197-3851 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods:Numerical,galaxies: jets,galaxies:Active,galaxies:Elliptical and lenticular:CD,galaxies:Formation,galaxies:Kinematics and dynamics}, -month = {aug}, -number = {4}, -pages = {3297--3313}, -pmid = {17099929}, -title = {{AGN-driven quenching of star formation: Morphological and dynamical implications for early-type galaxies}}, -volume = {433}, -year = {2013} -} -@article{Ellison2017, -abstract = {The tight correlation between total galaxy stellar mass and star formation rate (SFR) has become known as the star-forming main sequence. Using {\$\sim${}}487 000 spaxels from galaxies observed as part of the Sloan Digital Sky Survey Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, we confirm previous results that a correlation also exists between the surface densities of star formation ($\Sigma$SFR) and stellar mass ($\Sigma$*) on kpc scales, representing a 'resolved' main sequence. Using a new metric ($\Delta$$\Sigma$SFR), which measures the relative enhancement or deficit of star formation on a spaxel-by-spaxel basis relative to the resolved main sequence, we investigate the SFR profiles of 864 galaxies as a function of their position relative to the global star-forming main sequence ($\Delta$SFR). For galaxies above the global main sequence (positive $\Delta$SFR) $\Delta$$\Sigma$SFR is elevated throughout the galaxy, but the greatest enhancement in star formation occurs at small radii ({\textless} 3 kpc, or 0.5Re). Moreover, galaxies that are at least a factor of 3 above the main sequence show diluted gas phase metallicities out to 2Re, indicative of metal-poor gas inflows accompanying the starbursts. For quiescent/passive galaxies that lie at least a factor of 10 below the star-forming main sequence, there is an analogous deficit of star formation throughout the galaxy with the lowest values of $\Delta$$\Sigma$SFR in the central 3 kpc. Our results are in qualitative agreement with the 'compaction' scenario in which a central starburst leads to mass growth in the bulge and may ultimately precede galactic quenching from the inside-out.}, -archivePrefix = {arXiv}, -arxivId = {1711.00915}, -author = {Ellison, Sara L and S{\'{a}}nchez, Sebastian F and Ibarra-Medel, Hector and Antonio, Braulio and Mendel, J Trevor and Barrera-Ballesteros, Jorge}, -doi = {10.1093/mnras/stx2882}, -eprint = {1711.00915}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: interactions,Galaxies: star formation}, -number = {2}, -pages = {2039--2054}, -title = {{Star formation is boosted (and quenched) from the inside-out: Radial star formation profiles from MaNGA}}, -url = {http://arxiv.org/abs/1711.00915}, -volume = {474}, -year = {2018} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the foreground lenses and background sources are early-type galaxies. Using imaging from Hubble Space Telescope (HST)/Advanced Camera for Studies (ACS) andKeck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population ofmassive, compact galaxies at redshifts 0.4 ≲ z ≲ 0.7, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of highredshift red nuggets or their partly evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar populations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S{\'{e}}rsic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still compact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterized by red-to-blue colour gradients as a function of radius which are stronger at low redshift - indicative of ongoing accretion - but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are pre-dominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W and Fassnacht, Christopher D and Treu, Tommaso and Brewer, Brendon J and Koopmans, L V E and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z ∼ 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u - g color profiles for these galaxies and show that most z ∼ 2galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z ∼ 2galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: ($\Delta$(u - g rest)/$\Delta$(log r))median = -0.47, -0.33, and -0.46 for z ∼ 2, z ∼ 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z ∼ 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u - g colors, and lower S{\'{e}}rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch. {\textcopyright}2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J and {Van Dokkum}, Pieter G and Labb{\'{e}}, Ivo and Illingworth, Garth D and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Spindler2017, -abstract = {We study the spatially resolved star formation of 1494 galaxies in the SDSS-IV MaNGA Survey. Star formation rates (SFRs) are calculated using a two-step process, using H$\alpha$ in starforming regions and Dn4000 in regions identified as active galactic nucleus/low-ionization (nuclear) emission region [AGN/LI(N)ER] or lineless. The roles of secular and environmental quenching processes are investigated by studying the dependence of the radial profiles of specific star formation rate on stellar mass, galaxy structure, and environment. We report on the existence of 'centrally suppressed' galaxies, which have suppressed Specific Star Formation Rate (SSFR) in their cores compared to their discs. The profiles of centrally suppressed and unsuppressed galaxies are distributed in a bimodal way. Galaxies with high stellar mass and core velocity dispersion are found to be much more likely to be centrally suppressed than low-mass galaxies, and we show that this is related to morphology and the presence of AGN/LI(N)ER like emission. Centrally suppressed galaxies also display lower star formation at all radii compared to unsuppressed galaxies. The profiles of central and satellite galaxies are also compared, and we find that satellite galaxies experience lower specific star formation rates at all radii than central galaxies. This uniform suppression could be a signal of the stripping of hot halo gas in the process known as strangulation. We find that satellites are not more likely to be suppressed in their cores than centrals, indicating that the core suppression is an entirely internal process. We find no correlation between the local environment density and the profiles of star formation rate surface density.}, -archivePrefix = {arXiv}, -arxivId = {1710.05049}, -author = {Spindler, Ashley and Wake, David and Belfiore, Francesco and Bershady, Matthew and Bundy, Kevin and Drory, Niv and Masters, Karen and Thomas, Daniel and Westfall, Kyle and Wild, Vivienne}, -doi = {10.1093/mnras/sty247}, -eprint = {1710.05049}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Spindler et al. - 2018 - SDSS-IV MaNGA The spatial distribution of star formation and its dependence on mass, structure, and environment.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Bulges,Galaxies: Clusters: General,Galaxies: Evolution,Galaxies: Groups: General,Galaxies: Star formation,Galaxies: Structure}, -number = {1}, -pages = {580--600}, -title = {{SDSS-IV MaNGA: The spatial distribution of star formation and its dependence on mass, structure, and environment}}, -url = {http://arxiv.org/abs/1710.05049}, -volume = {476}, -year = {2018} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Geometryej, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Peng2010, -abstract = {We present a two-dimensional (2D) fitting algorithm (GALFIT, ver. 3) with new capabilities to study the structural components of galaxies and other astronomical objects in digital images. Our technique improves on previous 2D fitting algorithms by allowing for irregular, curved, logarithmic and power-law spirals, ring, and truncated shapes in otherwise traditional parametric functions like the S{\'{e}}rsic, Moffat, King, Ferrer, etc., profiles. One can mix and match these new shape features freely, with or without constraints, and apply them to an arbitrary number of model components of numerous profile types, so as to produce realistic-looking galaxy model images. Yet, despite the potential for extreme complexity, the meaning of the key parameters like the S{\'{e}}rsic index, effective radius, or luminosity remains intuitive and essentially unchanged. The new features have an interesting potential for use to quantify the degree of asymmetry of galaxies, to quantify low surface brightness tidal features beneath and beyond luminous galaxies, to allow more realistic decompositions of galaxy subcomponents in the presence of strong rings and spiral arms, and to enable ways to gauge the uncertainties when decomposing galaxy subcomponents. We illustrate these new features by way of several case studies that display various levels of complexity. {\textcopyright}2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0912.0731}, -author = {Peng, Chien Y and Ho, Luis C and Impey, Chris D and Rix, Hans Walter}, -doi = {10.1088/0004-6256/139/6/2097}, -eprint = {0912.0731}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Galaxies: bulges,Galaxies: fundamental parameters,Galaxies: structure,Techniques: image processing,Techniques: photometric}, -number = {6}, -pages = {2097--2129}, -title = {{Detailed decomposition of galaxy images. II. beyond axisymmetric models}}, -volume = {139}, -year = {2010} -} -@article{Mendez-Abreu2016, -abstract = {We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area data release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log (M∗/MȮ) {\textgreater} 11), the galaxy population is dominated by galaxies modelled with a single S{\'{e}}rsic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T {\textgreater} 0.2. At intermediate masses (9.5 {\textless} log (M∗/MȮ) {\textless} 11), galaxies described with bulge+disc but B/T {\textless} 0.2 are preponderant, whereas, at the low mass end (log (M∗/MȮ) {\textless} 9.5), the prevailing population is constituted by galaxies modelled with either purediscs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57{\%} of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5 {\textless} log (M∗/MȮ) {\textless} 11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62{\%}, 28{\%}, and 10{\%} for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.}, -archivePrefix = {arXiv}, -arxivId = {1610.05324}, -author = {M{\'{e}}ndez-Abreu, J and Ruiz-Lara, T and S{\'{a}}nchez-Menguiano, L and {De Lorenzo-C{\'{a}}ceres}, A and Costantin, L and Catal{\'{a}}n-Torrecilla, C and Florido, E and Aguerri, J A L and Bland-Hawthorn, J and Corsini, E M and Dettmar, R J and Galbany, L and Garc{\'{i}}a-Benito, R and Marino, R A and M{\'{a}}rquez, I and Ortega-Minakata, R A and Papaderos, P and S{\'{a}}nchez, S F and S{\'{a}}nchez-Blazquez, P and Spekkens, K and {Van De Ven}, G and Wild, V and Ziegler, B}, -doi = {10.1051/0004-6361/201629525}, -eprint = {1610.05324}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -title = {{Two-dimensional multi-component photometric decomposition of CALIFA galaxies}}, -url = {http://arxiv.org/abs/1610.05324%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201629525}, -volume = {598}, -year = {2017} -} -@article{Sanderson2009, -abstract = {We study the distribution of projected offsets between the cluster X-ray centroid and the brightest cluster galaxy (BCG) for 65 X-ray-selected clusters from the Local Cluster Substructure Survey, with a median redshift of z = 0.23. We find a clear correlation between X-ray/BCG projected offset and the logarithmic slope of the cluster gas density profile at 0.04r 500($\alpha$), implying that more dynamically disturbed clusters have weaker cool cores. Furthermore, there is a close correspondence between the activity of the BCG, in terms of detected H$\alpha$ and radio emission, and the X-ray/BCG offset, with the line-emitting galaxies all residing in clusters with X-ray/BCG offsets of ≤15 kpc. Of the BCGs with $\alpha$ {\textless} -0.85 and an offset {\textless}0.02r500, 96 per cent (23/24) have optical emission and 88 per cent (21/24) are radio active, while none has optical emission outside these criteria. We also study the cluster gas fraction (fgas) within r500 and find a significant correlation with X-ray/BCG projected offset. The mean fgas of the 'small offset' clusters ({\textless}0.02r 500) is 0.106 ± 0.005 ($\sigma$ = 0.03) compared to 0.145 ± 0.009 ($\sigma$ = 0.04) for those with an offset {\textgreater}0.02r 500, indicating that the total mass may be systematically underestimated in clusters with larger X-ray/BCG offsets. Our results imply a link between cool core strength and cluster dynamical state consistent with the view that cluster mergers can significantly perturb cool cores, and set new constraints on models of the evolution of the intracluster medium. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0906.1808}, -author = {Sanderson, Alastair J R and Edge, Alastair C and Smith, Graham P}, -doi = {10.1111/j.1365-2966.2009.15214.x}, -eprint = {0906.1808}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: Clusters: general,Galaxies: Elliptical and lenticular,Galaxies: Evolution,X-rays: Galaxies: Clusters,cD}, -number = {4}, -pages = {1698--1705}, -title = {{LoCuSS: The connection between brightest cluster galaxy activity, gas cooling and dynamical disturbance of X-ray cluster cores}}, -volume = {398}, -year = {2009} -} -@article{Rhodes2010, -abstract = {(Abridged) We examine the effects of charge transfer inefficiency (CTI) during CCD readout on galaxy shape measurements required by studies of weak gravitational lensing. We simulate a CCD readout with CTI such as that caused by charged particle radiation damage. We verify our simulations on data from laboratory-irradiated CCDs. Only charge traps with time constants of the same order as the time between row transfers during readout affect galaxy shape measurements. We characterize the effects of CTI on various galaxy populations. We baseline our study around p-channel CCDs that have been shown to have charge transfer efficiency up to an order of magnitude better than several models of n-channel CCDs designed for space applications. We predict that for galaxies furthest from the readout registers, bias in the measurement of galaxy shapes, Delta(e), will increase at a rate of 2.65 +/- 0.02 x 10{\^{}}(-4) per year at L2 for accumulated radiation exposure averaged over the solar cycle. If uncorrected, this will consume the entire shape measurement error budget of a dark energy mission within about 4 years. Software mitigation techniques demonstrated elsewhere can reduce this by a factor of {\$\sim${}}10, bringing the effect well below mission requirements. CCDs with higher CTI than the ones we studeied may not meet the requirements of future dark energy missions. We discuss ways in which hardware could be designed to further minimize the impact of CTI.}, -archivePrefix = {arXiv}, -arxivId = {1002.1479}, -author = {Rhodes, Jason and Leauthaud, Alexie and Stoughton, Chris and Massey, Richard and Dawson, Kyle and Kolbe, William and Roe, Natalie}, -doi = {10.1086/651675}, -eprint = {1002.1479}, -issn = {00046280}, -journal = {Publ. Astron. Soc. Pac.}, -month = {apr}, -number = {890}, -pages = {439--450}, -pmid = {275881000005}, -title = {{The Effects of Charge Transfer Inefficiency (CTI) on Galaxy Shape Measurements}}, -url = {http://arxiv.org/abs/1002.1479%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/651675}, -volume = {122}, -year = {2010} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the foreground lenses and background sources are early-type galaxies. Using imaging from HST/ACS and Keck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population of massive, compact galaxies at redshifts {\$}0.4 \backslashlesssim z \backslashlesssim 0.7{\$}, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of high-redshift red nuggets or their partly-evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar populations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S$\backslash$'ersic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still compact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterised by red-to-blue colour gradients as a function of radius which are stronger at low redshift -- indicative of ongoing accretion -- but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are predominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W and Fassnacht, Christopher D and Treu, Tommaso and Brewer, Brendon J and Koopmans, L V E and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Cao2021, -abstract = {The elliptical power-law model of the mass in a galaxy is widely used in strong gravitational lensing analyses. However, the distribution of mass in real galaxies is more complex. We quantify the biases due to this model mismatch by simulating and then analyzing mock Hubble Space Telescope imaging of lenses with mass distributions inferred from SDSS-MaNGA stellar dynamics data. We find accurate recovery of source galaxy morphology, except for a slight tendency to infer sources to be more compact than their true size. The Einstein radius of the lens is also robustly recovered with 0.1% accuracy, as is the global density slope, with 2.5% relative systematic error, compared to the 3.4% intrinsic dispersion. However, asymmetry in real lenses also leads to a spurious fitted "external shear"with typical strength 3 ext = 0.015. Furthermore, time delays inferred from lens modeling without measurements of stellar dynamics are typically underestimated by ∼5%. Using such measurements from a sub-sample of 37 lenses would bias measurements of the Hubble constant H 0 by ∼9%. Although this work is based on a particular set of MaNGA galaxies, and the specific value of the detected biases may change for another set of strong lenses, our results strongly suggest the next generation cosmography needs to use more complex lens mass models.}, -archivePrefix = {arXiv}, -arxivId = {2110.14554}, -author = {Cao, Xiaoyue and Li, Ran and Nightingale, J. W. and Massey, Richard and Robertson, Andrew and Frenk, Carlos S. and Amvrosiadis, Aristeidis and Amorisco, Nicola C. and He, Qiuhan and Etherington, Amy and Cole, Shaun and Zhu, Kai}, -doi = {10.1088/1674-4527/ac3f2b}, -eprint = {2110.14554}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Cao2021MangaLenses.pdf:pdf}, -issn = {16744527}, -journal = {Research in Astronomy and Astrophysics}, -keywords = {galaxies: halos,galaxies: structure,gravitational lensing: strong}, -number = {2}, -pages = {30 pp}, -title = {{Systematic Errors Induced by the Elliptical Power-law model in Galaxy-Galaxy Strong Lens Modeling}}, -url = {https://iopscience.iop.org/article/10.1149/1945-7111/ab9a2c/meta}, -volume = {22}, -year = {2022} -} -@article{Rasmussen2016, -author = {Rasmussen, Carl Edward}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rasmussen - 2016 - Factor Graphs and message passing Key concepts.pdf:pdf}, -pages = {1--13}, -title = {{Factor Graphs and message passing Key concepts}}, -year = {2016} -} -@article{Suyu2013, -abstract = {Strong gravitational lenses with measured time delays between the multiple images and models of the lens mass distribution allow a one-step determination of the time-delay distance, and thus a measure of cosmological parameters. We present a blind analysis of the gravitational lens RXJ1131-1231 incorporating (1) the newly measured time delays from COSMOGRAIL, the COSmological MOnitoring of GRAvItational Lenses, (2) archival Hubble Space Telescope imaging of the lens system, (3) a new velocity-dispersion measurement of the lens galaxy of 323 ± 20 km s-1 based on Keck spectroscopy, and (4) a characterization of the line-of-sight structures via observations of the lens' environment and ray tracing through the Millennium Simulation. Our blind analysis is designed to prevent experimenter bias. The joint analysis of the data sets allows a time-delay distance measurement to 6% precision that takes into account all known systematic uncertainties. In combination with the Wilkinson Microwave Anisotropy Probe seven-year (WMAP7) data set in flat wCDM cosmology, our unblinded cosmological constraints for RXJ1131-1231 are H 0 = 80.0-5.7+5.8 km-1 Mpc -1, $\Omega$de = 0.79 ± 0.03, and w = -1.25 -0.21+0.17. We find the results to be statistically consistent with those from the analysis of the gravitational lens B1608+656, permitting us to combine the inferences from these two lenses. The joint constraints from the two lenses and WMAP7 are H0 = 75.2 -4.2+4.4 km-1 Mpc-1, $\Omega$de = 0.76-0.03+0.02, and w = -1.14 0.200.17, and in flat wCDM, and H0 = 73.1 -3.6+2.4 km-1 Mpc-1, $\Omega$$\lambda$ = 0.75-0.02+0.01 and $\Omega$k = 0.003-0.006+0.005 in open $\Lambda$CDM. Time-delay lenses constrain especially tightly the Hubble constant H 0 (5.7% and 4.0% respectively in wCDM and open $\Lambda$CDM) and curvature of the universe. The overall information content is similar to that of Baryon Acoustic Oscillation experiments. Thus, they complement well other cosmological probes, and provide an independent check of unknown systematics. Our measurement of the Hubble constant is completely independent of those based on the local distance ladder method, providing an important consistency check of the standard cosmological model and of general relativity. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1208.6010}, -author = {Suyu, S. H. and Auger, M. W. and Hilbert, S. and Marshall, P. J. and Tewes, M. and Treu, T. and Fassnacht, C. D. and Koopmans, L. V.E. and Sluse, D. and Blandford, R. D. and Courbin, F. and Meylan, G.}, -doi = {10.1088/0004-637X/766/2/70}, -eprint = {1208.6010}, -issn = {15384357}, -journal = {ApJ}, -keywords = {distance scale,galaxies: individual (RXJ1131-1231),gravitational lensing: strong,methods: data analysis}, -number = {2}, -pages = {70}, -title = {{Two accurate time-delay distances from strong lensing: Implications for cosmology}}, -url = {http://stacks.iop.org/0004-637X/766/i=2/a=70?key=crossref.276b0a78f87c1d8698f0d90040ee5e57}, -volume = {766}, -year = {2013} -} -@article{Hoekstra2004, -abstract = {We present the results of a study of weak lensing by galaxies based on 45.5 deg$^2$ of $R_C$ band imaging data from the Red-Sequence Cluster Survey (RCS). We present the first weak lensing detection of the flattening of galaxy dark matter halos. We use a simple model in which the ellipticity of the halo is $f$ times the observed ellipticity of the lens. We find a best fit value of $f=0.77^{+0.18}_{-0.21}$, suggesting that the dark matter halos are somewhat rounder than the light distribution. The fact that we detect a significant flattening implies that the halos are well aligned with the light distribution. Given the average ellipticity of the lenses, this implies a halo ellipticity of $=0.33^{+0.07}_{-0.09}$, in fair agreement with results from numerical simulations of CDM. This result provides strong support for the existence of dark matter, as an isotropic lensing signal is excluded with 99.5% confidence. We also study the average mass profile around the lenses, using a maximum likelihood analysis. We consider two models for the halo mass profile: a truncated isothermal sphere (TIS) and an NFW profile. We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo. The best fit NFW model yields a mass $M_{200}=(8.4\pm0.7\pm0.4)\times 10^{11} h^{-1} M_\odot$ and a scale radius $r_s=16.2^{+3.6}_{-2.9} h^{-1}$ kpc. This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, H. K. C. and Gladders, Michael D.}, -doi = {10.1086/382726}, -eprint = {0306515}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hoekstra, Yee, Gladders - 2004 - Properties of Galaxy Dark Matter Halos from Weak Lensing.pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of Galaxy Dark Matter Halos from Weak Lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2004} -} -@article{Hall2014a, -abstract = {Charge-Coupled Devices are the detector of choice for the focal planes of many optical and X-ray space telescopes. In recent years, EM-CCDs, SCDs and CMOS sensors have been used, or baselined, for missions in which the detection of X-ray and visible photons are key to the science goals of the mission. When placed in orbit, silicon-based detectors will suffer radiation damage as a consequence of the harsh space radiation environment, creating traps in the silicon. The radiation-induced traps will capture and release signal electrons, effectively "smearing" the image. Without correction, this smearing of the image would have major consequences on the science goals of the missions. Fitting to observed results, through careful planning of observation strategies while the radiation dose received remains low in the early stages of the mission, has previously been used to correct against the radiation damage effects. As the science goals becoming increasingly demanding, however, the correction algorithms require greater accuracy and a more physical approach is required, removing the effects of the radiation damage by modelling the trap capture and release mechanisms to a high level of detail. The drive for increasingly accurate trap parameters has led to the development of new methods of characterisation of traps in the silicon, measuring the trap properties and their effects to the single-trap level in situ. Here, we summarise the latest developments in trap characterisation techniques for n-channel and p-channel devices. ? 2014 SPIE.}, -author = {Hall, David J. and Murray, Neil and Gow, Jason and Wood, Daniel and Holland, Andrew}, -doi = {10.1117/12.2055906}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hall et al. - 2014 - In situ trap parameter studies in CCDs for space applications.pdf:pdf}, -isbn = {9780819496225}, -issn = {0277-786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VI}, -keywords = {CTI,Defect,Euclid,Gaia,HST,N-channel,P,[CCD}, -number = {0}, -pages = {915408}, -title = {{ In situ trap parameter studies in CCDs for space applications }}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2055906}, -volume = {9154}, -year = {2014} -} -@article{Rogers2019, -abstract = {In contrast to the converging, achromatic behaviour of axisymmetric gravitational lenses, diverging frequency-dependent lensing occurs from refraction due to a distribution of overdense axisymmetric plasma along an observer's line of sight. Such plasma lenses are particularly interesting from the point of view of astronomical observations because they can both magnify and dim the appearance of background sources as a function of frequency. Plasma lensing is believed to be involved in a number of separate phenomena involving the scintillation of radio pulsars, extreme scattering events of background radio sources, and may also play a role in the generation of fast radio bursts. These lensing phenomena are believed to occur in dense environments, in which there may be many density perturbations between an observer and background source. In this work we generalize individual plasma lens models to produce dual-component lenses using families of plasma lens models previously studied in the literature, namely the exponential and softened power-law lenses. Similar to binary gravitational lens models, these dual-component plasma lenses feature a rich and complex critical and caustic morphology, as well as generate more complicated light curves. We map the number of criticals formed for a given component separation and angular size, and highlight a relevant degeneracy between two particular models. This work provides an argument in favour of close monitoring of extreme scattering events in progress in order to break such model degeneracies.}, -archivePrefix = {arXiv}, -arxivId = {1903.06384}, -author = {Rogers, Adam and Er, Xinzhong}, -doi = {10.1093/mnras/stz744}, -eprint = {1903.06384}, -file = {:C\:/Users/Jammy/Documents/Papers/FRBLenses/Rogers2018DustCompPlasmaLenses.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {gravitational lensing: micro,gravitational lensing: strong,plasmas,pulsars: general}, -number = {4}, -pages = {5800--5816}, -title = {{Dual-component plasma lens models}}, -volume = {485}, -year = {2019} -} -@article{Yang2019b, -abstract = {Using the Atacama Large Millimeter/submillimeter Array (ALMA), we report high angular-resolution observations of the redshift z = 3.63 galaxy H-ATLAS J083051.0+013224 (G09v1.97), one of the most luminous strongly lensed galaxies discovered by the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). We present 0.″2-0.″4 resolution images of the rest-frame 188 and 419 $\mu$m dust continuum and the CO(6-5), H2O(211-202), and Jup = 2 H2O+ line emission. We also report the detection of H2O(211-202) in this source. The dust continuum and molecular gas emission are resolved into a nearly complete ∼1.″5 diameter Einstein ring plus a weaker image in the center, which is caused by a special dual deflector lensing configuration. The observed line profiles of the CO(6-5), H2O(211-202), and Jup = 2 H2O+ lines are strikingly similar. In the source plane, we reconstruct the dust continuum images and the spectral cubes of the CO, H2O, and H2O+ line emission at sub-kiloparsec scales. The reconstructed dust emission in the source plane is dominated by a compact disk with an effective radius of 0.7 ± 0.1 kpc plus an overlapping extended disk with a radius twice as large. While the average magnification for the dust continuum is $\mu$ ∼ 10-11, the magnification of the line emission varies from 5 to 22 across different velocity components. The line emission of CO(6-5), H2O(211-202), and H2O+ have similar spatial and kinematic distributions. The molecular gas and dust content reveal that G09v1.97 is a gas-rich major merger in its pre-coalescence phase, with a total molecular gas mass of ∼1011 M. Both of the merging companions are intrinsically ultra-luminous infrared galaxies (ULIRGs) with infrared luminosities LIR reaching 4 × 1012 L, and the total LIR of G09v1.97 is (1.4 ± 0.7)×1013 L. The approaching southern galaxy (dominating from V = -400 to -150 km s-1 relative to the systemic velocity) shows no obvious kinematic structure with a semi-major half-light radius of as = 0.4 kpc, while the receding galaxy (0 to 350 km s-1) resembles an as = 1.2 kpc rotating disk. The two galaxies are separated by a projected distance of 1.3 kpc, bridged by weak line emission (-150 to 0 km s-1) that is co-spatially located with the cold dust emission peak, suggesting a large amount of cold interstellar medium (ISM) in the interacting region. As one of the most luminous star-forming dusty high-redshift galaxies, G09v1.97 is an exceptional source for understanding the ISM in gas-rich starbursting major merging systems at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {1903.00273}, -author = {Yang, C and Gavazzi, R and Beelen, A and Cox, P and Omont, A and Lehnert, M D and Gao, Y and Ivison, R J and Swinbank, A M and Barcos-Mu{\~{n}}oz, L and Neri, R and Cooray, A and Dye, S and Eales, S and Fu, H and Gonz{\'{a}}lez-Alfonso, E and Ibar, E and Micha{\l}owski, M J and Nayyeri, H and Negrello, M and Nightingale, J and P{\'{e}}rez-Fournon, I and Riechers, D A and Smail, I and {Van Der Werf}, P}, -doi = {10.1051/0004-6361/201833876}, -eprint = {1903.00273}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: ISM,Galaxies: high-redshift,Gravitational lensing: strong,ISM: molecules,Radio lines: ISM,Submillimeter: galaxies}, -title = {{CO, H2O, H2O+ line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales}}, -volume = {624}, -year = {2019} -} -@article{Lauer2005, -abstract = {We present observations of 77 early-type galaxies imaged with the PC1 CCD of the Hubble Space Telescope (HST) WFPC2. "Nuker-law" parametric fits to the surface brightness profiles are used to classify the central structure into "core" or "power-law" forms. Core galaxies are typically rounder than power-law galaxies. Nearly all power-law galaxies with central ellipticities $\epsilon$ ≥ 0.3 have stellar disks, implying that disks are present in power-law galaxies with $\epsilon$ {\textless} 0.3 but are not visible because of unfavorable geometry. A few low-luminosity flattened core galaxies also have disks; these may be transition forms from power-law galaxies to more luminous core galaxies, which lack disks. Several core galaxies have strong isophote twists interior to their break radii, although power-law galaxies have interior twists of similar physical significance when the photometric perturbations implied by the twists are evaluated. Central color gradients are typically consistent with the envelope gradients; core galaxies have somewhat weaker color gradients than power-law galaxies. Nuclei are found in 29{\%} of the core galaxies and 60{\%} of the power-law galaxies. Nuclei are typically bluer than the surrounding galaxy. While some nuclei are associated with active galactic nuclei (AGNs), just as many are not; conversely, not all galaxies known to have a low-level AGN exhibit detectable nuclei in the broadband filters. NGC 4073 and 4382 are found to have central minima in their intrinsic starlight distributions; NGC 4382 resembles the double nucleus of M31. In general, the peak brightness location is coincident with the photocenter of the core to a typical physical scale of {\textless} 1 pc. Five galaxies, however, have centers significantly displaced from their surrounding cores; these may be unresolved asymmetric double nuclei. Finally, as noted by previous authors, central dust is visible in about half of the galaxies. The presence and strength of dust correlates with nuclear emission; thus, dust may outline gas that is falling into the central black hole. The prevalence of dust and its morphology suggest that dust clouds form, settle to the center, and disappear repeatedly on ∼ 10 8 yr timescales. We discuss the hypothesis that cores are created by the decay of a massive black hole binary formed in a merger. Apart from their brightness profiles, there are no strong differences between core galaxies and power-law galaxies that demand this scenario; however, the rounder shapes of core, their lack of disks, and their reduced color gradients may be consistent with it. {\textcopyright}2005. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0412040}, -author = {Lauer, Tod R and Faber, S M and Gebhardt, Karl and Richstone, Douglas and Tremaine, Scott and Ajhar, Edward A and Aller, M C and Bender, Ralf and Dressler, Alan and Filippenko, Alexei V and Green, Richard and Grillmair, Carl J and Ho, Luis C and Kormendy, John and Magorrian, John and Pinkney, Jason and Siopis, Christos}, -doi = {10.1086/429565}, -eprint = {0412040}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2138--2185}, -primaryClass = {arXiv:astro-ph}, -title = {{ The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry }}, -url = {http://stacks.iop.org/1538-3881/129/i=5/a=2138}, -volume = {129}, -year = {2005} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}}, host galaxy Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {00160032}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -pages = {1--7}, -title = {{Spatially Resolved Patchy Lyman-{\$}\backslashbackslashalpha{\{}\backslash{\$}{\}} Emission Within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8}}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -year = {2017} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of {\$\sim${}}1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Suyu2010, -abstract = {Strong gravitational lens systems with measured time delays between the multiple images provide a method for measuring the "time-delay distance" to the lens, and thus the Hubble constant. We present a Bayesian analysis of the strong gravitational lens system B1608+656, incorporating (1) new, deep Hubble Space Telescope (HST) observations, (2) a new velocity-dispersion measurement of 260 ± 15 km s-1 for the primary lens galaxy, and (3) an updated study of the lens' environment. Our analysis of the HST images takes into account the extended source surface brightness, and the dust extinction and optical emission by the interacting lens galaxies. When modeling the stellar dynamics of the primary lens galaxy, the lensing effect, and the environment of the lens, we explicitly include the total mass distribution profile logarithmic slope $\gamma$′ and the external convergence $\kappa$ext; we marginalize over these parameters, assigning well-motivated priors for them, and so turn the major systematic errors into statistical ones. The HST images provide one such prior, constraining the lens mass density profile logarithmic slope to be $\gamma$′ = 2.08 ± 0.03; a combination of numerical simulations and photometric observations of the B1608+656 field provides an estimate of the prior for $\kappa$ext: 0.10+0.08-0.05. This latter distribution dominates the final uncertainty on H 0. Fixing the cosmological parameters at $\Omega$m = 0.3, $\Omega$ $\Lambda$ = 0.7, and w = -1 in order to compare with previous work on this system, we find H 0 = 70.6+3.1-3.1 km s-1 Mpc-1. The new data provide an increase in precision of more than a factor of 2, even including the marginalization over $\kappa$ext. Relaxing the prior probability density function for the cosmological parameters to that derived from the Wilkinson Microwave Anisotropy Probe (WMAP) five-year data set, we find that the B1608+656 data set breaks the degeneracy between $\Omega$m and $\Omega$$\Lambda$ at w = -1 and constrains the curvature parameter to be -0.031 < $\Omega$k < 0.009 (95% CL), a level of precision comparable to that afforded by the current Type Ia SNe sample. Asserting a flat spatial geometry, we find that, in combination with WMAP, H 0 = 69.7+4.9-5.0 km s-1 Mpc-1 and w = -0.94+0.17-0.19 (68% CL), suggesting that the observations of B1608+656 constrain w as tightly as the current Baryon Acoustic Oscillation data do. {\textcopyright} 2010 The American Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {0910.2773}, -author = {Suyu, S. H. and Marshall, P. J. and Auger, M. W. and Hilbert, S. and Blandford, R. D. and Koopmans, L. V.E. and Fassnacht, C. D. and Treu, T.}, -doi = {10.1088/0004-637X/711/1/201}, -eprint = {0910.2773}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Suyu2009SpiralPotentialCorr.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {Cosmology: observations,Distance scale,Gravitational lensing: Strong,Methods: data analysis}, -number = {1}, -pages = {201--221}, -title = {{Dissecting the gravitational lens B1608+656. II. Precision measurements of the hubble constant, spatial curvature, and the dark energy equation of state}}, -volume = {711}, -year = {2010} -} -@article{Geometryed, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Murray2013, -abstract = {A multi-level clocking scheme has been developed to improve the parallel CTE of four-phase CCDs by suppressing the effects of traps located in the transport channel under barrier phases by inverting one of these phases throughout the transfer sequence. In parallel it was apparent that persistence following optical overload in Euclid VIS detectors would lead to undesirable signal released in subsequent rows and frames and that a suitable scheme for flushing this signal would be required. With care, the negatively biased electrodes during the multi-level transfer sequence can be made to pin the entire surface, row-by-row, and annihilate the problematic charges. This process can also be extended for use during integration to significantly reduce the unusable area of the detector, as per the clocked anti-blooming techniques developed many years ago; however, with the four-phase electrodes architecture of modern CCDs, we can take precautionary measures to avoid the problem of charge pumping and clock induced charge within the science frames. Clock induced charge is not all bad! We also propose the use of on-orbit trap-pumping for Euclid VIS to provide calibration input to ground based correction algorithms and as such a uniform, low noise background is require. Clock induced charge can be manipulated to provide a very suitable, low signal and noise background to the imaging array. Here we describe and present results of multi-level parallel clocking schemes for use in four-phase CCDs that could improve performance of high precision astronomy applications such as Euclid VIS. ? 2013 SPIE.}, -author = {Murray, Neil J and Burt, David J and Holland, Andrew D and Stefanov, Konstantin D and Gow, Jason P D and MacCormick, Calum and Dryer, Ben J and Allanwood, Edgar A H}, -doi = {10.1117/12.2024839}, -isbn = {9780819497109}, -issn = {0277786X 1996756X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {Blooming,CAB,CCD,CIC,CTE,Euclid VIS,Mu,[BFW}, -pages = {88600K}, -title = {{Multi-level parallel clocking of CCDs for: improving charge transfer efficiency, clearing persistence, clocked anti-blooming, and generating low-noise backgrounds for pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024839}, -volume = {8860}, -year = {2013} -} -@article{Lipnicky2018, -abstract = {We reportHI observations of eight spiral galaxies that are strongly lensing background sources. Our targets were selected from the Sloan WFC (Wide Field Camera) Edge-on Late-type Lens Survey (SWELLS) using the Arecibo, Karl G. Jansky Very Large Array, and Green Bank telescopes. We securely detect J1703+2451 at z = 0.063 with a signal-to-noise ratio of 6.7 and W50 = 79 ± 13 km s-1, obtaining the first detection of HI emission in a strong spiral lens. We measure a mass of MHI = (1.77 ± 0.06 -0.75+0.35) × 109M⊙ for this source. We find that this lens is a normal spiral, with observable properties that are fairly typical of spiral galaxies. For three other sources, we did not secure a detection; however, we are able to place strong constraints on the HI masses of those galaxies. The observations for four of our sources were rendered unusable due to strong radio frequency interference.}, -archivePrefix = {arXiv}, -arxivId = {1802.01588}, -author = {Lipnicky, Andrew and Chakrabarti, Sukanya and Wright, Melvyn C H and Blitz, Leo and Heiles, Carl and Cotton, William and Frayer, David and Blandford, Roger and Shu, Yiping and Bolton, Adam S}, -doi = {10.1093/mnras/sty326}, -eprint = {1802.01588}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Radio lines: galaxies}, -number = {3}, -pages = {3097--3105}, -title = {{The first detection of neutral hydrogen in emission in a strong spiral lens}}, -url = {http://arxiv.org/abs/1802.01588%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty326}, -volume = {476}, -year = {2018} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright} 2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel, Sari, Ceverino - 2009 - Formation of massive galaxies at high redshift Cold streams, clumpy disks, and compact spheroids(2).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Cohen2024, -abstract = {The flux ratios of strongly lensed quasars have previously been used to infer the properties of dark matter. In these analyses it is crucial to separate the effect of the main lensing galaxy and the low-mass dark matter halo population. In this work, we investigate flux-ratio perturbations resulting from general third- and fourth-order multipole perturbations to the main lensing galaxy's mass profile. We simulate four lens systems, each with a different lensing configuration, without multipoles. The simulated flux ratios are perturbed by 10-40 per cent by a population of low-mass haloes consistent with CDM and, in one case, also a satellite galaxy. This level of perturbation is comparable to the magnitude of flux-ratio anomalies in real data that has been previously analyzed. We then attempt to fit the simulated systems using multipoles instead of low-mass haloes. We find that multipoles with amplitudes of 0.01 or less can produce flux-ratio perturbations in excess of 40 per cent. In all cases, third- or fourth-order multipoles can individually reduce the magnitude of, if not eliminate, flux-ratio anomalies. When both multipole orders are jointly included, all simulated flux ratios can be fit to within the observational uncertainty. Our results indicate that low-mass haloes and multipoles are highly degenerate when modelling quadruply-imaged quasars based just on image positions and flux ratios. In the presence of this degeneracy, flux-ratio anomalies in lensed quasars alone cannot be used to place strong constraints on the properties of dark matter without additional information that can inform our priors.}, -archivePrefix = {arXiv}, -arxivId = {2403.08895}, -author = {Cohen, Jacob S. and Fassnacht, Christopher D. and O'Riordan, Conor M. and Vegetti, Simona}, -eprint = {2403.08895}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Cohen2024Multipoles.pdf:pdf}, -journal = {arxiv.org:2403.08895}, -keywords = {dark matter,galaxies,gravitational lensing,strong,structure}, -number = {March}, -pages = {1--13}, -title = {{General Multipoles and Their Implications for Dark Matter Inference}}, -url = {http://arxiv.org/abs/2403.08895}, -volume = {13}, -year = {2024} -} -@article{Eales1999, -abstract = {We present the first results of a deep unbiased submillimeter survey carried out at 450 and 850 $\mu$m. We detected 12 sources at 850 $\mu$m at greater than the 3 $\sigma$ level, giving a surface density of sources with S850$\mu$m{\textgreater}2.8 mJy of 0.49 ± 0.16 arcmin-2. If replicated over the sky, our sources would generate a background at 850 $\mu$m of 9.6 × 10−11 W m-2 sr-1, which is sime20{\%} of the value measured by the Far-Infrared Absolute Spectrophotometer (FIRAS) and a significant fraction of the total background radiation produced by stars. This implies, through the connection between metallicity and background radiation, that a significant fraction of all the stars that have ever been formed were formed in objects like those detected here. The combination of their large contribution to the background radiation and their extreme bolometric luminosities makes these objects excellent candidates for being proto-elliptical galaxies. Optical astronomers have recently shown that the UV luminosity density of the universe increases by a factor of sime10 between z=0 and z=1-2 and then decreases again at higher redshifts. Using the results of a parallel submillimeter survey of the local universe, we show that both the submillimeter source density and background radiation (as detected by FIRAS) can be explained if the submillimeter luminosity density evolves in a similar way to the UV luminosity density. Thus, if these sources are elliptical galaxies in the process of formation, they are probably forming at relatively modest redshifts.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9808040}, -author = {Eales, Stephen and Lilly, Simon and Gear, Walter and Dunne, Loretta and Bond, J Richard and Hammer, Francois and {Le Fevre}, Olivier and Crampton, David}, -doi = {10.1086/307069}, -eprint = {9808040}, -isbn = {9780473203641}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {518--524}, -pmid = {17121902}, -primaryClass = {astro-ph}, -title = {{The Canada‐UK Deep Submillimeter Survey: First Submillimeter Images, the Source Counts, and Resolution of the Background}}, -url = {http://stacks.iop.org/0004-637X/515/i=2/a=518}, -volume = {515}, -year = {2002} -} -@article{Lipnicky2018, -abstract = {We reportHI observations of eight spiral galaxies that are strongly lensing background sources. Our targets were selected from the Sloan WFC (Wide Field Camera) Edge-on Late-type Lens Survey (SWELLS) using the Arecibo, Karl G. Jansky Very Large Array, and Green Bank telescopes. We securely detect J1703+2451 at z = 0.063 with a signal-to-noise ratio of 6.7 and W50 = 79 ± 13 km s-1, obtaining the first detection of HI emission in a strong spiral lens. We measure a mass of MHI = (1.77 ± 0.06 -0.75+0.35) × 109M⊙ for this source. We find that this lens is a normal spiral, with observable properties that are fairly typical of spiral galaxies. For three other sources, we did not secure a detection; however, we are able to place strong constraints on the HI masses of those galaxies. The observations for four of our sources were rendered unusable due to strong radio frequency interference.}, -archivePrefix = {arXiv}, -arxivId = {1802.01588}, -author = {Lipnicky, Andrew and Chakrabarti, Sukanya and Wright, Melvyn C.H. and Blitz, Leo and Heiles, Carl and Cotton, William and Frayer, David and Blandford, Roger and Shu, Yiping and Bolton, Adam S.}, -doi = {10.1093/mnras/sty326}, -eprint = {1802.01588}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lipnicky et al. - 2018 - The first detection of neutral hydrogen in emission in a strong spiral lens(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Radio lines: galaxies}, -number = {3}, -pages = {3097--3105}, -title = {{The first detection of neutral hydrogen in emission in a strong spiral lens}}, -url = {http://arxiv.org/abs/1802.01588%0Ahttp://dx.doi.org/10.1093/mnras/sty326}, -volume = {476}, -year = {2018} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high-resolution N-body simulations of galactic dark matter haloes to test if this remarkable property can be understood within the context of the cold dark matter (CDM) cosmology. We construct halo merger trees from the simulations and use a semi-analytic model to follow the formation of satellite galaxies. We find that in all six of our simulations, the 11 brightest satellites are indeed distributed along thin, disc-like structures analogous to that traced by the satellites of the Milky Way. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhaloes within it, which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhaloes but is similar to that of the subset of subhaloes that had the most massive progenitors at earlier times. The elongated disc-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I and Frenk, Carlos S and Cole, Shaun and Helly, John C and Jenkins, Adrian and Navarro, Julio F and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Goulding2016a, -abstract = {Studies of the physical properties of local elliptical galaxies (e.g., gas temperatures, halo masses, stellar kinematics) are shedding new light on galaxy formation. Here we present the hot X-ray gas properties of 33 early-type systems within the MASSIVE galaxy survey sample that have archival Chandra X-ray observations. Through careful X-ray spectral modeling, we derive X-ray luminosities (L_X) and plasma temperatures (T_gas) for the diffuse gas components in these galaxies. We combine the MASSIVE sample with 41 galaxies from the ATLAS^3D survey to investigate the X-ray and optical properties of a statistically significant sample of nearby early-type galaxies across a wide-range of environments. We deduce that all early-type galaxies (independent of galaxy mass and rotational support) follow a universal scaling law such that L_X$\sim$T_gas^4.5. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, the wide-scale environment does not contribute to the intrinsic scatter ($\sim$0.5dex) within the scaling relation. We further demonstrate that the scatter in L_X around both K-band luminosity (L_K) and the galaxy stellar velocity dispersion is primarily driven by T_gas, with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the origin of the gas directly to either the stellar mass or the galaxy potential. Indeed, our data require a steeper relation between L_X, L_K, and sigma_e than predicted by standard mass-loss models. Finally, we find a statistically significant correlation between sigma_e and T_gas, suggesting that T_gas is set by the galaxy potential inside the optical effective radius. We conclude that within the inner-most 10-30kpc region, early-types maintain pressure-supported hot gas, with a minimum T_gas set by the virial temperature, but the majority show evidence for some additional heating.}, -archivePrefix = {arXiv}, -arxivId = {1604.01764}, -author = {Goulding, Andy D. and Greene, Jenny E. and Ma, Chung-Pei and Veale, Melanie and Bogdan, Akos and Nyland, Kristina and Blakeslee, John P. and McConnell, Nicholas J. and Thomas, Jens}, -doi = {10.3847/0004-637x/826/2/167}, -eprint = {1604.01764}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Goulding et al. - 2016 - the Massive Survey. Iv. the X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {167}, -title = {{the Massive Survey. Iv. the X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe}}, -url = {http://arxiv.org/abs/1604.01764%0Ahttp://dx.doi.org/10.3847/0004-637X/826/2/167}, -volume = {826}, -year = {2016} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{Naab2009, -abstract = {Using a high resolution hydrodynamical cosmological simulation of the formation of a massive spheroidal galaxy we show that elliptical galaxies can be very compact and massive at high redshift in agreement with recent observations. Accretion of stripped in-falling stellar material increases the size of the system with time and the central concentration is reduced by dynamical friction of the surviving stellar cores. In a specific case of a spheroidal galaxy with a final stellar mass of {\$}1.5 \backslashtimes 10{\^{}}{\{}11{\}} M{\_}{\{}\backslashodot{\}}{\$} we find that the effective radius {\$}r{\_}e{\$} increases from {\$}0.7 \backslashpm 0.2 \backslashrm kpc{\$} at z = 3 to {\$}r{\_}e = 2.4 \backslashpm 0.4 \backslashrm kpc{\$} at z = 0 with a concomitant decrease in the effective density of an order of magnitude and a decrease of the central velocity dispersion by approximately 20{\%} over this time interval. A simple argument based on the virial theorem shows that during the accretion of weakly bound material (minor mergers) the radius can increase as the square of the mass in contrast to the usual linear rate of increase for major mergers. By undergoing minor mergers compact high redshift spheroids can evolve into present-day systems with sizes and concentrations similar to observed local ellipticals. This indicates that minor mergers may be the main driver for the late evolution of sizes and densities of early-type galaxies.}, -archivePrefix = {arXiv}, -arxivId = {0903.1636}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P}, -doi = {10.1088/0004-637X/699/2/L178}, -eprint = {0903.1636}, -issn = {2041-821}, -journal = {Astrophysical Journal Letters}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: interactions,Galaxies: structure,Methods: numerical,cd}, -month = {jul}, -number = {2 PART 2}, -pages = {L178----L182}, -title = {{Minor mergers and the size evolution of elliptical galaxies}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L178?key=crossref.405faa44137f4be9a7e3800a4c3e7dea}, -volume = {699}, -year = {2010} -} -@article{Salvatier2016, -abstract = {Probabilistic programming allows for automatic Bayesian inference on user-defined probabilistic models. Recent advances in Markov chain Monte Carlo (MCMC) sampling allow inference on increasingly complex models. This class of MCMC, known as Hamiltonian Monte Carlo, requires gradient information which is often not readily available. PyMC3 is a new open source probabilistic programming framework written in Python that uses Theano to compute gradients via automatic differentiation as well as compile probabilistic programs on-the-fly to C for increased speed. Contrary to other probabilistic programming languages, PyMC3 allows model specification directly in Python code. The lack of a domain specific language allows for great flexibility and direct interaction with the model. This paper is a tutorial-style introduction to this software package.}, -archivePrefix = {arXiv}, -arxivId = {1507.08050}, -author = {Salvatier, John and Wiecki, Thomas V. and Fonnesbeck, Christopher}, -doi = {10.7717/peerj-cs.55}, -eprint = {1507.08050}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Salvatier, Wiecki, Fonnesbeck - 2016 - Probabilistic programming in Python using PyMC3.pdf:pdf}, -issn = {23765992}, -journal = {PeerJ Computer Science}, -keywords = {Bayesian statistic,Markov chain Monte Carlo,Probabilistic Programming,Python,Statistical modeling}, -number = {4}, -pages = {1--24}, -title = {{Probabilistic programming in Python using PyMC3}}, -volume = {2016}, -year = {2016} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified {\$\sim${}}17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M {\textless}10{\^{}}9 M*), low-metallicity (Z{\$\sim${}}1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He {\$}\backslash{\$}ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A and Erb, Dawn K and Auger, Matthew W and Pettini, Max and Brammer, Gabriel B}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -isbn = {0004-637X}, -issn = {15384357}, -pages = {1--28}, -title = {{A Window On The Earliest Star Formation: Extreme Photoionization Conditions of a High-Ionization, Low-Metallicity Lensed Galaxy at z{\$\sim${}}2}}, -url = {http://arxiv.org/abs/1803.02340}, -year = {2018} -} -@article{Keeton1997, -abstract = {Galaxies modeled as singular isothermal ellipsoids with an axis ratio distribution similar to the observed axis ratio distribution of E and S0 galaxies are statistically consistent with both the observed numbers of two-image and four-image lenses and the inferred ellipticities of individual lenses. However, no four-image lens is well fit by the model (typical $\chi^2/N_{dof} \sim 20$), the axis ratio of the model can be significantly different from that of the observed lens galaxy, and the major axes of the model and the galaxy may be slightly misaligned. We found that models with a second, independent, external shear axis could fit the data well (typical $\chi^2/N_{dof} \sim 1$), while adding the same number of extra parameters to the radial mass distribution does not produce such a dramatic improvement in the fit. An independent shear axis can be produced by misalignments between the luminous galaxy and its dark matter halo, or by external shear perturbations due to galaxies and clusters correlated with the primary lens or along the line of sight. We estimate that the external shear perturbations have no significant effect on the expected numbers of two-image and four-image lenses, but that they can be important perturbations in individual lens models. However, the amplitudes of the external shears required to produce the good fits are larger than our estimates for typical external shear perturbations (10-15% shear instead of 1-3% shear) suggesting that the origin of the extra angular structure must be intrinsic to the primary lens galaxy in most cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9610163}, -author = {Keeton, C. R. and Kochanek, C. S. and Seljak, U.}, -doi = {10.1086/304172}, -eprint = {9610163}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Keeton, Kochanek, Seljak - 1997 - Shear and Ellipticity in Gravitational Lenses(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING,Galaxies: Elliptical and Lenticular,cD,cosmology: theory}, -number = {2}, -pages = {604--620}, -primaryClass = {astro-ph}, -title = {{Shear and Ellipticity in Gravitational Lenses}}, -url = {http://arxiv.org/abs/astro-ph/9610163%0Ahttp://dx.doi.org/10.1086/304172}, -volume = {482}, -year = {1997} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centres of typical {\$\sim${}} L* and lower mass spheroids exhibit power-law 'cusps' with $\Sigma$ $\alpha$ R-$\eta$, where 0.5 ≲ $\eta$ ≲ 1 for radii {\$\sim${}} 1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for, or strongly modify, the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m = 1 lopsided/eccentric disc instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*({\textless} R) « MBH. When the stellar surface density profile is comparatively shallow with $\eta$ {\textless} 1/2, the modes cannot efficiently propagate to R = 0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than $\eta$ = 1, the inward propagation of eccentricity is strongly damped, suppressing inflow and bringing $\eta$ down again. Together these results produce an equilibrium slope of 1/2 ≲ $\eta$ ≲ 1 in the potential of the central black hole. These physical arguments are supported by non-linear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies. {\textcopyright}2010 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z > 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G.}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2006 - Breaking the hierarchy of galaxy formation(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Geometryen, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(2).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Murray2013a, -abstract = {Pocket-pumping is an established technique for identifying the locations of charge trapping sites within the transport channels of CCDs. Various parameters of the pumping process can be manipulated to increase the efficiency, or allow characterisation of the trap sites effective during nominal operating modes. A CCD273 was irradiated in a triangular region by protons to a 10 MeV equivalent fluence of 1.2E9 p.cm-2, ensuring a suitably low trap density for the development of an automated trap recognition algorithm. X-rays of 5, 898 eV were incident on the CCD above the region irradiated with the triangle, such that events could be analysed having passed through an increasing length of irradiated silicon and hence number of trapping sites as a function of column number. Here we present the relationship between the number of traps identified by pocket pumping within the parallel transport channels of a CCD273 and the amount of signal that is deferred by the trapping process during readout. {\textcopyright} 2013 SPIE.}, -author = {Murray, Neil J. and Burt, David J. and Hall, David and Holland, Andrew D.}, -doi = {10.1117/12.2024826}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2013 - The relationship between pumped traps and signal loss in buried channel CCDs(2).pdf:pdf}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {ccd,cic,cte,eper,euclid vis,fpr,multi-level,pocket pumping,trap pumping,tri-level}, -number = {0}, -pages = {88600H}, -title = {{The relationship between pumped traps and signal loss in buried channel CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024826}, -volume = {8860}, -year = {2013} -} -@article{Wang2013, -abstract = {We investigate the spatial distribution of galactic satellites in high-resolution simulations of structure formation in the $\Lambda$ cold dark matter ($\Lambda$CDM) model: the Aquarius dark matter simulations of individual haloes and the Millennium-II simulation of a large cosmological volume. To relate the simulations to observations of the Milky Way we use two alternative models to populate dark haloes with `visible' galaxies: a semi-analytic model of galaxy formation and an abundance matching technique. We find that the radial density profile of massive satellites roughly follows that of the dark matter halo (unlike the distribution of dark matter subhaloes). Furthermore, our two galaxy formation models give results consistent with the observed profile of the 11 classical satellites of the Milky Way. Our simulations predict that larger, fainter samples of satellites should still retain this profile at least up to samples of 100 satellites. The angular distribution of the classical satellites of the Milky Way is known to be highly anisotropic. Depending on the exact measure of flattening, 5-10 per cent of satellite systems in our simulations are as flat as the Milky Way's and this fraction does not change when we correct for possible obscuration of satellites by the Galactic disc. A moderate flattening of satellite systems is a general property of $\Lambda$CDM, best understood as the consequence of preferential accretion along filaments of the cosmic web. Accretion of a single rich group of satellites can enhance the flattening due to such anisotropic accretion. We verify that a typical Milky Way-mass cold dark matter halo does not acquire its 11 most massive satellites from a small number of rich groups. Single-group accretion becomes more likely for less massive satellites. Our model predictions should be testable with forthcoming studies of satellite systems in other galaxies and surveys of fainter satellites in the Milky Way.}, -archivePrefix = {arXiv}, -arxivId = {1206.1340}, -author = {Wang, Jie and Frenk, Carlos S and Cooper, Andrew P}, -doi = {10.1093/mnras/sts442}, -eprint = {1206.1340}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxy: formation,Galaxy: structure,Methods: numerical}, -number = {2}, -pages = {1502--1513}, -title = {{The spatial distribution of galactic satellites in the $\Lambda$ cold dark matter cosmology}}, -volume = {429}, -year = {2013} -} -@article{Mendez-Abreu2016, -abstract = {We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the CALIFA Data Release 3. They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i SDSS images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log(Mstar/Msun){\textgreater}11), the galaxy population is dominated by galaxies modelled with a single Sersic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T{\textgreater}0.2. At intermediate masses (9.5{\textless}log(Mstar/Msun){\textless}11), galaxies described with bulge+disc but B/T {\textless} 0.2 are preponderant, whereas, at the low mass end (log(Mstar/Msun){\textless}9.5), the prevailing population is constituted by galaxies modelled with either pure discs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57{\%} of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5{\textless}log(Mstar/Msun){\textless}11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62{\%}, 28{\%}, and 10{\%} for the so-called Type I, Type II, and Type III disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.}, -archivePrefix = {arXiv}, -arxivId = {1610.05324}, -author = {Mendez-Abreu, J and Ruiz-Lara, T and Sanchez-Menguiano, L and de Lorenzo-Caceres, A and Costantin, L and Catalan-Torrecilla, C and Florido, E and Aguerri, J A L and Bland-Hawthorn, J and Corsini, E M and Dettmar, R J and Galbany, L and Garcia-Benito, R and Marino, R A and Marquez, I and Ortega-Minakata, R A and Papaderos, P and Sanchez, S F and Sanchez-Blazquez, P and Spekkens, K and van de Ven, G and Wild, V and Ziegler, B}, -doi = {10.1051/0004-6361/201629525}, -eprint = {1610.05324}, -issn = {0004-6361}, -title = {{Two-dimensional multi-component photometric decomposition of CALIFA galaxies}}, -url = {http://arxiv.org/abs/1610.05324%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201629525}, -year = {2016} -} -@article{Guo:2008aa, -abstract = {We use galaxy and dark halo data from the public database for the Millennium Simulation to study the growth of galaxies in the De Lucia et al. model for galaxy formation. Previous work has shown this model to reproduce many aspects of the systematic properties and the clustering of real galaxies, both in the nearby universe and at high redshift. It assumes the stellar masses of galaxies to increase through three processes, major mergers, the accretion of smaller satellite systems and star formation. We show the relative importance of these three modes to be a strong function of stellar mass and redshift. Galaxy growth through major mergers depends strongly on stellar mass, but only weakly on redshift. Except for massive systems, minor mergers contribute more to galaxy growth than major mergers at all redshifts and stellar masses. For galaxies significantly less massive than the Milky Way, star formation dominates the growth at all epochs. For galaxies significantly more massive than the Milky Way, growth through mergers is the dominant process at all epochs. At a stellar mass of 6 × 1010Msolar, about that of the Milk Way, star formation dominates at z {\textgreater} 1 and mergers at later times. At every stellar mass, the growth rates through star formation increase rapidly with increasing redshift. Specific star formation rates are the decreasing function of stellar mass not only at z = 0 but also at all higher redshifts. For comparison, we carry out a similar analysis of the growth of dark matter haloes. In contrast to the galaxies, growth rates depend strongly on redshift, but only weakly on mass. They agree qualitatively with analytic predictions for halo growth.}, -author = {{Guo, Q.} and {White, S. D. M.}}, -doi = {10.1111/j.1365-2966.2007.12619.x}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: evolution,galaxies: formation,galaxies: high-redshift,galaxies: interactions}, -month = {feb}, -number = {1}, -pages = {2--10}, -title = {{Galaxy growth in the concordance $\Lambda$CDM cosmology}}, -url = {http://adsabs.harvard.edu/abs/2008MNRAS.384....2G}, -volume = {384}, -year = {2008} -} -@article{Spindler2017, -abstract = {We study the spatially resolved star formation of 1494 galaxies in the SDSSIV-MaNGA Survey. SFRs are calculated using a two-step process, using {\$}H{\_}\backslashalpha{\$} in star forming regions and {\$}D{\_}n4000{\$} in regions identified as AGN/LI(N)ER or lineless. The roles of secular and environmental quenching processes are investigated by studying the dependence of the radial profiles of specific star formation rate on stellar mass, galaxy structure and environment. We report on the existence of `Centrally Suppressed' galaxies, which have suppressed SSFR in their cores compared to their disks. The profiles of centrally suppressed and unsuppressed galaxies are distibuted in a bimodal way. Galaxies with high stellar mass and core velocity dispersion are found to be much more likely to be centrally suppressed than low mass galaxies, and we show that this is related to morphology and the presence of AGN/LI(N)ER like emission. Centrally suppressed galaxies also display lower star formation at all radii compared to unsuppressed galaxies. The profiles of central and satellite galaxies are also compared, and we find that satellite galaxies experience lower specific star formation rates at all radii than central galaxies. This uniform suppression could be a signal of the stripping of hot halo gas in the process known as strangulation. We find that satellites are not more likely to be suppressed in their cores than centrals, indicating that the core suppression is an entirely internal process. We find no correlation between the local environment density and the profiles of star formation rate surface density.}, -archivePrefix = {arXiv}, -arxivId = {1710.05049}, -author = {Spindler, Ashley and Wake, David and Belfiore, Francesco and Bershady, Matthew and Bundy, Kevin and Drory, Niv and Masters, Karen and Thomas, Daniel and Westfall, Kyle and Wild, Vivienne}, -doi = {10.1093/mnras/sty247}, -eprint = {1710.05049}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Bulges,Galaxies: Clusters: General,Galaxies: Evolution,Galaxies: Groups: General,Galaxies: Star formation,Galaxies: Structure}, -number = {1}, -pages = {580--600}, -title = {{SDSS-IV MaNGA: The spatial distribution of star formation and its dependence on mass, structure, and environment}}, -url = {http://arxiv.org/abs/1710.05049}, -volume = {476}, -year = {2018} -} -@article{Wang2017, -abstract = {Difference imaging or image subtraction is a method that measures differential photometry by matching the pointing and point-spread function (PSF) between image frames. It is used for the detection of time-variable phenomena. Here we present a new category of method---CPM Difference Imaging, in which differences are not measured between matched images but instead between image frames and a data-driven predictive model that has been designed only to predict the pointing, PSF, and detector effects but not astronomical variability. In CPM Difference Imaging each pixel is modelled by the Causal Pixel Model (CPM) originally built for modeling Kepler data, in which pixel values are predicted by a linear combination of other pixels at the same epoch but far enough away such that these pixels are causally disconnected, astrophysically. It does not require that the user have any explicit model or description of the pointing or point-spread function of any of the images. Its principal drawback is that---in its current form---it requires an imaging campaign with many epochs and fairly stable telescope pointing. The method is applied to simulated data and also the K2 Campaign 9 microlensing data. We show that CPM Difference Imaging can detect variable objects and produce precise differentiate photometry in a crowded field. CPM Difference Imaging is capable of producing image differences at nearly photon-noise precision.}, -archivePrefix = {arXiv}, -arxivId = {1710.02428}, -author = {Wang, Dun and Hogg, David W and Foreman-Mackey, Daniel and Sch{\"{o}}lkopf, Bernhard}, -eprint = {1710.02428}, -pages = {1--23}, -title = {{A pixel-level model for event discovery in time-domain imaging}}, -url = {http://arxiv.org/abs/1710.02428}, -year = {2017} -} -@article{Christensen2014, -abstract = {We present a detailed comparison between the photometric properties of the bulges of two simulated galaxies and those of a uniform sample of observed galaxies. This analysis shows that the simulated galaxies have bulges with realistic surface brightnesses for their sizes and magnitude. These two field disc galaxies have rotational velocities {\$\sim${}} 100 km/s and were integrated to a redshift of zero in a fully cosmological Lambda cold dark matter context as part of high-resolution smoothed particle hydrodynamic simulations. We performed bulge-disc decompositions of the galaxies using artificial observations, in order to conduct a fair comparison to observations. We also dynamically decomposed the galaxies and compared the star formation histories of the bulges to those of the entire galaxies. These star formation histories showed that the bulges were primarily formed before z = 1 and during periods of rapid star formation. Both galaxies have large amounts of early star formation, which is likely related to the relatively high bulge-to-disc ratios also measured for them. Unlike almost all previous cosmological simulations, the realistically concentrated bulges of these galaxies do not lead to unphysically high rotational velocities, causing them to naturally lie along the observed Tully-Fisher relation.}, -archivePrefix = {arXiv}, -arxivId = {1402.2702}, -author = {Christensen, C R and Brooks, A M and Fisher, D B and Governato, F and McCleary, J and Quinn, T R and Shen, S and Wadsley, J}, -doi = {10.1093/mnrasl/slu020}, -eprint = {1402.2702}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Bulges,Formation,Galaxies,Methods,Numerical,Spiral,Structure}, -number = {1}, -pages = {1--6}, -title = {{Simulating disc galaxy bulges that are consistent with observed scaling relations}}, -volume = {440}, -year = {2014} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism, which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio (M/L) and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R, z) and characterized by the classic anisotropy parameter. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters ($\beta$z and the inclination), the models generally provide remarkably good descriptions of the shape of the first (V) and second () velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the dynamical structure of these objects. With the observationally motivated assumption that $\beta$z ≳ 0, the method is able to recover the inclination. The technique can be used to determine the dynamical M/L and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modelling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy and multiple kinematic components. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Xie:2015aa, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -month = {feb}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Mazzali2003, -author = {Journal, The Astrophysical}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Edge2003Abell1201.pdf:pdf}, -pages = {10--13}, -title = {{The Astrophysical Journal , 599:L5–L8, 2003 December 10 ᭧ 2003.}}, -year = {2003} -} -@article{Siverd2009, -abstract = {We identify, categorize, and quantify alignment effects among host and satellite galaxies using a spectroscopically-confirmed, low-redshift (z{\textless}0.23) galaxy sample from the Sloan Digital Sky Survey Data Release 6. Consistent with other recent findings, we find that satellite galaxies (SGs) of red, centrally concentrated (elliptical) host galaxies (HGs) with radial velocity separation |Delta{\_}V|{\textless}600 km/s preferentially reside near the projected major axes of their HGs. Among these, this preference is strongest for highly concentrated, red SGs. We find that fractional anisotropy increases with decreasing $\backslash$Delta{\_}V and Delta{\_}R and is nearly 40{\%} greater among the closest SGs (Delta{\_}R{\textless}250 kpc/h) relative to more distant (Delta{\_}R{\textgreater}500 kpc/h) SGs. For highly concentrated SGs at small ({\textless}300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to {\textless}15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby ({\textless}40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ({\$\sim${}}3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R J and Ryden, B S and Gaudi, B S}, -eprint = {0903.2264}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@article{Tenneti2016, -abstract = {We study the shapes and intrinsic alignments of discs and elliptical galaxies in the MassiveBlack-II (MBII) and Illustris cosmological hydrodynamic simulations, with volumes of (100 h-1 Mpc)3and (75 h-1 Mpc)3, respectively. We find that simulated disc galaxies are more oblate in shape and more misaligned with the shape of their host dark matter subhalo when compared with ellipticals. The discmajor axis is found to be oriented towards the location of nearby elliptical galaxies. We also find that the discs are thinner in MBII and misalignments with dark matter halo orientations are smaller in both discs and ellipticals when compared with Illustris. As a result, the intrinsic alignment correlation functions at fixed mass have a higher amplitude in MBII than in Illustris. Finally, at scales above $\sim$0.1 h-1 Mpc, the intrinsic alignment two-point correlation functions for disc galaxies in both simulations are consistent with a null detection, unlike those for ellipticals. Despite significant differences in the treatments of hydrodynamics and baryonic physics in the simulations, we find that the w$\delta$ + correlation function scales similarly with transverse separation. However, the less massive galaxies show different scale dependence in the ellipticity-direction correlation. This result indicates that, while hydrodynamic simulations are a promising tool to study intrinsic alignments, further study is needed to understand the impact of differences in the implementations of hydrodynamics and baryonic feedback.}, -archivePrefix = {arXiv}, -arxivId = {1510.07024}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana}, -doi = {10.1093/mnras/stw1823}, -eprint = {1510.07024}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tenneti, Mandelbaum, Di Matteo - 2016 - Intrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris sim(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies,Gravitational lensing: weak,Hydrodynamics,Kinematics and dynamics,Methods,Numerical}, -number = {3}, -pages = {2668--2680}, -title = {{Intrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris simulations}}, -volume = {462}, -year = {2016} -} -@article{Falco1985, -abstract = {The images of a background source formed by a foreground mass $\backslash$ndistribution in a matter-dominated Friedmann cosmology are considered. A $\backslash$ntransformation is presented that leaves unchanged the image observables, $\backslash$nincluding positions, relative magnifications, apparent luminosities, and $\backslash$ndifferences in propagation times associated with image pairs. The $\backslash$nobservables are related to the parameters of the source and of a $\backslash$ngeneralized lens model. The transformation is applied to these relations $\backslash$nto scale the value of H(0) and to modify the mass distribution of the $\backslash$nlens and move the position of the source. One lens model for Q0957 + 561 }, -author = {Falco, E E and Gorenstein, M V and Shapiro, I I}, -doi = {10.1086/184422}, -isbn = {9781416033431}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {ASTRONOMICAL MODELS,Background Radiation,GALACTIC CLUSTERS,Geometrical Optics,Gravitational Lenses,Hubble Diagram,MASS DISTRIBUTION,Quasars,Radiation Sources}, -pages = {L1}, -title = {{On model-dependent bounds on H(0) from gravitational images Application of Q0957 + 561A,B}}, -url = {http://adsabs.harvard.edu/doi/10.1086/184422}, -volume = {289}, -year = {2002} -} -@article{Seabroke2013, -abstract = {The European Space Agency (ESA) Gaia satellite has 106 CCD image sensors which will suffer from increased charge transfer inefficiency (CTI) as a result of radiation damage. To aid the mitigation at low signal levels, the CCD design includes supplementary buried channels (SBCs, otherwise known as 'notches') within each CCD column. We present the largest published sample of Gaia CCD SBC full well capacity (FWC) laboratory measurements and simulations based on 13 devices. We find that Gaia CCDs manufactured post-2004 have SBCs with FWCs in the upper half of each CCD that are systematically smaller by two orders of magnitude (<50 electrons) compared to those manufactured pre-2004 (thousands of electrons). Gaia's faint star (13 < G < 20 mag) astrometric performance predictions by Prod'homme et al. and Holl et al. use pre-2004 SBC FWCs as inputs to their simulations. However, all the CCDs already integrated on to the satellite for the 2013 launch are post-2004. SBC FWC measurements are not available for one of our five post-2004 CCDs but the fact that it meets Gaia's image location requirements suggests that it has SBC FWCs similar to pre-2004. It is too late to measure the SBC FWCs onboard the satellite and it is not possible to theoretically predict them. Gaia's faint star astrometric performance predictions depend on knowledge of the onboard SBC FWCs but as these are currently unavailable, it is not known how representative of the whole focal plane the current predictions are. Therefore, we suggest that Gaia's initial in-orbit calibrations should include measurement of the onboard SBC FWCs. We present a potential method to do this. Faint star astrometric performance predictions based on onboard SBC FWCs at the start of the mission would allow satellite operating conditions or CTI software mitigation to be further optimized to improve the scientific return of Gaia. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1302.1873v1}, -author = {Seabroke, G. M. and Prod'homme, T. and Murray, N. J. and Crowley, C. and Hopkinson, G. and Brown, A. G.A. and Kohley, R. and Holland, A.}, -doi = {10.1093/mnras/stt121}, -eprint = {arXiv:1302.1873v1}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Seabroke et al. - 2013 - Digging supplementary buried channels Investigating the notch architecture within the CCD pixels on ESA's Gaia.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Galaxies: General,Instrumentation: Detectors,Methods: Laboratory,Methods: Numerical,Space vehicles: Instruments}, -number = {4}, -pages = {3155--3170}, -title = {{Digging supplementary buried channels: Investigating the notch architecture within the CCD pixels on ESA's Gaia satellite}}, -volume = {430}, -year = {2013} -} -@article{Brewer2012a, -abstract = {We present gravitational lens models for 20 strong gravitational lens systems observed as part of the Sloan WFC Edge-on Late-type Lens Survey (SWELLS) project. 15 of the lenses are taken from Paper I, while five are newly discovered systems. The systems are galaxy-galaxy lenses where the foreground deflector has an inclined disc, with a wide range of morphological types, from late-type spiral to lenticular. For each system, we compare the total mass inside the critical curve inferred from gravitational lens modelling to the stellar mass inferred from stellar population synthesis (SPS) models, computing the stellar mass fraction f*≡M SPS/M lens. We find that, for the lower mass SWELLS systems, adoption of a Salpeter stellar initial mass function (IMF) leads to estimates of f* that exceed 1. This is unphysical and provides strong evidence against the Salpeter IMF being valid for these systems. Taking the lower mass end of the SWELLS sample ($\sigma$ SIE < 230kms -1), we find that the IMF is lighter (in terms of stellar mass-to-light ratio) than Salpeter with 98 percent probability, and consistent with the Chabrier IMF and IMFs between the two. This result is consistent with previous studies of spiral galaxies based on independent techniques. In combination with recent studies of massive early-type galaxies that have favoured a heavier Salpeter-like IMF, this result strengthens the evidence against a universal stellar IMF. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.1677}, -author = {Brewer, Brendon J. and Dutton, Aaron A. and Treu, Tommaso and Auger, Matthew W. and Marshall, Philip J. and Barnab{\`{e}}, Matteo and Bolton, Adam S. and Koo, David C. and Koopmans, L{\'{e}}on V.E.}, -doi = {10.1111/j.1365-2966.2012.20870.x}, -eprint = {1201.1677}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Stars: luminosity function, mass function}, -number = {4}, -pages = {3574--3590}, -title = {{The SWELLS survey - III. Disfavouring 'heavy' initial mass functions for spiral lens galaxies}}, -volume = {422}, -year = {2012} -} -@article{Seabroke2011, -abstract = {Gaia will only achieve its unprecedented measurement accuracy requirements with detailed calibration and correction for radiation damage. We present our Silvaco 3D engineering software model of the Gaia CCD pixel and two of its applications for Gaia: (1) physically interpreting supplementary buried channel (SBC) capacity measurements (pocket-pumping and first pixel response) in terms of e2v manufacturing doping alignment tolerances; and (2) deriving electron densities within a charge packet as a function of the number of constituent electrons and 3D position within the charge packet as input to microscopic models being developed to simulate radiation damage. {\textcopyright}EAS, EDP Sciences 2011.}, -archivePrefix = {arXiv}, -arxivId = {1009.2431}, -author = {Seabroke, G M and Prod'homme, T and Hopkinson, G and Burt, D and Robbins, M and Holland, A}, -doi = {10.1051/eas/1045077}, -eprint = {1009.2431}, -isbn = {9782759806089}, -issn = {16334760}, -journal = {EAS Publications Series}, -pages = {433--436}, -title = {{Modelling Gaia CCD pixels with silvaco 3D engineering software}}, -url = {http://www.eas-journal.org/10.1051/eas/1045077}, -volume = {45}, -year = {2011} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}1011 to {\textgreater} 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Lovell2018, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}} \backslashleqslant M{\_}{\{}\backslashast{\}} \backslashleqslant 10{\^{}}{\{}11.9{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashlangle\backslashgamma{\^{}}{\{}\backslashprime{\}}\backslashrangle = 2.003 \backslashpm 0.008{\$} and a standard deviation of {\$}\backslashsigma{\_}{\{}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashgamma{\_}{\{}\backslashmathrm{\{}mw{\}}{\}}{\^{}}{\{}\backslashprime{\}}-f{\_}{\{}\backslashmathrm{\{}DM{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {dm,galaxies,galaxy,kinematic and dynamic,structure}, -number = {2}, -pages = {1950--1975}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {481}, -year = {2018} -} -@article{Browne2003, -abstract = {We report the final results of the search for gravitationally lensed flat-spectrum radio sources found in the combination of CLASS (Cosmic Lens All-Sky Survey) and JVAS (Jodrell Bank VLA Astrometric Survey). VLA (Very Large Array) observations of 16 503 sources have been made, resulting in the largest sample of arcsec-scale lens systems available. Contained within the 16 503 sources is a complete sample of 11685 sources which have two-point spectral indices between 1.4 and 5 GHz flatter than -0.5, and 5-GHz flux densities ≥30 mJy. A subset of 8958 sources form a well-defined statistical sample suitable for analysis of the lens statistics. We describe the systematic process by which 149 candidate lensed sources were picked from the statistical sample on the basis of possessing multiple compact components in the 0.2-arcsec resolution VLA maps. Candidates were followed up with 0.05-arcsec resolution MERLIN and 0.003-arcsec VLBA observations at 5 GHz and rejected as lens systems if they failed well-defined surface brightness and/or morphological tests. To illustrate the candidate elimination process, we show examples of sources representative of particular morphologies that have been ruled out by the follow-up observations. 194 additional candidates, not in the well-defined sample, were also followed up. Maps for all the candidates can be found on the World Wide Web at http://www.jb.man.ac.uk/research/gravlens/index.html. We summarize the properties of each of the 22 gravitational lens systems in JVAS/CLASS. 12 are double-image systems, nine are four-image systems and one is a six-image system. 13 constitute a statistically well-defined sample giving a point-source lensing rate of 1:690 ± 190. The interpretation of the results in terms of the properties of the lensing galaxy population and cosmological parameters will be published elsewhere.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0211069v2}, -author = {Browne, I. W.A. and Wilkinson, P. N. and Jackson, N. J.F. and Myers, S. T. and Fassnacht, C. D. and Koopmans, L. V.E. and Marlow, D. R. and Norbury, M. and Rusin, D. and Sykes, C. M. and Biggs, A. D. and Blandford, R. D. and {De Bruyn}, A. G. and Chae, K. H. and Heibig, P. and King, L. J. and McKean, J. P. and Pearson, T. J. and Phillips, P. M. and Readhead, A. C.S. and Xanthopoulos, E. and York, T.}, -doi = {10.1046/j.1365-8711.2003.06257.x}, -eprint = {0211069v2}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitation,Gravitational lensing,Radio continuum: Galaxies}, -month = {may}, -number = {1}, -pages = {13--32}, -primaryClass = {arXiv:astro-ph}, -title = {{The Cosmic Lens All-Sky Survey - II. Gravitational lens candidate selection and follow-up}}, -volume = {341}, -year = {2003} -} -@article{Holloway2023, -abstract = {We present new lensing frequency estimates for existing and forthcoming deep near-infrared surveys, including those from JWST and VISTA. The estimates are based on the JAdes extragalactic Ultradeep Artificial Realisations (JAGUAR) galaxy catalogue accounting for the full photometry and morphologies for each galaxy. Due to the limited area of the JAGUAR simulations, they are less suited to wide-area surveys; however, we also present extrapolations to the surveys carried out by Euclid and the Nancy Grace Roman Space Telescope. The methodology does not make assumptions about the nature of the lens itself and probes a wide range of lens masses. The lenses and sources are selected from the same catalogue and extend the analysis from the visible bands into the near-infrared. After generating realistic simulated lensed sources and selecting those that are detectable with SNR > 20, we verify the lensing frequency expectations against published lens samples selected in the visible, finding them to be broadly consistent. We find that JWST could yield ∼65 lensed systems in COSMOS-Web, of which ∼25 per cent have source redshifts >4. Deeper, narrower programs (e.g. JADES-Medium) will probe more typical source galaxies (in flux and mass) but will find fewer systems (∼25). Of the surveys we investigate, we find 55-80 per cent have detectable multiple imaging. Forthcoming NIR surveys will likely reveal new and diverse strong lens systems including lensed sources that are at higher redshift (JWST) and dustier, more massive and older (Euclid NISP) than those typically detected in the corresponding visible surveys.}, -archivePrefix = {arXiv}, -arxivId = {2308.00851}, -author = {Holloway, Philip and Verma, Aprajita and Marshall, Philip J. and More, Anupreeta and Tecza, Matthias}, -doi = {10.1093/mnras/stad2371}, -eprint = {2308.00851}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Holloway2024JWSTForecast.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {galaxies: evolution,gravitational lensing: strong,infrared: galaxies}, -number = {2}, -pages = {2341--2354}, -title = {{On the detectability of strong lensing in near-infrared surveys}}, -volume = {525}, -year = {2023} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the TIGER principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper will report on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R and Copin, Y and Monnet, G and Miller, Bryan W and Allington-Smith, J R and Bureau, M and Carollo, C Marcella and Davies, Roger L and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F and Verolme, E K and {De Zeeuw}, P Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs,cD}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{Gow2016, -abstract = {{\textcopyright}2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P D and Murray, Neil J}, -doi = {10.1117/12.2232706}, -isbn = {9781510602090}, -issn = {1996756X}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, $\sigma$(R), for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude MK < -25.3mag, or stellar mass M* ≳ 4 × 1011M⊙, within 108 Mpc. Our wide-field 107 arcsec × 107 arcsec IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes $\gamma$ inner and $\gamma$ outer of s(R). While $\gamma$ inner is mostly negative, of the 56 galaxies with sufficient radial coverage to determine $\gamma$ outer we find 36 per cent to have rising outer dispersion profiles, 30 per cent to be flat within the uncertainties and 34 per cent to be falling. The fraction of galaxies with rising outer profiles increases with M* and in denser galaxy environment, with 10 of the 11 most massive galaxies in our sample having flat or rising dispersion profiles. The strongest environmental correlations are with local density and halo mass, but a weaker correlation with large-scale density also exists. The average $\gamma$ outer is similar for brightest group galaxies, satellites and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis h4. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E. and Thomas, Jens and Blakeslee, John P. and Walsh, Jonelle L. and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Veale et al. - 2018 - The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxie.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{Blei2017, -abstract = {One of the core problems of modern statistics is to approximate difficult-to-compute probability densities. This problem is especially important in Bayesian statistics, which frames all inference about unknown quantities as a calculation involving the posterior density. In this paper, we review variational inference (VI), a method from machine learning that approximates probability densities through optimization. VI has been used in many applications and tends to be faster than classical methods, such as Markov chain Monte Carlo sampling. The idea behind VI is to first posit a family of densities and then to find the member of that family which is close to the target. Closeness is measured by Kullback-Leibler divergence. We review the ideas behind mean-field variational inference, discuss the special case of VI applied to exponential family models, present a full example with a Bayesian mixture of Gaussians, and derive a variant that uses stochastic optimization to scale up to massive data. We discuss modern research in VI and highlight important open problems. VI is powerful, but it is not yet well understood. Our hope in writing this paper is to catalyze statistical research on this class of algorithms.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1601.00670v9}, -author = {Blei, David M and Kucukelbir, Alp and McAuliffe, Jon D}, -doi = {10.1080/01621459.2017.1285773}, -eprint = {arXiv:1601.00670v9}, -isbn = {1601.00670}, -issn = {1537274X}, -journal = {Journal of the American Statistical Association}, -keywords = {Algorithms,Computationally intensive methods,Statistical computing}, -number = {518}, -pages = {859--877}, -pmid = {303902}, -title = {{Variational Inference: A Review for Statisticians}}, -volume = {112}, -year = {2017} -} -@article{DiCintio2017, -abstract = {We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of supermassive black hole (SMBH) formation and evolution is used, as in Tremmel et al., allowing us to explicitly follow the SMBH dynamics at the centre of galaxies. A high SIDM constant cross-section is chosen, $\sigma$ = 10 cm2gr-1, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in cold dark matter (CDM), with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals, the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80 per cent of the SMBH population is offcentred in the SIDM case, as opposed to the CDM case in which {\$\sim${}}90 per cent of SMBHs have reached their host's centre. SMBHs are found as far as {\$\sim${}}9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction time-scale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in core stalling. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to the SMBH physics to study their influence on galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1701.04410}, -author = {{Di Cintio}, Arianna and Tremmel, Michael and Governato, Fabio and Pontzen, Andrew and Zavala, Jes{\'{u}}s and Fry, Alexander Bastidas and Brooks, Alyson and Vogelsberger, Mark}, -doi = {10.1093/mnras/stx1043}, -eprint = {1701.04410}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution}, -number = {3}, -pages = {2845--2854}, -title = {{A rumble in the dark: Signatures of self-interacting dark matter in supermassive black hole dynamics and galaxy density profiles}}, -url = {http://arxiv.org/abs/1701.04410%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1043}, -volume = {469}, -year = {2017} -} -@article{Bower2005, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z{\textgreater}1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AGN) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z 5 and a star formation rate density which rises at least out to z 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Sales2012a, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Mahler2022, -abstract = {This study explores the gravitational lensing effects of supermassive black holes (SMBHs) in galaxy clusters. While the presence of central SMBHs in galaxies is firmly established, recent work from high-resolution simulations predict the existence of an additional population of wandering SMBHs. Though the masses of these SMBHs are a minor perturbation on the larger scale and individual galaxy scale dark matter components in the cluster, they can impact statistical lensing properties and individual lensed image configurations. Probing for these potentially observable signatures, we find that SMBHs imprint detectable signatures in rare, higher-order strong lensing image configurations although they do not manifest any statistically significant detectable evidence in either the magnification distribution or the integrated shear profile. Investigating specific lensed image geometries, we report that a massive, near point-like, potential of an SMBH causes the following detectable effects: (ii) image splitting leading to the generation of extra images; (ii) positional and magnification asymmetries in multiply imaged systems; and (iii) the apparent disappearance of a lensed counter-image. Of these, image splitting inside the cluster tangential critical curve, is the most prevalent notable observational signature. We demonstrate these possibilities in two cases of observed giant arcs in $SGAS\,J003341.5+024217$ and $RX\,J1347.5-1145$, wherein specific image configurations seen can be reproduced with SMBHs. Future observations with high-resolution instrumentation (e.g. MAVIS-Very Large Telescope, MICADO-Extremely Large Telescope, and the upgraded ngVLA, along with data from the \textit{Euclid} \& \textit{Nancy Grace Roman} Space Telescopes and the Rubin LSST Observatory are likely to allow us to probe these unique yet rare SMBHs lensing signatures.}, -archivePrefix = {arXiv}, -arxivId = {2201.10900}, -author = {Mahler, Guillaume and Natarajan, Priyamvada and Jauzac, Mathilde and Richard, Johan}, -eprint = {2201.10900}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Maheler2022SMBHInClusters.pdf:pdf}, -journal = {MNRAS}, -keywords = {galaxy clusters,gravitational lensing,supermassive black holes}, -number = {1}, -pages = {54}, -title = {{Gravitational lensing effects of supermassive black holes in cluster environments}}, -url = {http://arxiv.org/abs/2201.10900}, -volume = {518}, -year = {2023} -} -@article{Gow2016, -abstract = {{\textcopyright}2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P D and Murray, Neil J}, -doi = {10.1117/12.2232706}, -isbn = {9781510602090}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{He2017, -abstract = {Small distortions in the images of Einstein rings or giant arcs offer the exciting prospect of detecting dark matter haloes or subhaloes of mass below $10^9$M$_{\odot}$, most of which are too small to have made a visible galaxy. A very large number of such haloes are predicted to exist in the cold dark matter model of cosmogony; in contrast other models, such as warm dark matter, predict no haloes below a mass of this order which depends on the properties of the warm dark matter particle. Attempting to detect these small perturbers could therefore discriminate between different kinds of dark matter particles, and even rule out the cold dark matter model altogether. Globular clusters in the lens galaxy also induce distortions in the image which could, in principle, contaminate the test. Here, we investigate the population of globular clusters in six early type galaxies in the Virgo cluster. We find that the number density of globular clusters of mass $\sim10^6$M$_{\odot}$ is comparable to that of the dark matter perturbers (including subhaloes in the lens and haloes along the line-of-sight). We show that the very different degrees of mass concentration in globular clusters and dark matter haloes result in different lensing distortions. These are detectable with milli-arcsecond resolution imaging which can distinguish between globular cluster and dark matter halo signals.}, -archivePrefix = {arXiv}, -arxivId = {1707.01849}, -author = {He, Qiuhan and Li, Ran and Lim, Sungsoon and Frenk, Carlos S and Cole, Shaun and Peng, Eric W and Wang, Qiao}, -doi = {10.1093/mnras/sty2260}, -eprint = {1707.01849}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/He et al. - 2018 - Globular clusters vs dark matter haloes in strong lensing observations.pdf:pdf}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -number = {July}, -title = {{Globular clusters vs dark matter haloes in strong lensing observations}}, -url = {http://arxiv.org/abs/1707.01849}, -volume = {000}, -year = {2018} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kilo parsecs. These stellar halos provide a fossil record of galaxy assembly histories. Using data that is both wide ({\$\sim${}}100 square degree) and deep (i{\textgreater}28.5 mag/arcsec{\^{}}2 in i-band), we present a systematic study of the stellar halos of a sample of more than 3000 galaxies at 0.3 {\textless} z {\textless} 0.5 with {\$}\backslashlog M{\_}{\{}\backslashstar{\}}/M{\_}{\{}\backslashodot{\}} {\textgreater} 11.4{\$}. Our study is based on high-quality (0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP), which enables us to individually estimate surface mass density profiles to 100 kpc without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles. When this extended light is not properly accounted for as a result of shallow imaging or inadequate profile modeling, the derived stellar mass function can be significantly underestimated at the highest masses. Across our sample, the ellipticity of outer light profiles increases substantially as we probe larger radii. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass-dependence in outer color gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at late times from a series of merging events. We provide surface mass surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high-resolution N-body simulations of galactic dark matter haloes to test if this remarkable property can be understood within the context of the cold dark matter (CDM) cosmology. We construct halo merger trees from the simulations and use a semi-analytic model to follow the formation of satellite galaxies. We find that in all six of our simulations, the 11 brightest satellites are indeed distributed along thin, disc-like structures analogous to that traced by the satellites of the Milky Way. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhaloes within it, which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhaloes but is similar to that of the subset of subhaloes that had the most massive progenitors at earlier times. The elongated disc-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I. and Frenk, Carlos S. and Cole, Shaun and Helly, John C. and Jenkins, Adrian and Navarro, Julio F. and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Libeskind et al. - 2005 - The distribution of satellite galaxies The great pancake.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58 arcsec in the i band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including an $\sim$10 per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally,we check the sensitivity of our shear calibration estimates to other cutsmade on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalogue are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E. and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Mandelbaum et al. - 2018 - Weak lensing shear calibration with simulations of the HSC survey(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{MacArthur2009a, -abstract = {We present a detailed study of the stellar populations (SPs) and kinematics of the bulge and inner disk regions of eight nearby spiral galaxies (Sa-Sd) based on deep Gemini/GMOS data. The long-slit spectra extend to 1-2 disk scale lengths with S/N/Ang{\textgreater}=50. Several different model fitting techniques involving absorption-line indices and full spectrum fitting are explored and found to weigh age, metallicity, and abundance ratios differently. The SPs of spiral galaxies are not well matched by single episodes of star formation; representative SPs must involve average SP values integrated over the star formation history (SFH) of the galaxy. Our "full population synthesis" method is an optimised linear combination of model templates to the full spectrum with masking of regions poorly represented by the models. Our spiral bulges follow the same correlations of increasing light-weighted age and metallicity with central velocity dispersion as those of elliptical galaxies and early-type bulges found in other studies, but when SFHs more complex and realistic than a single burst are invoked, the trend with age is shallower and the scatter much reduced. In a mass-weighted context, all bulges are predominantly composed of old and metal-rich SPs. Bulge formation appears to dominated by early processes that are common to all spheroids, whether they currently reside in disks or not. While monolithic collapse cannot be ruled out in some cases, merging must be invoked to explain the SP gradients in most bulges. Further bulge growth via secular processes or "rejuvenated" star formation generally contributes minimally to the stellar mass budget. (Abridged)}, -archivePrefix = {arXiv}, -arxivId = {0901.4135}, -author = {MacArthur, Lauren A and Gonz{\'{a}}lez, J Jes{\'{u}}s and Courteau, St{\'{e}}phane}, -doi = {10.1111/j.1365-2966.2009.14519.x}, -eprint = {0901.4135}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: spiral,Galaxies: stellar content}, -number = {1}, -pages = {28--63}, -title = {{Stellar population and kinematic profiles in spiral bulges and discs: Population synthesis of integrated spectra}}, -volume = {395}, -year = {2009} -} -@article{Dekel2009b, -abstract = {The massive galaxies in the young universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids (Genzel et al. 2006, 2008). Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are stream-fed galaxies, formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes (Dekel {\&} Birnboim 2006; Keres et al. 2005). A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duy cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid (Noguchi 1999; Genzel et al. 2008, Elmegreen, Bournaud {\&} Elmegreen 2008, Dekel, Sari {\&} Ceverino 2009). This stream-driven scenario for the formation of disks and spheroids is an alternative to the merger picture.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/19158792}, -volume = {457}, -year = {2009} -} -@inproceedings{MartinNavarro2013, -abstract = {We have developed an innovative 'index scanning technique” to map the stellar kinematics of early-type galaxies by measuring for the first time the absorption line strength of the near-IR CaII triplet with the Red Tunable Filters of OSIRIS at GTC. Unlike classical spectroscopy, these filters allow us to perform a two-dimensional study, taking advantage of a 10.4 meter class telescope with a unvignetted field of view of 7.8 × 7.8 arcmin. We show the velocity fields obtained for two Virgo elliptical galaxies of very different masses and their globular cluster systems reaching galactocentric distances beyond 2 effective radii.}, -author = {Mart{\'{i}}n-Navarro, Ignacio and Vazdekis, Alexander and Bongiovanni, {\'{A}}ngel and Falc{\'{o}}n-Barroso, Jes{\'{u}}s and Cepa, Jordi and Cenarro, Javier and S{\'{a}}nchez-Bl{\'{a}}zquez, Patricia}, -booktitle = {Proceedings of the 10th Scientific Meeting of the Spanish Astronomical Society - Highlights of Spanish Astrophysics VII, SEA 2012}, -editor = {Guirado, J.$\sim$C. and Lara, L.$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable filters at gtc: A novel approach}}, -year = {2020} -} -@article{Veale2016, -abstract = {We present spatially resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (ETGs; MK ≲ -25.7 mag, stellar mass M* ≳ 1011.8 M⊙) of the volumelimited (D {\textless} 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650-5850 {\AA}from the 246-fibre Mitchell integral-field spectrograph at McDonald Observatory, covering a 107 arcsec×107 arcsec field of view(often reaching 2 to 3 effective radii).We measure the 2D spatial distribution of each galaxy's angular momentum ($\lambda$ and fast or slow rotator status), velocity dispersion ($\sigma$), and higher order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ({\$\sim${}}80 per cent) of slow and non-rotators with $\lambda$ ≲ 0.2. When combined with the lower mass ETGs in the ATLAS3D survey, we find the fraction of slow rotators to increase dramatically with galaxy mass, reaching {\$\sim${}}50 per cent at MK {\$\sim${}} -25.5 mag and {\$\sim${}}90 per cent at MK ≲ -26 mag. All of our fast rotators show a clear anticorrelation between h3 and V/$\sigma$, and the slope of the anticorrelation is steeper in more round galaxies. The radial profiles of s show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK ≲ -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat s profiles, whereas five of the seven 'isolated' galaxies are all fainter than MK = -25.8 mag and have falling $\sigma$. All of our galaxies have positive average h4; the most luminous galaxies have average h4 {\$\sim${}} 0.05, while less luminous galaxies have a range of values between 0 and 0.05. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising s profiles. We discuss the implications for the relationship among dynamical mass, $\sigma$, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E and McConnell, Nicholas J and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ($\rho\sim r^{-\gamma}$), we find that, although the zero cosmic curvature is still included within $2 \sigma$ confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile $\rho\sim r^{-\alpha}$ to be different from that of the total-mass density profile $\nu\sim r^{-\delta}$, a weaker constraint on the curvature ($\Omega_k<0.197$ at 68\% confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of $\Delta \Omega_k\simeq 10^{-3}$, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Qi et al. - 2018 - A revised test of cosmic curvature at high redshifts the distance sum rule(2).pdf:pdf}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{Bartelmann1999, -abstract = {We review theory and applications of weak gravitational lensing. After summarising Friedmann-Lema{\^{i}}tre cosmological models, we present the formalism of gravitational lensing and light propagation in arbitrary space-times. We discuss how weak-lensing effects can be measured. The formalism is then applied to reconstructions of galaxy-cluster mass distributions, gravitational lensing by large-scale matter distributions, QSO-galaxy correlations induced by weak lensing, lensing of galaxies by galaxies, and weak lensing of the cosmic microwave background. {\textcopyright} 2001 Elsevier Science B.V.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9912508}, -author = {Bartelmann, Matthias and Schneider, Peter}, -doi = {10.1016/S0370-1573(00)00082-X}, -eprint = {9912508}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bartelmann, Schneider - 2001 - Weak gravitational lensing.pdf:pdf}, -issn = {03701573}, -journal = {Physics Report}, -number = {4-5}, -pages = {291--472}, -primaryClass = {astro-ph}, -title = {{Weak gravitational lensing}}, -url = {http://arxiv.org/abs/astro-ph/9912508%0Ahttp://dx.doi.org/10.1016/S0370-1573(00)00082-X}, -volume = {340}, -year = {2001} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Bellstedt2018, -abstract = {{\textcopyright}2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 10 10 {\textless} M * /M ⊙ {\textless} 10 11.6 that cover a large radial range of 0.1-4.0 effective radii.We combine SLUGGS and ATLAS3D data sets to model the total-mass profiles of a sample of 21 fast-rotator galaxies, utilizing a hyperparameter method to combine the two independent data sets. The total-mass density profile slope values derived for these galaxies are consistent with those measured in the inner regions of galaxies by other studies. Furthermore, the total-mass density slopes ($\gamma$ tot ) appear to be universal over this broad stellar mass range, with an average value of $\gamma$ tot = -2.24± 0.05, i.e. slightly steeper than isothermal. We compare our results to model galaxies from the Magneticum and EAGLE cosmological hydrodynamic simulations, in order to probe the mechanisms that are responsible for varying total-mass density profile slopes. The simulated-galaxy slopes are shallower than the observed values by {\$\sim${}}0.3-0.5, indicating that the physical processes shaping the mass distributions of galaxies in cosmological simulations are still incomplete. For galaxies with M * {\textgreater} 1010.7M ⊙ in the Magneticum simulations, we identify a significant anticorrelation between total-mass density profile slopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas this anticorrelation is weaker for lower stellar masses, implying that the measured total-mass density slopes for low-mass galaxies are less likely to be determined by merger activity.}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A and Romanowsky, Aaron J and Remus, Rhea Silvia and Stevens, Adam R H and Brodie, Jean P and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to {\$\sim${}}4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Minka2009, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture models is not well captured by factor graphs unless the entire mixture is represented by one factor, because the message equations have a containment structure. Gates capture this containment structure graphically, allowing both the independences and the message-passing equations for a model to be readily visualized. Different variational approximations for mixture models can be understood as different ways of drawing the gates in a model. We present general equations for expectation propagation and variational message passing in the presence of gates.}, -author = {Minka, Tom and Winn, John}, -doi = {10.5790/hongkong/9789888083091.003.0088}, -isbn = {9781605609492}, -issn = {0018702X}, -journal = {Advances in Neural Information Processing Systems 21 - Proceedings of the 2008 Conference}, -pages = {1073--1080}, -title = {{Gates}}, -year = {2009} -} -@article{VanDeVen2009, -abstract = {Studies of strong gravitational lensing in current and upcoming wide and deep photometric surveys, and of stellar kinematics from (integral-field) spectroscopy at increasing redshifts, promise to provide valuable constraints on galaxy density profiles and shapes. However, both methods are affected by various selection and modelling biases, which we aim to investigate in a consistent way. In this first paper in a series, we develop a flexible but efficient pipeline to simulate lensing by realistic galaxy models. These galaxy models have separate stellar and dark matter components, each with a range of density profiles and shapes representative of early-type, central galaxies without significant contributions from other nearby galaxies. We use Fourier methods to calculate the lensing properties of galaxies with arbitrary surface density distributions, and Monte Carlo methods to compute lensing statistics such as point-source lensing cross-sections. Incorporating a variety of magnification bias modes lets us examine different survey limitations in image resolution and flux. We rigorously test the numerical methods for systematic errors and sensitivity to basic assumptions. We also determine the minimum number of viewing angles that must be sampled in order to recover accurate orientation-averaged lensing quantities. We find that for a range of non-isothermal stellar and dark matter density profiles typical of elliptical galaxies, the combined density profile and corresponding lensing properties are surprisingly close to isothermal around the Einstein radius. The converse implication is that constraints from strong lensing and/or stellar kinematics, which are indeed consistent with isothermal models near the Einstein radius, cannot trivially be extrapolated to smaller and larger radii. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:0808.2493v1}, -author = {{Van De Ven}, Glenn and Mandelbaum, Rachel and Keeton, Charles R.}, -doi = {10.1111/j.1365-2966.2009.15167.x}, -eprint = {arXiv:0808.2493v1}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: kinematics and dynamics,Galaxies: photometry,Galaxies: structure,Gravitational lensing,Methods: numerical,Stellar dynamics}, -number = {2}, -pages = {607--634}, -title = {{Galaxy density profiles and shapes - I. Simulation pipeline for lensing by realistic galaxy models}}, -volume = {398}, -year = {2009} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in SPH simulations. About half the gas shock heats to roughly the virial temperature of the galaxy potential well before cooling, condensing, and forming stars, but the other half radiates its acquired gravitational energy at much lower temperatures, typically T{\textless}10{\^{}}5 K, and the histogram of maximum gas temperatures is clearly bimodal. The "cold mode" of gas accretion dominates for low mass galaxies (M{\_}baryon {\textless}10{\^{}}{\{}10.3{\}}Msun or M{\_}halo {\textless}10{\^{}}{\{}11.4{\}}Msun), while the conventional "hot mode" dominates the growth of high mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasi-spherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with cold mode dominating at high redshift and in low density regions today, and hot mode dominating in group and cluster environments at low redshift. Star formation rates closely track accretion rates, and we discuss the physics behind the observed environment and redshift dependence of galactic scale star formation. If we allowed hot accretion to be suppressed by conduction or AGN feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colors of ellipticals and the cutoff of the galaxy luminosity function. The transition between cold and hot accretion at M{\_}h {\$\sim${}} 10{\^{}}{\{}11.4{\}}Msun is similar to that found by Birnboim {\&} Dekel (2003) using 1-d simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. (2003) find a marked shift in galaxy properties. We speculate on connections between these theoretical and observational transitions.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10^11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r_vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of $\sim$25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r_vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bailin, Steinmetz - 2005 - Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos(2).pdf:pdf}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -publisher = {MNRAS}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance $\Lambda$ cold dark matter cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for 'radio' feedback from those active galactic nuclei that lie at the centre of a quasi-static X-ray-emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models that might explain the accretion rate scalings required for our phenomenological 'radio mode' model to be successful. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J and Springel, Volker and White, Simon D M and {De Lucia}, G and Frenk, C S and Gao, L and Jenkins, A and Kauffmann, G and Navarro, J F and Yoshida, N}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Wong2017, -abstract = {We present long-baseline ALMA observations of the strong gravitational lens H-ATLAS J090740.0-004200 (SDP.9), which consists of an elliptical galaxy at $z_{\mathrm{L}}=0.6129$ lensing a background submillimeter galaxy into two extended arcs. The data include Band 6 continuum observations, as well as CO $J$=6$-$5 molecular line observations, from which we measure an updated source redshift of $z_{\mathrm{S}}=1.5747$. The image morphology in the ALMA data is different from that of the HST data, indicating a spatial offset between the stellar, gas, and dust component of the source galaxy. We model the lens as an elliptical power law density profile with external shear using a combination of archival HST data and conjugate points identified in the ALMA data. Our best model has an Einstein radius of $\theta_{\mathrm{E}}=0.66\pm0.01$ and a slightly steeper than isothermal mass profile slope. We search for the central image of the lens, which can be used constrain the inner mass distribution of the lens galaxy including the central supermassive black hole, but do not detect it in the integrated CO image at a 3$\sigma$ rms level of 0.0471 Jy km s$^{-1}$.}, -archivePrefix = {arXiv}, -arxivId = {1707.00702}, -author = {Wong, Kenneth C. and Ishida, Tsuyoshi and Tamura, Yoichi and Suyu, Sherry H. and Oguri, Masamune and Matsushita, Satoki}, -doi = {10.3847/2041-8213/aa7d4a}, -eprint = {1707.00702}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Wong2071ALMACentralImage.pdf:pdf}, -issn = {2041-8213}, -journal = {ApJ}, -number = {2}, -pages = {L35}, -title = {{ALMA Observations of the Gravitational Lens SDP.9}}, -volume = {843}, -year = {2017} -} -@article{Boylan-Kolchin:2006aa, -author = {Boylan-Kolchin, M and Ma, C.-P. and Quataert, E}, -journal = {\mnras}, -month = {jul}, -pages = {1081--1089}, -title = {{Red mergers and the assembly of massive elliptical galaxies: the fundamental plane and its projections}}, -volume = {369}, -year = {2006} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z {\$\sim${}} 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u – g color profiles for these galaxies and show that most z {\$\sim${}} 2 galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z {\$\sim${}} 2 galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: ({\$}\Delta{\$}(u – g rest)/{\$}\Delta{\$}(log r))median = –0.47, –0.33, and –0.46 for z {\$\sim${}} 2, z {\$\sim${}} 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z {\$\sim${}} 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u – g colors, and lower S{\'{e}}rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J and {Van Dokkum}, Pieter G and Labb{\'{e}}, Ivo and Illingworth, Garth D and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Naab2009, -abstract = {Using a high-resolution hydrodynamical cosmological simulation of the formation of a massive spheroidal galaxy we show that elliptical galaxies can be very compact and massive at high redshift in agreement with recent observations. Accretion of stripped infalling stellar material increases the size of the system with time and the central concentration is reduced by dynamical friction of the surviving stellar cores. In a specific case of a spheroidal galaxy with a final stellar mass of 1.5 × 1011 M ⊙ we find that the effective radius re increases from 0.7 ± 0.2 kpc at z = 3 to re = 2.4 ± 0.4 kpc at z = 0 with a concomitant decrease in the effective density of an order of magnitude and a decrease of the central velocity dispersion by approximately 20{\%} over this time interval. A simple argument based on the virial theorem shows that during the accretion of weakly bound material (minor mergers) the radius can increase as the square of the mass in contrast to the usual linear rate of increase for major mergers. By undergoing minor mergers compact high-redshift spheroids can evolve into present-day systems with sizes and concentrations similar to observed local ellipticals. This indicates that minor mergers may be the main driver for the late evolution of sizes and densities of early-type galaxies. {\textcopyright}2009 The American Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {0903.1636}, -author = {Naab, Thorsten and Johansson, Peter H and Ostriker, Jeremiah P}, -doi = {10.1088/0004-637X/699/2/L178}, -eprint = {0903.1636}, -issn = {2041-821}, -journal = {Astrophysical Journal Letters}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: interactions,Galaxies: structure,Methods: numerical,cd}, -month = {jul}, -number = {2 PART 2}, -pages = {L178----L182}, -title = {{Minor mergers and the size evolution of elliptical galaxies}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L178?key=crossref.405faa44137f4be9a7e3800a4c3e7dea}, -volume = {699}, -year = {2010} -} -@article{2001eq, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyse sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in 255 deg2 of the Kilo Degree Survey (KiDS), one of the currentgeneration optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii ≳1.4 arcsec, about twice the r-band seeing in KiDS. In a sample of 21 789 colour-magnitude selected luminous red galaxies (LRGs), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find {\$\sim${}}100 massive LRGgalaxy lenses at z ≲ 0.4 in KiDS when completed. In the most optimistic scenario, this number can grow considerably (to maximally {\$\sim${}}2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C E and Tortora, C and Chatterjee, S and Vernardos, G and Koopmans, L V E and Kleijn, G Verdoes and Napolitano, N R and Covone, G and Schneider, P and Grado, A and McFarland, J}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys,cD}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{Xie2014, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P. and Frenk, Carlos S. and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xie et al. - 2015 - The size evolution of elliptical galaxies(3).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stu2487}, -volume = {447}, -year = {2015} -} -@article{Stacey2024, -abstract = {The large-scale mass distributions of strong-lensing galaxies have long been assumed to be well-described by a singular ellipsoidal power-law density profile with external shear. However, the inflexibility of this model could lead to systematic errors in astrophysical parameters inferred with gravitational lensing observables. Here, we present observations with the Atacama Large (sub-)Millimetre Array (ALMA) of three strongly lensed dusty star-forming galaxies at $\simeq30$ mas angular resolution and investigate the sensitivity of these data to angular structure in the lensing galaxies. We jointly infer the lensing mass distribution and the full surface brightness of the lensed sources with multipole expansions of the power-law density profile up to fourth order using a technique developed for interferometric data. All three data sets strongly favour third and fourth-order multipole amplitudes of $\approx1$ percent of the convergence. While the infrared stellar isophotes and isodensity shapes agree for one lens system, for the other two the isophotes disagree to varying extents, suggesting contributions to the angular structure from dark matter intrinsic or extrinsic to the lensing galaxy.}, -archivePrefix = {arXiv}, -arxivId = {2403.04850}, -author = {Stacey, H. R. and Powell, D. M. and Vegetti, S. and McKean, J. P. and Fassnacht, C. D. and Wen, D. and O'Riordan, C. M.}, -eprint = {2403.04850}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Stacey2024MultipolesALMA.pdf:pdf}, -journal = {arxiv.org/2403.04850}, -keywords = {cd,elliptical and lenticular,galaxies,general,gravitational lensing,strong,submillimeter}, -title = {{Complex angular structure of three elliptical galaxies from high-resolution ALMA observations of strong gravitational lenses}}, -url = {http://arxiv.org/abs/2403.04850}, -year = {2024} -} -@article{Oser:2010aa, -author = {Naab, Thorsten}, -journal = {Direct}, -month = {dec}, -pages = {2312--2323}, -title = {{The two phases of massive galaxy formation}}, -volume = {725}, -year = {2010} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless} $\sigma$∗ {\textless} 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history. {\textcopyright}2015. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Cautun2015a, -abstract = {We investigate the angular and kinematic distributions of satellite galaxies around a large sample of bright isolated primaries in the spectroscopic and photometric catalogues of the Sloan Digital Sky Survey (SDSS). We detect significant anisotropy in the spatial distribution of satellites. To test whether this anisotropy could be related to the rotating discs of satellites recently found by Ibata et al. in a sample of SDSS galaxies, we repeat and extend their analysis. Ibata et al. found an excess of satellites on opposite sides of their primaries having anticorrelated radial velocities. We find that this excess is sensitive to small changes in the sample selection criteria which can greatly reduce its significance. In addition, we find no evidence for correspondingly correlated velocities for satellites observed on the same side of their primaries, which would be expected for rotating discs of satellites. We conclude that the detection of rotating planes of satellites in the observational sample of Ibata et al. is not robust to changes in the sample selection criteria. We compare our data to the $\Lambda$ cold dark matter Millennium simulations populated with galaxies according to the semi-analytic model of Guo et al. We find excellent agreement with the spatial distribution of satellites in the SDSS data and the lack of a strong signal from coherent rotation.}, -archivePrefix = {arXiv}, -arxivId = {1410.7778}, -author = {Cautun, Marius and Wang, Wenting and Frenk, Carlos S and Sawala, Till}, -doi = {10.1093/mnras/stv490}, -eprint = {1410.7778}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {3}, -pages = {2576--2587}, -title = {{A new spin on discs of satellite galaxies}}, -volume = {449}, -year = {2015} -} -@article{Weinberg2007, -abstract = {A galaxy remains near equilibrium for most of its history. Only through resonances can non-axisymmetric features, such as spiral arms and bars, exert torques over large scales and change the overall structure of the galaxy. In this paper, we describe the resonant interaction mechanism in detail, derive explicit criteria for the particle number required to simulate these dynamical processes accurately using N-body simulations, and illustrate them with numerical experiments. To do this, we perform a direct numerical solution of perturbation theory, in short, by solving for each orbit in an ensemble and make detailed comparisons with N-body simulations. The criteria include: sufficient particle coverage in phase space near the resonance and enough particles to minimize gravitational potential fluctuations that will change the dynamics of the resonant encounter. These criteria are general in concept and can be applied to any dynamical interaction. We use the bar-halo interaction as our primary example owing to its technical simplicity and astronomical ubiquity. Some of our more surprising findings are as follows. First, the inner Lindblad like resonance, responsible for coupling the bar to the central halo cusp, requires more than script O sign (108) equal-mass particles within the virial radius or O(107) inside the bar radius for a Milky Way like bar in a Navarro, Frenk & White profile. Secondly, orbits that linger near the resonance receive more angular momentum than orbits that move through the resonance quickly. Small-scale fluctuations present in state-of-the-art particle-particle simulations can knock orbits out of resonance, preventing them from lingering and, thereby, decrease the torque per orbit. This can be offset by the larger number of orbits affected by the resonance due to the diffusion. However, noise from orbiting substructure remains at least an order of magnitude too small to be of consequence. Applied to N-body simulations, the required particle numbers are sufficiently high for scenarios of interest that apparent convergence in particle number is misleading: the convergence with N may still be in the noise-dominated regime. State-of-the-art simulations are not adequate to follow all aspects of secular evolution driven by the bar-halo interaction. It is not possible to derive particle number requirements that apply to all situations, for example, more subtle interactions may be even more difficult to simulate. Therefore, we present a procedure to test the requirements for individual N-body codes to the actual problem of interest. {\textcopyright} 2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508166}, -author = {Weinberg, Martin D. and Katz, Neal}, -doi = {10.1111/j.1365-2966.2006.11306.x}, -eprint = {0508166}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxy: structure,Stellar dynamics}, -number = {2}, -pages = {425--459}, -primaryClass = {astro-ph}, -title = {{The bar-halo interaction - I. From fundamental dynamics to revised N-body requirements}}, -volume = {375}, -year = {2007} -} -@article{Holloway2024, -abstract = {The arrival of the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST), Euclid-Wide and Roman wide-area sensitive surveys will herald a new era in strong lens science in which the number of strong lenses known is expected to rise from to. However, current lens-finding methods still require time-consuming follow-up visual inspection by strong lens experts to remove false positives which is only set to increase with these surveys. In this work, we demonstrate a range of methods to produce calibrated probabilities to help determine the veracity of any given lens candidate. To do this we use the classifications from citizen science and multiple neural networks for galaxies selected from the Hyper Suprime-Cam survey. Our methodology is not restricted to particular classifier types and could be applied to any strong lens classifier which produces quantitative scores. Using these calibrated probabilities, we generate an ensemble classifier, combining citizen science, and neural network lens finders. We find such an ensemble can provide improved classification over the individual classifiers. We find a false-positive rate of 10-3 can be achieved with a completeness of 46 per cent, compared to 34 per cent for the best individual classifier. Given the large number of galaxy-galaxy strong lenses anticipated in LSST, such improvement would still produce significant numbers of false positives, in which case using calibrated probabilities will be essential for population analysis of large populations of lenses and to help prioritize candidates for follow-up.}, -archivePrefix = {arXiv}, -arxivId = {2311.07455}, -author = {Holloway, Philip and Marshall, Philip J. and Verma, Aprajita and More, Anupreeta and Ca{\~{n}}ameras, Raoul and Jaelani, Anton T. and Ishida, Yuichiro and Wong, Kenneth C.}, -doi = {10.1093/mnras/stae875}, -eprint = {2311.07455}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Holloway2024JWSTForecast.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {gravitational lensing: strong,methods: data analysis,methods: statistical}, -number = {2}, -pages = {1297--1310}, -title = {{A Bayesian approach to strong lens finding in the era of wide-area surveys}}, -volume = {530}, -year = {2024} -} -@article{Funk2014, -abstract = {The details of what constitutes the majority of the mass that makes up dark matter in the Universe remains one of the prime puzzles of cosmology and particle physics today-80 y after the first observational indications. Today, it is widely accepted that dark matter exists and that it is very likely composed of elementary particles, which are weakly interacting and massive [weakly interacting massive particles (WIMPs)]. As important as dark matter is in our understanding of cosmology, the detection of these particles has thus far been elusive. Their primary properties such as mass and interaction cross sections are still unknown. Indirect detection searches for the products of WIMP annihilation or decay. This is generally done through observations of {\~{a}}-ray photons or cosmic rays. Instruments such as the Fermi large-area telescope, high-energy stereoscopic system, major atmospheric gamma-ray imaging Cherenkov, and very energetic radiation imaging telescope array, combined with the future Cherenkov telescope array, will provide important complementarity to other search techniques. Given the expected sensitivities of all search techniques, we are at a stage where the WIMP scenario is facing stringent tests, and it can be expected that WIMPs will be either be detected or the scenario will be so severely constrained that it will have to be rethought. In this sense, we are on the threshold of discovery. In this article, I will give a general overview of the current status and future expectations for indirect searches of dark matter (WIMP) particles.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1310.2695v1}, -author = {Funk, Stefan}, -doi = {10.1073/pnas.1308728111}, -eprint = {arXiv:1310.2695v1}, -isbn = {0-8264-6667-2}, -issn = {10916490}, -journal = {Proceedings of the National Academy of Sciences of the United States of America}, -keywords = {CTA,Fermi-LAT,H.E.S.S.,MAGIC|VERITAS}, -month = {oct}, -number = {40}, -pages = {12264--12271}, -pmid = {24821791}, -title = {{Indirect detection of dark matter with $\gamma$ rays}}, -url = {http://www.pnas.org/lookup/doi/10.1073/pnas.1308728111}, -volume = {112}, -year = {2015} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kremer et al. - 2017 - Big Universe, Big Data Machine Learning and Image Analysis for Astronomy.pdf:pdf}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Khochfar2011, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* > 1010.5M⊙ contributing $\sim$20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between $\sim$50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z > 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) > 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z < 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive (>1010M⊙) fast rotators being more than one order of magnitude more frequent at z$\sim$ 2. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R. and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Khochfar et al. - 2011 - The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies.pdf:pdf}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: structure}, -month = {oct}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright} 2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel, Sari, Ceverino - 2009 - Formation of massive galaxies at high redshift Cold streams, clumpy disks, and compact spheroids(2).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Kochanek2001, -abstract = {We develop a theory of Einstein rings and demonstrate it using the infrared Einstein ring images of the quasar host galaxies observed in PG 1115]080, B1608]656, and B1938]666. The shape of an Ein-stein ring accurately and independently determines the shape of the lens potential and the shape of the lensed host galaxy. We Ðnd that the host galaxies of PG 1115]080, B1608]656, and B1938]666 have axis ratios of 0.58 ^ 0.02, 0.69 ^ 0.02, and 0.62 ^ 0.14, respectively, including the uncertainties in the lens models. The Einstein rings break the degeneracies in the mass distributions or Hubble constants inferred from observations of gravitational lenses. In particular, the Einstein ring in PG 1115]080 rules out the centrally concentrated mass distributions that lead to a high Hubble constant km s$\sim$1 Mpc$\sim$1) (H 0 [ 60 given the measured time delays. Deep, detailed observations of Einstein rings will be revolutionary for constraining mass models and determining the Hubble constant from time-delay measurements.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0006116}, -author = {Kochanek, C. S. and Keeton, C. R. and McLeod, B. A.}, -doi = {10.1086/318350}, -eprint = {0006116}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Distance Scale,Cosmology: Gravitational Lensing,Cosmology: Observations}, -month = {jan}, -number = {1}, -pages = {50--59}, -primaryClass = {astro-ph}, -title = {{The Importance of Einstein Rings}}, -url = {http://stacks.iop.org/0004-637X/547/i=1/a=50}, -volume = {547}, -year = {2001} -} -@article{Read2005, -abstract = {Dwarf spheroidal galaxies have shallow central dark matter density profiles, low angular momentum and approximately exponential surface brightness distributions. Through N-body simulations and analytic calculations we investigate the extent to which these properties can be generated from ``typical'' $\Lambda$CDM galaxies, which differ in all of these properties, by the dynamical consequences of feedback. We find that, for a wide range of initial conditions, one impulsive mass loss event will naturally produce a surface brightness profile in the remaining stellar component of a dwarf spheroidal galaxy (dSph) which is well fit over many scale lengths by an exponential, in good qualitative agreement with observations of Local Group dSphs. Furthermore, two impulsive mass loss phases, punctuated by significant gas re-accretion, are found to be sufficient to transform a central density cusp in the dark matter profile into a near-constant density core. This may then provide the missing link between current cosmological simulations, which predict a central cusp in the dark matter density profile, and current observations, which find much shallower central density profiles. We also look at the angular momentum history of dSphs and demonstrate that if these galaxies have spent most of their lifetime in tidal isolation from massive galaxies then they cannot have formed from high angular momentum gas discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0409565}, -author = {Read, J. I. and Gilmore, G.}, -doi = {10.1111/j.1365-2966.2004.08424.x}, -eprint = {0409565}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Evolution,Galaxies,Galaxies: dwarf,Galaxies: haloes,Galaxies: kinematics and dynamics,Galaxies: structure}, -month = {jan}, -number = {1}, -pages = {107--124}, -primaryClass = {astro-ph}, -title = {{Mass loss from dwarf spheroidal galaxies: The origins of shallow dark matter cores and exponential surface brightness profiles}}, -volume = {356}, -year = {2005} -} -@article{Hopkins2012, -abstract = {Feedback from massive stars is believed to play a critical role in driving galactic super-winds that enrich the intergalactic medium and shape the galaxy mass function, mass-metallicity relation and other global galaxy properties. In previous papers, we have introduced new numerical methods for implementing stellar feedback on sub-giant molecular cloud (sub-GMC) through galactic scales in numerical simulations of galaxies; the key physical processes include radiation pressure in the ultraviolet through infrared, supernovae (Type I and Type II), stellar winds ('fast' O star through 'slow' asymptotic giant branch winds), and Hii photoionization. Here, we show that these feedback mechanisms drive galactic winds with outflow rates as high as ∼10-20 times the galaxy star formation rate. The mass-loading efficiency (wind mass-loss rate divided by the star formation rate) scales roughly as M wind/M* ∞ V c-1 (where V c is the galaxy circular velocity), consistent with simple momentum-conservation expectations. We use our suite of simulations to study the relative contribution of each feedback mechanism to the generation of galactic winds in a range of galaxy models, from Small Magellanic Cloud like dwarfs and Milky Way (MW) analogues to z∼ 2 clumpy discs. In massive, gas-rich systems (local starbursts and high-z galaxies), radiation pressure dominates the wind generation. By contrast, for MW-like spirals and dwarf galaxies the gas densities are much lower and sources of shock-heated gas such as supernovae and stellar winds dominate the production of large-scale outflows. In all of our models, however, the winds have a complex multiphase structure that depends on the interaction between multiple feedback mechanisms operating on different spatial scales and time-scales: any single feedback mechanism fails to reproduce the winds observed. We use our simulations to provide fitting functions to the wind mass loading and velocities as a function of galaxy properties, for use in cosmological simulations and semi-analytic models. These differ from typically adopted formulae with an explicit dependence on the gas surface density that can be very important in both low-density dwarf galaxies and high-density gas-rich galaxies. {\textcopyright} 2012 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.4638}, -author = {Hopkins, Philip F. and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2012.20593.x}, -eprint = {1110.4638}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins, Quataert, Murray - 2012 - Stellar feedback in galaxies and the origin of galaxy-scale winds.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Stars: formation}, -number = {4}, -pages = {3522--3537}, -title = {{Stellar feedback in galaxies and the origin of galaxy-scale winds}}, -volume = {421}, -year = {2012} -} -@article{Khochfar2011a, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}R{\$}. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the {\$}\backslash{\$}atl survey, assuming that fast rotating ETGs have at least 10{\%} of their total stellar mass in a disc component. In agreement with {\$}\backslash{\$}atl observations we find that slow rotators are predominantly galaxies with {\$} M{\_}* {\textgreater}10{\^{}}{\{}10.5{\}}{\$} M{\$}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} contributing {\$}\backslashbackslashsim 20{\%}{\$} to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between {\$}\backslashbackslashsim 50{\%} -90{\%}{\$} of their stellar mass from satellites and their most massive progenitors have on average up to 3 major mergers during their evolution. Fast rotators in contrast, accrete less than 50{\%} and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stops, galaxies grow via infall from satellites. Frequent minor mergers thereby, destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering {\$}\backslashbackslashlambda{\{}\backslash{\_}{\}}R{\$} into the slow rotator regime. Abridged...}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M and Cappellari, Michele and Davies, Roger L and Davis, Timothy A and de Zeeuw, P T and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: structure,cD}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3Dproject - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within {\$}\Lambda{\$}CDM}}, -volume = {417}, -year = {2011} -} -@article{Gilman2019, -abstract = {{Strong lensing provides a powerful means of investigating the nature of dark matter as it probes dark matter structure on sub-galactic scales. We present an extension of a forward modelling framework that uses flux ratios from quadruply imaged quasars (quads) to measure the shape and amplitude of the halo mass function, including line-of-sight (LOS) haloes and main deflector subhaloes. We apply this machinery to 50 mock lenses - roughly the number of known quads - with warm dark matter (WDM) mass functions exhibiting free-streaming cut-offs parametrized by the half-mode mass mhm. Assuming cold dark matter (CDM), we forecast bounds on mhm and the corresponding thermal relic particle masses over a range of tidal destruction severity, assuming a particular WDM mass function and mass-concentration relation. With significant tidal destruction, at 2$\sigma$ we constrain mhm < 107.9(108.4) M⊙, or a 4.4 (3.1) keV thermal relic, with image flux uncertainties from measurements and lens modelling of 2 percent 6 per cent}. With less severe tidal destruction we constrain mhm 107 107.4)M⊙, or an 8.2 (6.2) keV thermal relic. If dark matter is warm, with mhm= 107.7, M⊙ (5.1 keV), we would favour WDM with mhm > 107.7 M⊙ over CDM with relative likelihoods of 22:1 and 8:1 with flux uncertainties of 2rm per cent and 6rm per cent, respectively. These bounds improve over those obtained by modelling only main deflector subhaloes because LOS objects produce additional flux perturbations, especially for high-redshift systems. These results indicate that ∼50 quads can conclusively differentiate between WDM and CDM.}, -archivePrefix = {arXiv}, -arxivId = {1901.11031}, -author = {Gilman, Daniel and Birrer, Simon and Treu, Tommaso and Nierenberg, Anna and Benson, Andrew}, -doi = {10.1093/mnras/stz1593}, -eprint = {1901.11031}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Gilman2019LowMass.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {dark matter,galaxies: structure,gravitational lensing: strong,methods: statistical}, -number = {4}, -pages = {5721--5738}, -title = {{Probing dark matter structure down to 107 solar masses: flux ratio statistics in gravitational lenses with line-of-sight haloes}}, -volume = {487}, -year = {2019} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned r- and g-band images from a sample of 45 508 galaxies from Sloan Digital Sky Survey Data Release 9 in the redshift range 0.06≤z≤0.1 and in the mass range 1010.0M⊙ 60°), nonvariable, unidentified sources contained in this catalog, only one or two are compatible with the spectrum of a dark matter particle heavier than approximately 50-100 GeV. The majority of these nine sources, however, feature a spectrum that is compatible with that predicted from a lighter (∼5-40GeV) dark matter particle. This population is consistent with the number of observable subhalos predicted for a dark matter candidate in this mass range and with an annihilation cross section of a simple thermal relic ($\sigma$v∼3×10 -26cm3/s). Observations in the direction of these sources at other wavelengths will be necessary to either reveal their astrophysical nature (as blazars or other active galactic nuclei, for example), or to further support the possibility that they are dark matter subhalos by failing to detect any non-gamma-ray counterpart. {\textcopyright} 2012 American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {1111.2613}, -author = {Belikov, Alexander V. and Buckley, Matthew R. and Hooper, Dan}, -doi = {10.1103/PhysRevD.86.043504}, -eprint = {1111.2613}, -issn = {15507998}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -number = {4}, -title = {{Searching for dark matter subhalos in the Fermi-LAT second source catalog}}, -volume = {86}, -year = {2012} -} -@article{Cooper:2015aa, -author = {Cooper, A.$\sim$P. and Parry, O.$\sim$H. and Lowing, B and Cole, S and Frenk, C}, -journal = {\mnras}, -month = {dec}, -pages = {3185--3199}, -title = {{Formation of in situ stellar haloes in Milky Way-mass galaxies}}, -volume = {454}, -year = {2015} -} -@article{Wang2017, -abstract = {Difference imaging or image subtraction is a method that measures differential photometry by matching the pointing and point-spread function (PSF) between image frames. It is used for the detection of time-variable phenomena. Here we present a new category of method---CPM Difference Imaging, in which differences are not measured between matched images but instead between image frames and a data-driven predictive model that has been designed only to predict the pointing, PSF, and detector effects but not astronomical variability. In CPM Difference Imaging each pixel is modelled by the Causal Pixel Model (CPM) originally built for modeling Kepler data, in which pixel values are predicted by a linear combination of other pixels at the same epoch but far enough away such that these pixels are causally disconnected, astrophysically. It does not require that the user have any explicit model or description of the pointing or point-spread function of any of the images. Its principal drawback is that---in its current form---it requires an imaging campaign with many epochs and fairly stable telescope pointing. The method is applied to simulated data and also the K2 Campaign 9 microlensing data. We show that CPM Difference Imaging can detect variable objects and produce precise differentiate photometry in a crowded field. CPM Difference Imaging is capable of producing image differences at nearly photon-noise precision.}, -archivePrefix = {arXiv}, -arxivId = {1710.02428}, -author = {Wang, Dun and Hogg, David W and Foreman-Mackey, Daniel and Sch{\"{o}}lkopf, Bernhard}, -eprint = {1710.02428}, -pages = {1--23}, -title = {{A pixel-level model for event discovery in time-domain imaging}}, -url = {http://arxiv.org/abs/1710.02428}, -year = {2017} -} -@article{Kitching2008, -abstract = {In this paper, we extend the Bayesian model fitting shape measurement method presented in Miller et al., and use the method to estimate the shear from the Shear TEsting Programme simulations (STEP). The method uses a fast model fitting algorithm that uses realistic galaxy profiles and analytically marginalizes over the position and amplitude of the model by doing the model fitting in Fourier space. This is used to find the full posterior probability in ellipticity. The shear is then estimated in a Bayesian way from this posterior probability surface. The Bayesian estimation allows measurement bias arising from the presence of random noise to be removed. In this paper, we introduce an iterative algorithm that can be used to estimate the intrinsic ellipticity prior and show that this is accurate and stable. We present results using the STEP parametrization that relates the input shear $\gamma$T to the estimated shear $\gamma$M by introducing a bias m and an offset c: $\gamma$M - $\gamma$T = m$\gamma$T + c. The average number density of galaxies used in the STEP1 analysis was 9 per square arcminute, for STEP2 the number density was 30 per square arcminute. By using the method to estimate the shear from the STEP1 simulations we find the method to have a shear bias of m = 0.006 ± 0.005 and a variation in shear offset with point spread function type of $\sigma$c = 0.0002. Using the method to estimate the shear from the STEP2 simulations we find that the shear bias and offset are m = 0.002 ± 0.016 and c = -0.0007 ± 0.0006, respectively. In addition, we find that the bias and offset are stable to changes in the magnitude and size of the galaxies. Such biases should yield any cosmological constraints from future weak lensing surveys robust to systematic effects in shape measurement. Finally, we present an alternative to the STEP parametrization by using a quality factor that relates the intrinsic shear variance in a simulation to the variance in shear that is measured and show that the method presented has an average of Q ≳ 100 which is at least a factor of 10 times better than other shape measurement methods. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0802.1528}, -author = {Kitching, T D and Miller, L and Heymans, C E and {Van Waerbeke}, L and Heavens, A F}, -doi = {10.1111/j.1365-2966.2008.13628.x}, -eprint = {0802.1528}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observation,Gravitational lensing,Methods: data analysis,Methods: numerical,Methods: statistical}, -number = {1}, -pages = {149--167}, -title = {{Bayesian galaxy shape measurement for weak lensing surveys - II. Application to simulations}}, -volume = {390}, -year = {2008} -} -@article{Reynolds2015, -abstract = {Compact radio sources sometimes exhibit intervals of large, rapid changes in their flux-density, due to lensing by interstellar plasma crossing the line-of-sight. A novel survey program has made it possible to discover these "Extreme Scattering Events" (ESEs) in real time, resulting in a high-quality dynamic spectrum of an ESE observed in PKS 1939-315. Here we present a method for determining the column-density profile of a plasma lens, given only the dynamic radio spectrum of the lensed source, under the assumption that the lens is either axisymmetric or totally anisotropic. Our technique relies on the known, strong frequency dependence of the plasma refractive index in order to determine how points in the dynamic spectrum map to positions on the lens. We apply our method to high-frequency (4.2-10.8 GHz) data from the Australia Telescope Compact Array of the PKS 1939-315 ESE. The derived electron column-density profiles are very similar for the two geometries we consider, and both yield a good visual match to the data. However, the fit residuals are substantially above the noise level, and deficiencies are evident when we compare the predictions of our model to lower-frequency (1.6-3.1 GHz) data on the same ESE, thus motivating future development of more sophisticated inversion techniques.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1512.03411}, -author = {Tuntsov, Artem V and Walker, Mark A and Koopmans, Leon V E and Bannister, Keith W and Stevens, Jamie and Johnston, Simon and Reynolds, Cormac and Bignall, Hayley E}, -doi = {10.3847/0004-637x/817/2/176}, -eprint = {1512.03411}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {176}, -title = {{Dynamic Spectral Mapping of Interstellar Plasma Lenses}}, -url = {http://arxiv.org/abs/1512.03411%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/2/176}, -volume = {817}, -year = {2016} -} -@article{Wood2014, -abstract = {? 2014 IOP Publishing Ltd and Sissa Medialab srl.The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D and Hall, D J and Murray, N J and Gow, J P D and Holland, A and Turner, P and Burt, D}, -doi = {10.1088/1748-0221/9/12/C12028}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv,visible and ir photons (s}, -number = {12}, -pages = {C12028--------C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{Lee2016, -abstract = {We study how properties of discrete dark matter halos depend on halo environment, characterized by the mass density around the halos on scales from 0.5 to 16 {\$}h{\^{}}{\{}-1{\}}{\{}\backslashrm Mpc{\}}{\$}. We find that low mass halos (those less massive than the characteristic mass {\$}M{\_}{\{}\backslashrm C{\}}{\$} of halos collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations, and rounder shapes than halos in median density environments. Halos in median and low-density environments have similar accretion rates and concentrations, but halos in low density environments have lower spins and are more elongated. Halos of a given mass in high-density regions accrete material earlier than halos of the same mass in lower-density regions. All but the most massive halos in high-density regions are losing mass (i.e., being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low mass halos in high density regions at low redshifts {\$}z {\textless} 1{\$}, by preferentially removing higher angular momentum material from halos. Halos in low-density regions have lower than average spins because they lack nearby halos whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an Extreme Value Distribution, and that the density distribution becomes broader with cosmic time.}, -archivePrefix = {arXiv}, -arxivId = {1610.02108}, -author = {Lee, Christoph T and Primack, Joel R and Behroozi, Peter and Rodr{\'{i}}guez-Puebla, Aldo and Hellinger, Doug and Dekel, Avishai}, -doi = {10.1093/mnras/stw3348}, -eprint = {1610.02108}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology,Halos -Methods,Large Scale Structure -Dark Matter -Galaxies,Numerical}, -number = {4}, -pages = {3834--3858}, -title = {{Properties of dark matter haloes as a function of local environment density}}, -url = {http://arxiv.org/abs/1610.02108%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3348}, -volume = {466}, -year = {2017} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print)$\backslash$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Lee2016, -abstract = {We study how properties of discrete dark matter haloes depend on halo environment, characterized by the mass density around the haloes on scales from 0.5 to 16 h−1 Mpc. We find that low-mass haloes (those less massive than the characteristic mass MC of haloes collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations and rounder shapes than haloes in median density environments. Haloes in median- and low-density environments have similar accretion rates and concentrations, but haloes in low-density environments have lower spins and are more elongated. Haloes of a given mass in high-density regions accrete material earlier than haloes of the same mass in lower density regions. All but the most massive haloes in high-density regions are losing mass (i.e. being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low-mass haloes in high-density regions at low redshifts z {\textless} 1, by preferentially removing higher angular momentum material from haloes. Haloes in low-density regions have lower than average spins because they lack nearby haloes whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an extreme value distribution, and that the density distribution becomes broader with cosmic time.}, -archivePrefix = {arXiv}, -arxivId = {1610.02108}, -author = {Lee, Christoph T and Primack, Joel R and Behroozi, Peter and Rodr{\'{i}}guez-Puebla, Aldo and Hellinger, Doug and Dekel, Avishai}, -doi = {10.1093/mnras/stw3348}, -eprint = {1610.02108}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Large-scale structure of Universe,Methods: numerical}, -number = {4}, -pages = {3834--3858}, -title = {{Properties of dark matter haloes as a function of local environment density}}, -url = {http://arxiv.org/abs/1610.02108%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3348}, -volume = {466}, -year = {2017} -} -@article{Schombert2013, -abstract = {Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the S{\'{e}}rsic r 1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the S{\'{e}}rsic r 1/n model produces good fits to the core regions of ellipticals (r{\textless}r half), but is an inadequate function for the entire profile of an elliptical from core to halo due to competing effects on the S{\'{e}}rsic n index and the fact that the interior shape of an elliptical is only weakly correlated with its halo shape. In addition, there are a wide range of S{\'{e}}rsic parameters that will equally describe the shape of the outer profile, degrading the S{\'{e}}rsic model's usefulness as a describer of the entire profile. Empirically determined parameters, such as half-light radius and total luminosity, have less scatter than fitting function variables. The scaling relations for ellipticals are often non-linear, but for ellipticals brighter than MJ {\textless}-23 the following structural relations are found: L ∞ r 0.8±0.1, L ∞ $\Sigma$-0.5±0.1, and $\Sigma$ ∞ r -1.5±0.1. {\textcopyright}2013 Astronomical Society of Australia.}, -archivePrefix = {arXiv}, -arxivId = {1303.4710}, -author = {Schombert, J M}, -doi = {10.1017/pas.2013.010}, -eprint = {1303.4710}, -issn = {13233580}, -journal = {Publications of the Astronomical Society of Australia}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: star formation,galaxies: structure}, -number = {1}, -title = {{The structure of galaxies: II. Fitting functions and scaling relations for ellipticals}}, -url = {http://arxiv.org/abs/1303.4710%7B%5C%25%7D0Ahttp://dx.doi.org/10.1017/pas.2013.010}, -volume = {30}, -year = {2013} -} -@article{Hall2014a, -abstract = {Charge-Coupled Devices are the detector of choice for the focal planes of many optical and X-ray space telescopes. In recent years, EM-CCDs, SCDs and CMOS sensors have been used, or baselined, for missions in which the detection of X-ray and visible photons are key to the science goals of the mission. When placed in orbit, silicon-based detectors will suffer radiation damage as a consequence of the harsh space radiation environment, creating traps in the silicon. The radiation-induced traps will capture and release signal electrons, effectively "smearing" the image. Without correction, this smearing of the image would have major consequences on the science goals of the missions. Fitting to observed results, through careful planning of observation strategies while the radiation dose received remains low in the early stages of the mission, has previously been used to correct against the radiation damage effects. As the science goals becoming increasingly demanding, however, the correction algorithms require greater accuracy and a more physical approach is required, removing the effects of the radiation damage by modelling the trap capture and release mechanisms to a high level of detail. The drive for increasingly accurate trap parameters has led to the development of new methods of characterisation of traps in the silicon, measuring the trap properties and their effects to the single-trap level in situ. Here, we summarise the latest developments in trap characterisation techniques for n-channel and p-channel devices. ? 2014 SPIE.}, -author = {Hall, David J and Murray, Neil and Gow, Jason and Wood, Daniel and Holland, Andrew}, -doi = {10.1117/12.2055906}, -isbn = {9780819496225}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VI}, -keywords = {CTI,Defect,Euclid,Gaia,HST,N-channel,P,[CCD}, -number = {0}, -pages = {915408}, -title = {{ In situ trap parameter studies in CCDs for space applications }}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2055906}, -volume = {9154}, -year = {2014} -} -@article{Sales2012a, -abstract = {In the simplest scenario, disk galaxies form predominantly in halos with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly-rotating remnants of repeated merging events. We explore these assumptions using one hundred systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations GIMIC. At z=0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disk galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: disks form in halos with high and low net spin, and mergers play a negligible role in the formation of spheroid stars, most of which form in-situ. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly-accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Disks, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier-accreted material. Gas accretion from a hot corona thus favours disk formation, whereas gas that flows "cold", often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, most spheroids consist of superpositions of stellar components with distinct kinematics, age, and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology is imprinted early by the interplay of the tidal field and the shape of the material destined to form the galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 {\textless} z {\textless} 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J{\textless}inf{\textgreater}125{\textless}/inf{\textgreater}, i{\textless}inf{\textgreater}814{\textless}/inf{\textgreater}, v{\textless}inf{\textgreater}606{\textless}/inf{\textgreater} HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{Smith2012, -abstract = {We present a pan-chromatic analysis of an unprecedented sample of 1402 250 $\mu$m selected galaxies at z {\textless} 0.5 (z-=0.24) from the Herschel-ATLAS survey. We complement our Herschel 100-500$\mu$m data with UV-K-band photometry from the Galaxy And Mass Assembly (GAMA) survey and apply the magphys energy-balance technique to produce pan-chromatic spectral energy distributions (SEDs) for a representative sample of 250$\mu$m selected galaxies spanning the most recent 5 Gyr of cosmic history. We derive estimates of physical parameters, including star formation rates, stellar masses, dust masses and infrared (IR) luminosities. The typical H-ATLAS galaxy at z {\textless} 0.5 has a far-infrared luminosity in the range 10 10-10 12L ⊙ (SFR: 1-50 M ⊙yr -1) and thus is broadly representative of normal star-forming galaxies over this redshift range. We show that 250$\mu$m selected galaxies contain a larger mass of dust at a given IR luminosity or star formation rate than previous samples selected at 60$\mu$m from the IRAS. We derive typical SEDs for H-ATLAS galaxies, and show that the emergent SED shape is most sensitive to specific star formation rate. The optical-UV SEDs also become more reddened due to dust at higher redshifts. Our template SEDs are significantly cooler than existing IR templates. They may therefore be most appropriate for inferring total IR luminosities from moderate redshift sub-millimetre selected samples and for inclusion in models of the lower redshift sub-millimetre galaxy populations. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1208.3079}, -author = {Smith, D J B and Dunne, L and da Cunha, E and Rowlands, K and Maddox, S J and Gomez, H L and Bonfield, D G and Charlot, S and Driver, S P and Popescu, C C and Tuffs, R J and Dunlop, J S and Jarvis, M J and Seymour, N and Symeonidis, M and Baes, M and Bourne, N and Clements, D L and Cooray, A and {De Zotti}, G and Dye, S and Eales, S and Scott, D and Verma, A and van der Werf, P and Andrae, E and Auld, R and Buttiglione, S and Cava, A and Dariush, A and Fritz, J and Hopwood, R and Ibar, E and Ivison, R J and Kelvin, L and Madore, B F and Pohlen, M and Rigby, E E and Robotham, A and Seibert, M and Temi, P}, -doi = {10.1111/j.1365-2966.2012.21930.x}, -eprint = {1208.3079}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: starburst}, -number = {1}, -pages = {703--727}, -primaryClass = {astro-ph.CO}, -title = {{Herschel-ATLAS: Multi-wavelength SEDs and physical properties of 250 $\mu$m selected galaxies at z {\textless} 0.5}}, -volume = {427}, -year = {2012} -} -@article{Pearson2024, -abstract = {Bright galaxies at submillimetre wavelengths from Herschel are now well known to be predominantly strongly gravitationally lensed. The same models that successfully predicted this strongly lensed population also predict about 1 per cent of faint 450 $\mu$m-selected galaxies from deep James Clerk Maxwell Telescope (JCMT) surveys will also be strongly lensed. Follow-up ALMA campaigns have so far found one potential lens candidate, but without clear compelling evidence, for example, from lensing arcs. Here, we report the discovery of a compelling gravitational lens system confirming the lensing population predictions, with a zs = 3.4 ± 0.4 submm source lensed by a zspec = 0.360 foreground galaxy within the COSMOS field, identified through public JWST imaging of a 450 $\mu$m source in the SCUBA-2 Ultra Deep Imaging EAO Survey (STUDIES) catalogue. These systems will typically be well within the detectable range of future wide-field surveys such as Euclid and Roman, and since submillimetre galaxies are predominantly very red at optical/near-infrared wavelengths, they will tend to appear in near-infrared channels only. Extrapolating to the Euclid-Wide survey, we predict tens of thousands of strongly lensed near-infrared galaxies. This will be transformative for the study of dusty star-forming galaxies at cosmic noon, but will be a contaminant population in searches for strongly lensed ultra-high-redshift galaxies in Euclid and Roman.}, -archivePrefix = {arXiv}, -arxivId = {2309.00888}, -author = {Pearson, James and Serjeant, Stephen and Wang, Wei Hao and Gao, Zhen Kai and Babul, Arif and Chapman, Scott and Chen, Chian Chou and Clements, David L. and Conselice, Christopher J. and Dunlop, James and Fan, Lulu and Ho, Luis C. and Hwang, Ho Seong and Koprowski, Maciej and Micha{\l}owski, Micha{\l}J and Shim, Hyunjin}, -doi = {10.1093/mnras/stad3916}, -eprint = {2309.00888}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Pearson2024StrongLensJWST.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {galaxies: evolution,gravitational lensing: strong,infrared: galaxies,submillimetre: galaxies}, -number = {4}, -pages = {12044--12052}, -title = {{A large population of strongly lensed faint submillimetre galaxies in future dark energy surveys inferred from JWST imaging}}, -volume = {527}, -year = {2024} -} -@book{Boyd2018, -abstract = {This groundbreaking textbook combines straightforward explanations with a wealth of practical examples to offer an innovative approach to teaching linear algebra. Requiring no prior knowledge of the subject, it covers the aspects of linear algebra - vectors, matrices, and least squares - that are needed for engineering applications, discussing examples across data science, machine learning and artificial intelligence, signal and image processing, tomography, navigation, control, and finance. The numerous practical exercises throughout allow students to test their understanding and translate their knowledge into solving real-world problems, with lecture slides, additional computational exercises in Julia and MATLAB, and data sets accompanying the book online. It is suitable for both one-semester and one-quarter courses, as well as self-study, this self-contained text provides beginning students with the foundation they need to progress to more advanced study.}, -author = {Boyd, Stephen and Vandenberghe, Lieven}, -booktitle = {Introduction to Applied Linear Algebra}, -doi = {10.1017/9781108583664}, -file = {:C\:/Users/Jammy/Documents/Papers/linearalgebra.pdf:pdf}, -isbn = {9781316518960}, -title = {{Introduction to Applied Linear Algebra}}, -year = {2018} -} -@article{VanDerWel2012, -abstract = {We present global structural parameter measurements of 109,533 unique, H F160W-selected objects from the CANDELS multi-cycle treasury program. S{\'{e}}rsic model fits for these objects are produced with GALFIT in all available near-infrared filters (H F160W, J F125W and, for a subset, Y F105W). The parameters of the best-fitting S{\'{e}}rsic models (total magnitude, half-light radius, S{\'{e}}rsic index, axis ratio, and position angle) are made public, along with newly constructed point-spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties, we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements - to 10% or better - of all structural parameters can typically be obtained for galaxies with H F160W < 23, with comparable fidelity for basic size and shape measurements for galaxies to H F160W ∼ 24.5. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1211.6954}, -author = {{Van Der Wel}, A. and Bell, E. F. and H{\"{a}}ussler, B. and McGrath, E. J. and Chang, Yu Yen and Guo, Yicheng and McIntosh, D. H. and Rix, H. W. and Barden, M. and Cheung, E. and Faber, S. M. and Ferguson, H. C. and Galametz, A. and Grogin, N. A. and Hartley, W. and Kartaltepe, J. S. and Kocevski, D. D. and Koekemoer, A. M. and Lotz, J. and Mozena, M. and Peth, M. A. and Peng, Chien Y.}, -doi = {10.1088/0067-0049/203/2/24}, -eprint = {1211.6954}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Van Der Wel et al. - 2012 - Structural parameters of galaxies in candels.pdf:pdf}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: high-redshift,galaxies: statistics,galaxies: structure surveys}, -number = {2}, -title = {{Structural parameters of galaxies in candels}}, -volume = {203}, -year = {2012} -} -@article{Lilly2016, -abstract = {There are very strong observed correlations between the specific star-formation rates (sSFR) of galaxies and their mean surface mass densities, {\Sigma}, as well as other aspects of their internal structure. These strong correlations have often been taken to indicate that the internal structure of a galaxy must play a major physical role, directly or indirectly, in the control of star-formation. In this paper we show by means of a very simple toy model that these correlations can arise naturally without any such physical role once the observed evolution of the size-mass relation for star-forming galaxies is taken into account. In particular, the model reproduces the sharp threshold in {\Sigma} between galaxies that are star-forming and those that are quenched, and the evolution of this threshold with redshift. Similarly, it produces iso-quenched-fraction contours in the ${f_Q(m,R_e)}$ plane that are almost exactly parallel to lines of constant {\Sigma} for centrals and shallower for satellites. It does so without any dependence on quenching on size or {\Sigma}, and without invoking any differences between centrals and satellites, beyond the different mass-dependences of their quenching laws. The toy-model also reproduces several other observations, including the sSFR gradients within galaxies and the appearance of inside-out build-up of passive galaxies. Finally, it is shown that curvature in the Main Sequence sSFR-mass relation can produce curvature in the apparent B/T ratios with mass. Our analysis therefore suggests that many of the strong correlations that are observed between galaxy structure and sSFR may well be a consequence of things unrelated to quenching and should not be taken as evidence of the physical processes that drive quenching.}, -archivePrefix = {arXiv}, -arxivId = {1604.06459}, -author = {Lilly, Simon J. and Carollo, C. Marcella}, -doi = {10.3847/0004-637x/833/1/1}, -eprint = {1604.06459}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lilly, Carollo - 2016 - Surface Density Effects in Quenching Cause or Effect.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {1}, -pmid = {15540530}, -title = {{Surface Density Effects in Quenching: Cause or Effect?}}, -url = {http://arxiv.org/abs/1604.06459%0Ahttp://dx.doi.org/10.3847/0004-637X/833/1/1}, -volume = {833}, -year = {2016} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z{\textgreater}1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AGN) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z 5 and a star formation rate density which rises at least out to z 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -publisher = {MNRAS}, -title = {{Breaking the hierarchy of galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0511338%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2006.10519.x}, -volume = {370}, -year = {2006} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance $\Lambda$ cold dark matter cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for 'radio' feedback from those active galactic nuclei that lie at the centre of a quasi-static X-ray-emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models that might explain the accretion rate scalings required for our phenomenological 'radio mode' model to be successful. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J. and Springel, Volker and White, Simon D.M. and {De Lucia}, G. and Frenk, C. S. and Gao, L. and Jenkins, A. and Kauffmann, G. and Navarro, J. F. and Yoshida, N.}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Croton et al. - 2006 - The many lives of active galactic nuclei Cooling flows, black holes and the luminosities and colours of galaxi(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Heckman2014, -abstract = {We summarize what large surveys of the contemporary Universe have taught us about the physics and phenomenology of the processes that link the formation and evolution of galaxies with their central supermassive black holes. We present a picture in which the population of active galactic nuclei (AGNs) can be divided into two distinct populations. The radiative-mode AGNs are associated with black holes (BHs) that produce radiant energy powered by accretion at rates in excess of ∼1% of the Eddington limit. They are primarily associated with less massive BHs growing in high-density pseudobulges at a rate sufficient to produce the total mass budget in these BHs in ∼10 Gyr. The circumnuclear environment contains high-density cold gas and associated star formation. Major mergers are not the primary mechanism for transporting this gas inward; secular processes appear dominant. Stellar feedback is generic in these objects, and strong AGN feedback is seen only in the most powerful AGNs. In jet-mode AGNs the bulk of energetic output takes the form of collimated outflows (jets). These AGNs are associated with the more massive BHs in more massive (classical) bulges and elliptical galaxies. Neither the accretion onto these BHs nor star formation in their host bulge is significant today. These AGNs are probably fueled by the accretion of slowly cooling hot gas that is limited by the feedback/heating provided by AGN radio sources. Surveys of the high-redshift Universe paint a similar picture. Noting that the volume-averaged ratio of star formation to BH growth has remained broadly constant over the past 10 Gyrs, we argue that the processes that linked the cosmic evolution of galaxies and BHs are still at play today. Copyright {\textcopyright} 2014 by Annual Reviews.}, -archivePrefix = {arXiv}, -arxivId = {1403.4620}, -author = {Heckman, Timothy M. and Best, Philip N.}, -doi = {10.1146/annurev-astro-081913-035722}, -eprint = {1403.4620}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Heckman, Best - 2014 - The coevolution of galaxies and supermassive black holes Insights from surveys of the contemporary universe.pdf:pdf}, -issn = {00664146}, -journal = {Annual Review of Astronomy and Astrophysics}, -keywords = {QSOs,Seyfert galaxies,active galactic nuclei,quasi-stellar objects,radio galaxies}, -number = {1}, -pages = {589--660}, -title = {{The coevolution of galaxies and supermassive black holes: Insights from surveys of the contemporary universe}}, -volume = {52}, -year = {2014} -} -@article{Griffiths2019, -abstract = {We report an embarrassingly parallel method for the evaluation of thermodynamic properties over an energy landscape exhibiting broken ergodicity, nested is the likelihood of the observed data D givenbasin-sampling (NBS). We also introduce the No Galilean U-Turn Sampler (NoGUTS), a new sampling scheme based on the No U-Turn Sampler (NUTS) introduced by Hoffman and Gelman (2014) that works with the Galilean Monte Carlo scheme introduced by Betancourt (2012) to aid the efficient generation of new live points. NoGUTS can be thought of as a form of reflective slice sampling with an automatic stopping criterion. We apply this approach to a benchmark atomic cluster of 31 Lennard-Jones atoms, which exhibits a low temperature solid-solid heat capacity peak. The calculated heat capacity is compared with results generated by parallel tempering (PT), basin-sampling parallel tempering (BSPT), and standard nested sampling (NS) simulations. NBS reproduces the full heat capacity curve predicted by PT and BSPT, while the NS calculation with similar computational cost fails to resolve the low-temperature solid-solid phase transition.}, -author = {Griffiths, Matthew and Wales, David J.}, -doi = {10.1021/acs.jctc.9b00567}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Griffiths, Wales - 2019 - Nested Basin-Sampling.pdf:pdf}, -issn = {15499626}, -journal = {Journal of Chemical Theory and Computation}, -number = {12}, -pages = {6865--6881}, -pmid = {31557432}, -title = {{Nested Basin-Sampling}}, -volume = {15}, -year = {2019} -} -@article{Schramm1990, -abstract = {Gravitational lensing of the cosmic microwave background by large-scale structure in the late universe is both a source of cosmological information and a potential contaminant of primordial gravity waves. Because lensing imprints growth of structure in the late universe on the CMB, measurements of CMB lensing will constrain parameters to which the CMB would not otherwise be sensitive, such as neutrino mass. In CMB polarization, gravitational lensing is the largest guaranteed source of Bmode (or curl-like) polarization. Future CMB polarization experiments with sufficient sensitivity to measure B-modes on small angular scales (l ̃ 1000) can measure lensing with better sensitivity, and on different scales, than could be achieved by measuring CMB temperature alone. If the instrumental noise is sufficiently small (≤ 5 $\mu$K-arcmin), the gravitational lensing contribution to the large-scale B-mode will be the limiting source of contamination when constraining a stochastic background of gravity waves in the early universe, one of the most exciting prospects for future CMB polarization experiments. High-sensitivity measurements of small-scale B-modes can reduce this contamination through a lens reconstruction technique that separates the lensing and primordial contributions to the B-mode on large scales. A fundamental design decision for a future CMB polarization experiment such as CMBpol is whether to have coarse angular resolution so that only the large-scale Bmode (and the large-scale E-mode from reionization) is measured, or high resolution to additionally measure CMB lensing. The purpose of this white paper is to evaluate the science case for CMB lensing in polarization: constraints on cosmological parameters, increased sensitivity to the gravity wave B-mode via lens reconstruction, expectedlevel of contamination from non-CMB foregrounds, and required control of beam systematics. {\textcopyright} 2009 American Institute of Physics.}, -archivePrefix = {arXiv}, -arxivId = {1010.3829}, -author = {Smith, Kendrick M. and Cooray, Asantha and Das, Sudeep and Dor{\'{e}}, Olivier and Hanson, Duncan and Hirata, Chris and Kaplinghat, Manoj and Keating, Brian and LoVerde, Marilena and Miller, Nathan and Rocha, Gra{\c{c}}a and Shimon, Meir and Zahn, Oliver}, -doi = {10.1063/1.3160886}, -eprint = {1010.3829}, -isbn = {9780735406780}, -issn = {0094243X}, -journal = {AIP Conference Proceedings}, -number = {23}, -pages = {121--178}, -pmid = {730073}, -title = {{Gravitational lensing}}, -url = {http://www.sciencedirect.com/science/article/pii/S037015730000082X%5Cnhttp://arxiv.org/abs/1010.3829%5Cnhttp://stacks.iop.org/0264-9381/27/i=23/a=233001?key=crossref.44713e6ff0001383bbf8c4f2e031bf76}, -volume = {1141}, -year = {2009} -} -@inproceedings{MartinNavarro2013, -author = {Mart$\backslash$'$\backslash$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Wertz2018, -abstract = {Modern time-delay cosmography aims to infer the cosmological parameters with a competitive precision from observing a multiply imaged quasar. The success of this technique relies upon a robust modeling of the lens mass distribution. Unfortunately strong degeneracies between density profiles that lead to almost the same lensing observables may bias precise estimates of the Hubble constant. The source position transformation (SPT), which covers the well-known mass-sheet transformation (MST) as a special case, defines a new framework to investigate these degeneracies. In this paper, we present pySPT, a python package dedicated to the SPT. We describe how it can be used to evaluate the impact of the SPT on lensing observables. We review most of its capabilities and elaborate on key features that we used in a companion paper regarding SPT and time delays. The pySPT program also comes with a subpackage dedicated to simple lens modeling. This can be used to generate lensing related quantities for a wide variety of lens models independent of any SPT analysis. As a first practical application, we present a correction to the first estimate of the impact on time delays of the SPT, which has been experimentally found in a previous work between a softened power law and composite (baryons + dark matter) lenses. We find that the large deviations previously predicted have been overestimated because of a minor bug in the public lens modeling code lensmodel (v1.99), which is now fixed. We conclude that the predictions for the Hubble constant deviate by ∼7{\%}, first and foremost as a consequence of an MST. The latest version of pySPT is available on Github, a software development platform, along with some tutorials to describe in detail how making the best use of pySPT.}, -archivePrefix = {arXiv}, -arxivId = {1801.04151}, -author = {Wertz, Olivier and Orthen, Bastian}, -doi = {10.1051/0004-6361/201732242}, -eprint = {1801.04151}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Cosmological parameters,Gravitational lensing: Strong}, -pages = {A117}, -title = {{A dedicated source-position transformation package: PySPT}}, -url = {http://arxiv.org/abs/1801.04151%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201732242}, -volume = {619}, -year = {2018} -} -@article{Schawinski2014, -abstract = {We use SDSS+GALEX+Galaxy Zoo data to study the quenching of star formation in lowredshift galaxies. We show that the green valley between the blue cloud of star-forming galaxies and the red sequence of quiescent galaxies in the colour-mass diagram is not a single transitional state through which most blue galaxies evolve into red galaxies. Rather, an analysis that takes morphology into account makes clear that only a small population of blue early-type galaxies move rapidly across the green valley after the morphologies are transformed from disc to spheroid and star formation is quenched rapidly. In contrast, the majority of blue star-forming galaxies have significant discs, and they retain their late-type morphologies as their star formation rates decline very slowly. We summarize a range of observations that lead to these conclusions, including UV-optical colours and halo masses, which both show a striking dependence on morphological type. We interpret these results in terms of the evolution of cosmic gas supply and gas reservoirs. We conclude that late-type galaxies are consistent with a scenario where the cosmic supply of gas is shut off, perhaps at a critical halo mass, followed by a slow exhaustion of the remaining gas over several Gyr, driven by secular and/or environmental processes. In contrast, early-type galaxies require a scenario where the gas supply and gas reservoir are destroyed virtually instantaneously, with rapid quenching accompanied by a morphological transformation from disc to spheroid. This gas reservoir destruction could be the consequence of a major merger, which in most cases transforms galaxies from disc to elliptical morphology, and mergers could play a role in inducing black hole accretion and possibly active galactic nuclei feedback. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1402.4814}, -author = {Schawinski, Kevin and Urry, C. Megan and Simmons, Brooke D. and Fortson, Lucy and Kaviraj, Sugata and Keel, William C. and Lintott, Chris J. and Masters, Karen L. and Nichol, Robert C. and Sarzi, Marc and Skibba, Ramin and Treister, Ezequiel and Willett, Kyle W. and Wong, O. Ivy and Yi, Sukyoung K.}, -doi = {10.1093/mnras/stu327}, -eprint = {1402.4814}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Active,Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,Galaxies: Spiral}, -month = {may}, -number = {1}, -pages = {889--907}, -title = {{The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early-and late-type galaxies}}, -volume = {440}, -year = {2014} -} -@article{Shu2017, -abstract = {We present the full sample of 118 galaxy-scale strong-lens candidates in the Sloan Lens ACS (SLACS) Survey for the Masses (S4TM) Survey, which are spectroscopically selected from the final data release of the Sloan Digital Sky Survey. Follow-up Hubble Space Telescope ( HST ) imaging observations confirm that 40 candidates are definite strong lenses with multiple lensed images. The foreground-lens galaxies are found to be early-type galaxies (ETGs) at redshifts 0.06–0.44, and background sources are emission-line galaxies at redshifts 0.22–1.29. As an extension of the SLACS Survey, the S4TM Survey is the first attempt to preferentially search for strong-lens systems with relatively lower lens masses than those in the pre-existing strong-lens samples. By fitting HST data with a singular isothermal ellipsoid model, we find that the total projected mass within the Einstein radius of the S4TM strong-lens sample ranges from 3 × 10 10 M ⊙ to 2 × 10 11 M ⊙ . In Shu et al., we have derived the total stellar mass of the S4TM lenses to be 5 × 10 10 M ⊙ to 1 × 10 12 M ⊙ . Both the total enclosed mass and stellar mass of the S4TM lenses are on average almost a factor of 2 smaller than those of the SLACS lenses, which also represent the typical mass scales of the current strong-lens samples. The extended mass coverage provided by the S4TM sample can enable a direct test, with the aid of strong lensing, for transitions in scaling relations, kinematic properties, mass structure, and dark-matter content trends of ETGs at intermediate-mass scales as noted in previous studies.}, -archivePrefix = {arXiv}, -arxivId = {1711.00072}, -author = {Shu, Yiping and Brownstein, Joel R. and Bolton, Adam S. and Koopmans, L{\'{e}}on V. E. and Treu, Tommaso and Montero-Dorta, Antonio D. and Auger, Matthew W. and Czoske, Oliver and Gavazzi, Rapha{\"{e}}l and Marshall, Philip J. and Moustakas, Leonidas A.}, -doi = {10.3847/1538-4357/aa9794}, -eprint = {1711.00072}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Shu2018SLACS4Mass.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -number = {1}, -pages = {48}, -title = {{The Sloan Lens ACS Survey. XIII. Discovery of 40 New Galaxy-scale Strong Lenses ∗}}, -volume = {851}, -year = {2017} -} -@article{Harvey2015, -abstract = {Collisions between galaxy clusters provide a test of the nongravitational forces acting on dark matter. Dark matter's lack of deceleration in the "bullet cluster" collision constrained its self-interaction cross section $\sigma$DM/m {\textless} 1.25 square centimeters per gram (cm2/g) [68{\%} confidence limit (CL)] ($\sigma$DM, self-interaction cross section; m, unit mass of dark matter) for long-ranged forces. Using the Chandra and Hubble Space Telescopes, we have now observed 72 collisions, including both major and minor mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6s significance. The position of the dark mass has remained closely aligned within 5.8 T 8.2 kiloparsecs of associated stars, implying a self-interaction cross section $\sigma$DM/m {\textless} 0.47 cm2/g (95{\%} CL) and disfavoring some proposed extensions to the standard model.}, -archivePrefix = {arXiv}, -arxivId = {1503.07675}, -author = {Harvey, David and Massey, Richard and Kitching, Thomas and Taylor, Andy and Tittley, Eric}, -doi = {10.1126/science.1261381}, -eprint = {1503.07675}, -issn = {10959203}, -journal = {Science}, -number = {6229}, -pages = {1462--1465}, -pmid = {25814581}, -title = {{The nongravitational interactions of dark matter in colliding galaxy clusters}}, -volume = {347}, -year = {2015} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the LambdaCDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no statistically significant detection of a stellar halo, as in the case of M101, NGC3351 and NGC1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction f{\_}SH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming and assemble their dark matter halos on average earlier than galaxies with similar stellar masses. Accreted satellites are also lower in stellar mass and have earlier infall times than centrals with high f{\_}SH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretion-dominated r{\$\sim${}}45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers only at higher redshifts and evolved relatively unperturbed in the last {\$\sim${}}10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M and Sales, Laura V and Creasey, Peter and Cooper, Michael C and Bullock, James S and {Michael Rich}, R and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Chabrier2003, -abstract = {We review recent determinations of the present day and initial mass functions in various components of the Galaxy, disk, spheroid, young and globular clusters. As a general feature, the IMF is well described by a power-law form for $m\ga 1 \msol$ and a lognormal form below. The extension of the disk IMF into the brown dwarf (BD) regime is in good agreement with observations and yields a disk BD number-density comparable to the stellar one $\sim 0.1 \pc3$. The IMF of young clusters is found to be consistent with the disk field IMF, providing the same correction for unresolved binaries. The spheroid IMF relies on much less robust grounds. Within all the uncertainties, it is found to be similar to the one derived for globular clusters, and is well represented also by a lognormal form with a characteristic mass slightly larger than for the disk. The IMF characteristic of early star formation remains undetermined, but different observational constraints suggest that it does not extend below $\sim 1 \msol$. These IMFs allow a reasonably robust determination of the Galactic present-day and initial stellar and brown dwarf contents. They also have important galactic implications in yielding more accurate mass-to-light ratio determinations. The M/L ratios obtained with the disk and the spheroid IMF yield values 1.8 and 1.4 smaller than a Salpeter IMF, respectively. This general IMF determination is examined in the context of star formation theory. (shortened)}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0304382}, -author = {Chabrier, Gilles}, -doi = {10.1086/376392}, -eprint = {0304382}, -isbn = {10.1086/376392}, -issn = {0004-6280}, -journal = {Publications of the Astronomical Society of the Pacific}, -keywords = {Galaxies: Luminosity Function,Invited Reviews,Mass Function}, -month = {jul}, -number = {809}, -pages = {763--795}, -pmid = {26438271}, -primaryClass = {astro-ph}, -title = {{Galactic Stellar and Substellar Initial Mass Function}}, -url = {http://arxiv.org/abs/astro-ph/0304382%0Ahttp://dx.doi.org/10.1086/376392}, -volume = {115}, -year = {2003} -} -@article{Baugh:1996aa, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -month = {dec}, -number = {4}, -pages = {1361--1378}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -url = {http://adsabs.harvard.edu/abs/1996MNRAS.283.1361B}, -volume = {283}, -year = {1996} -} -@article{MacArthur2009a, -abstract = {We present a detailed study of the stellar populations (SPs) and kinematics of the bulge and inner disc regions of eight nearby spiral galaxies (Sa-Sd) based on deep Gemini/GMOS data. The long-slit spectra extend to 1-2 disc scalelengths with S/N/{\AA}≥ 50. Several different model fitting techniques involving absorption-line indices and full spectrum fitting are explored, and found to weigh age, metallicity and abundance ratios differently. We find that the SPs of spiral galaxies are not well matched by single episodes of star formation; more representative SPs must involve average SP values integrated over the star formation history (SFH) of the galaxy. Our 'full population synthesis' method is an optimized linear combination of model templates to the full spectrum with masking of regions poorly represented by the models. Realistic determinations of the SP parameters and kinematics (rotation and velocity dispersion) also rely on careful attention to data/model matching (resolution and flux calibration). The population fits reveal a wide range of age and metallicity gradients (from negative to positive) in the bulge, allowing for diverse formation mechanisms. The observed positive age gradients within the effective radius of some late-type bulges helps reconcile the long-standing conundrum of the coexistence of secular-like kinematics, light profile shape and stellar bar with the 'classical'-like old and $\alpha$-enhanced SPs in the Milky Way bulge. The discs, on the other hand, almost always show mildly decreasing to flat profiles in both age and metallicity, consistent with inside-out formation. Our spiral bulges follow the same correlations of increasing light-weighted age and metallicity with central velocity dispersion as those of elliptical galaxies and early-type bulges found in other studies, but when SFHs more complex and realistic than a single burst are invoked, the trend with age is shallower and the scatter much reduced. In a mass-weighted context, however, all bulges are predominantly composed of old and metal-rich SPs. While secular contributions to the evolution of many of our bulges are clearly evident, with young (0.001-1 Gyr) SPs contributing as much as 90 per cent of the optical (V-band) light, the bulge mass fraction from young stars is small (≲25 per cent). The implies a bulge formation dominated by early processes that are common to all spheroids, whether they currently reside in discs or not. While monolithic collapse cannot be ruled out in some cases, merging must be invoked to explain the SP gradients in most bulges. Further bulge growth via secular processes or 'rejuvenated' star formation generally contributes minimally to the stellar mass budget, with the relative secular weight increasing with decreasing central velocity dispersion. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4135}, -author = {MacArthur, Lauren A and Gonz{\'{a}}lez, J Jes{\'{u}}s and Courteau, St{\'{e}}phane}, -doi = {10.1111/j.1365-2966.2009.14519.x}, -eprint = {0901.4135}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: spiral,Galaxies: stellar content}, -number = {1}, -pages = {28--63}, -title = {{Stellar population and kinematic profiles in spiral bulges and discs: Population synthesis of integrated spectra}}, -volume = {395}, -year = {2009} -} -@article{Ness2015, -abstract = {New spectroscopic surveys offer the promise of consistent stellar parameters and abundances ('stellar labels') for hundreds of thousands of stars in the Milky Way: this poses a formidable spectral modeling challenge. In many cases, there is a sub-set of reference objects for which the stellar labels are known with high(er) fidelity. We take advantage of this with The Cannon, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the 'known' labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with Teff, log g and [Fe/H] as the labels, and then applying it to the spectra of 56,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.}, -archivePrefix = {arXiv}, -arxivId = {1501.07604}, -author = {Ansorge, Frank and Stigler, Thomas and Heumann, Katja and Ifland, David and Reichl, Herbert}, -doi = {10.1088/0004-637X/808/1/16}, -eprint = {1501.07604}, -issn = {15384357}, -journal = {Smart Systems Integration 2010 - 4th European Conference and Exhibition on Integration Issues of Miniaturized Systems - MEMS, MOEMS, ICs and Electronic Components}, -keywords = {methods: data analysis,methods: statistical,stars: abundances,stars: fundamental parameters,surveys,techniques: spectroscopic}, -number = {1}, -pages = {1--45}, -title = {{Embedding of electronic and system in package using added manufacturing technologies}}, -volume = {808}, -year = {2010} -} -@article{2001fa, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M{\_}*/M{\_}sun) {\textgreater} 11.5 (M{\_}K {\textless} -25.3 mag) and distance D {\textless} 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38$\backslash$pm6{\%} down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80$\backslash$pm10{\%} and 28$\backslash$pm6{\%}, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R{\_}e), and the gas morphologies are diverse, with 17/28 = 61$\backslash$pm9{\%} being centrally concentrated, 8/28 = 29$\backslash$pm9{\%} exhibiting clear rotation out to several kpc, and 3/28 = 11$\backslash$pm6{\%} being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly {\$\sim${}}10{\^{}}5M{\_}sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A and Blakeslee, John P and Goulding, Andy D and McConnell, Nicholas J and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {https://ui.adsabs.harvard.edu/%7B%5C#%7Dabs/2009Natur.457..451D/abstract}, -volume = {457}, -year = {2009} -} -@article{Gebhardt2011, -abstract = {We present the stellar kinematics in the central 2″ of the luminous elliptical galaxy M87 (NGC 4486), using laser adaptive optics to feed the Gemini telescope integral-field spectrograph, Near-infrared Integral Field Spectrograph (NIFS). The velocity dispersion rises to 480km s-1 at 02. We combine these data with extensive stellar kinematics out to large radii to derive a black hole mass equal to (6.6 0.4) × 109 M⊙, using orbit-based axisymmetric models and including only the NIFS data in the central region. Including previously reported ground-based data in the central region drops the uncertainty to 0.25 × 109 M⊙ with no change in the best-fit mass; however, we rely on the values derived from the NIFS-only data in the central region in order to limit systematic differences. The best-fit model shows a significant increase in the tangential velocity anisotropy of stars orbiting in the central region with decreasing radius, similar to that seen at the centers of other core galaxies. The black hole mass is insensitive to the inclusion of a dark halo in the models - the high angular resolution provided by the adaptive optics breaks the degeneracy between black hole mass and stellar mass-to-light ratio. The present black hole mass is in excellent agreement with the Gebhardt & Thomas value, implying that the dark halo must be included when the kinematic influence of the black hole is poorly resolved. This degeneracy implies that the black hole masses of luminous core galaxies, where this effect is important, may need to be re-evaluated. The present value exceeds the prediction of the black hole-dispersion and black hole-luminosity relations, both of which predict about 1 × 109 M for M87, by close to twice the intrinsic scatter in the relations. The high end of the black hole correlations may be poorly determined at present. {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1101.1954}, -author = {Gebhardt, Karl and Adams, Joshua and Richstone, Douglas and Lauer, Tod R. and Faber, S. M. and G{\"{u}}ltekin, Kayhan and Murphy, Jeremy and Tremaine, Scott}, -doi = {10.1088/0004-637X/729/2/119}, -eprint = {1101.1954}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gebhardt et al. - 2011 - The black hole mass in M87 from GeminiNIFS adaptive optics observations(2).pdf:pdf}, -isbn = {0004-637X}, -issn = {15384357}, -journal = {ApJ}, -keywords = {NGC 4486),cD,galaxies: elliptical and lenticular,galaxies: individual (M87,galaxies: kinematics and dynamics}, -number = {2}, -pages = {1--12}, -title = {{The black hole mass in M87 from Gemini/NIFS adaptive optics observations}}, -volume = {729}, -year = {2011} -} -@article{Morishita2018, -abstract = {Observations have revealed massive (logM*/Msun>11) galaxies that were already dead when the universe was only $\sim$2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6 50% of their extant masses by $\sim$1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of $\sim$0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z$\sim$5.5 to $\sim$2.2 at a rate of $\sim$0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, $\sim$0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T. and Abramson, L. E. and Treu, T. and Brammer, G. B. and Jones, T. and Kelly, P. and Stiavelli, M. and Trenti, M. and Vulcani, B. and Wang, X.}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Morishita et al. - 2019 - Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enr(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Wagner-Carena2021, -abstract = {In the past few years, approximate Bayesian Neural Networks (BNNs) have demonstrated the ability to produce statistically consistent posteriors on a wide range of inference problems at unprecedented speed and scale. However, any disconnect between training sets and the distribution of real-world objects can introduce bias when BNNs are applied to data. This is a common challenge in astrophysics and cosmology, where the unknown distribution of objects in our Universe is often the science goal. In this work, we incorporate BNNs with flexible posterior parameterizations into a hierarchical inference framework that allows for the reconstruction of population hyperparameters and removes the bias introduced by the training distribution. We focus on the challenge of producing posterior PDFs for strong gravitational lens mass model parameters given Hubble Space Telescope (HST) quality single-filter, lens-subtracted, synthetic imaging data. We show that the posterior PDFs are sufficiently accurate (i.e., statistically consistent with the truth) across a wide variety of power-law elliptical lens mass distributions. We then apply our approach to test data sets whose lens parameters are drawn from distributions that are drastically different from the training set. We show that our hierarchical inference framework mitigates the bias introduced by an unrepresentative training set's interim prior. Simultaneously, given a sufficiently broad training set, we can precisely reconstruct the population hyperparameters governing our test distributions. Our full pipeline, from training to hierarchical inference on thousands of lenses, can be run in a day. The framework presented here will allow us to efficiently exploit the full constraining power of future ground- and space-based surveys.}, -archivePrefix = {arXiv}, -arxivId = {2010.13787}, -author = {Wagner-Carena, Sebastian and Park, Ji Won and Birrer, Simon and Marshall, Philip J. and Roodman, Aaron and Wechsler, Risa H.}, -doi = {10.3847/1538-4357/abdf59}, -eprint = {2010.13787}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/WagnerCarena2021BNNHierachical.pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Strong gravitational lensing,Cosmology,Computation}, -number = {2}, -pages = {187}, -publisher = {IOP Publishing}, -title = {{Hierarchical Inference with Bayesian Neural Networks: An Application to Strong Gravitational Lensing}}, -url = {http://dx.doi.org/10.3847/1538-4357/abdf59}, -volume = {909}, -year = {2021} -} -@article{Du2019, -abstract = {We develop an analytic mass model for lensing galaxies, based on a broken power-law (BPL) density profile, which is a power-law profile with a mass deficit or surplus in the central region. Under the assumption of an elliptically symmetric surface mass distribution, the deflection angle and magnification can be evaluated analytically for this new model. We compute the theoretical prediction for various quantities, including the volume and surface mass density profiles of the galaxies, and the aperture and luminosity-weighted line-of-sight velocity dispersions, and compare them to those measured from the Illustris simulation. We find an excellent agreement between our model prediction and the simulation, which validates our modeling. The high efficiency and accuracy of our model manifests itself as a promising tool for studying properties of galaxies with strong lensing.}, -archivePrefix = {arXiv}, -arxivId = {1911.11761}, -author = {Du, Wei and Zhao, Gong-Bo and Fan, Zuhui and Shu, Yiping and Li, Ran and Mao, Shude}, -doi = {10.3847/1538-4357/ab7a15}, -eprint = {1911.11761}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {dark matter,galaxies,gravitational lensing,halos,kinematics and dynamics}, -number = {1}, -pages = {62}, -title = {{An Accurate Analytic Mass Model for Lensing Galaxies}}, -url = {http://arxiv.org/abs/1911.11761}, -volume = {892}, -year = {2020} -} -@article{Weinberg2002, -abstract = {Simulations predict that the dark matter halos of galaxies should have central cusps, while those inferred from observed galaxies do not have cusps. We demonstrate, using both linear perturbation theory and n-body simulations, that a disk bar, which should be ubiquitous in forming galaxies, can produce cores in cuspy CDM dark matter profiles within five bar orbital times. Simulations of forming galaxies suggest that one of Milky Way size could have a 10 kpc primordial bar; this bar will remove the cusp out to approximately 5 kpc in approximately 1.5 gigayears, while the disk only loses approximately 8% of its original angular momentum. An inner Lindblad-like resonance couples the rotating bar to orbits at all radii through the cusp, transferring the bar pattern angular momentum to the dark matter cusp, rapidly flattening it. This resonance disappears for profiles with cores and is responsible for a qualitative difference in bar driven halo evolution with and without a cusp. This bar induced evolution will have a profound effect on the structure and evolution of almost all galaxies. Hence, both to understand galaxy formation and evolution and to make predictions from theory it is necessary to resolve these dynamical processes. Unfortunately, correctly resolving these important dynamical processes in ab initio calculations of galaxy formation is a daunting task, requiring at least 4,000,000 halo particles using our SCF code, and probably requiring many times more particles when using noisier tree, direct summation, or grid based techniques, the usual methods employed in such calculations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0110632}, -author = {Weinberg, Martin D. and Katz, Neal}, -doi = {10.1086/343847}, -eprint = {0110632}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Theory,Galaxies: Evolution,Galaxies: Halos,Galaxies: Kinematics and Dynamics}, -month = {dec}, -number = {2}, -pages = {627--633}, -primaryClass = {astro-ph}, -title = {{Bar‐driven Dark Halo Evolution: A Resolution of the Cusp‐Core Controversy}}, -url = {http://stacks.iop.org/0004-637X/580/i=2/a=627}, -volume = {580}, -year = {2002} -} -@article{Nightingalea, -author = {Nightingale, James and Dye, Simon}, -journal = {---}, -pages = {0}, -title = {{Density Profile Decomposition of ER 0047-2808}}, -volume = {000} -} -@article{Vika2014, -abstract = {Bulge-disc decomposition is a valuable tool for understanding galaxies. However, achieving robust measurements of component properties is difficult, even with high-quality imaging, and it becomes even more so with the imaging typical of large surveys. In this paper, we consider the advantages of a new, multiband approach to galaxy fitting. We perform automated bulge-disc decompositions for 163 nearby galaxies, by simultaneously fitting multiple images taken in five photometric filters. We show that we are able to recover structural measurements that agree well with various other works, and confirm a number of key results. We additionally use our results to illustrate the link between total S{\'{e}}rsic index and bulge-disc structure, and demonstrate that the visually classification of lenticular galaxies is strongly dependent on the inclination of their disc component. By simulating the same set of galaxies as they would appear if observed at a range of redshifts, we are able to study the behaviour of bulge-disc decompositions as data quality diminishes. We examine how our multiband fits perform, and compare to the results of more conventional, single-band methods.Multiband fitting improves the measurement of all parameters, but particularly the bulge-to-total flux ratio and component colours. We therefore encourage the use of this approach with future surveys.}, -archivePrefix = {arXiv}, -arxivId = {1408.4070}, -author = {Vika, Marina and Bamford, Steven P. and H{\"{a}}u{\ss}ler, Boris and Rojas, Alex L.}, -doi = {10.1093/mnras/stu1696}, -eprint = {1408.4070}, -isbn = {978-054-922-7717717}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure,Methods: data analysis,Techniques: image processing}, -month = {nov}, -number = {4}, -pages = {3603--3621}, -pmid = {11747826}, -title = {{MegaMorph - multiwavelength measurement of galaxy structure: Physically meaningful bulge-disc decomposition of galaxies near and far}}, -volume = {444}, -year = {2014} -} -@article{Shirazi2013, -abstract = {We present an analysis of near-infrared integral field unit spectroscopy of the 8 o'clock arc, a gravitationally lensed Lyman break galaxy, taken with SINFONI. We explore the shape of the spatially resolved H$\beta$ profile and demonstrate that we can decompose it into three components that partially overlap (spatially) but are distinguishable when we include dynamical information. We use existing B and H imaging from the Hubble Space Telescope to construct a rigorous lens model using a Bayesian grid-based lens modelling technique. We apply this lens model to the SINFONI data cube to construct the de-lensed H$\beta$ line-flux velocity and velocity dispersion maps of the galaxy. We find that the 8 o'clock arc has a complex velocity field that is not simply explained by a single rotating disc. The H$\beta$ profile of the galaxy shows a blueshifted wing suggesting gas outflows of $\sim$200 km s-1. We confirm that the 8 o'clock arc lies on the stellar mass-oxygen abundance-star formation rate plane found locally, but it has nevertheless significantly different gas surface density (a factor of 2-4 higher) and electron density in the ionized gas (five times higher) from those in similar nearby galaxies, possibly indicating a higher density interstellar medium for this galaxy. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1306.6282}, -author = {Shirazi, M. and Vegetti, S. and Nesvadba, N. and Allam, S. and Brinchmann, J. and Tucker, D.}, -doi = {10.1093/mnras/stu316}, -eprint = {1306.6282}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: formation,Galaxies: high-redshift,Galaxies: kinematics and dynamics,Gravitational lensing: strong}, -number = {3}, -pages = {2201--2221}, -title = {{The physical nature of the 8 o'clock arc based on near-IR IFU spectroscopy with SINFONI}}, -volume = {440}, -year = {2014} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disk and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al, we assume that galaxies form stars quiescently in a disk until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow disks again. Thus, an individual galaxy may pass through various phases of disk or spheroid dominance during its lifetime. To distinguish between disks and spheroids we add one additional free parameter to the semianalytic model of Cole et al. which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an Ω = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals and the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50{\%} of ellipticals, but only about 15{\%} of spirals, have undergone a major merger during the redshift interval 0.0 ≤ z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long timescale for galaxy mergers compared with the timescale for cluster assembly at high redshift. The assembly of low redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor halos. As a result z = 0 rich clusters become E/S0 dominated and we find a " Butcher-Oemler " effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1 and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between disks and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/9602085v1}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085v1}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {arXiv:astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{DiMauro2014b, -abstract = {Active galactic nuclei (AGNs) with jets seen at small viewing angles are the most luminous and abundant objects in the $\gamma$-ray sky. AGNs with jets misaligned along the line of sight appear fainter in the sky but are more numerous than the brighter blazars. We calculate the diffuse $\gamma$-ray emission due to the population of misaligned AGNs (MAGNs) unresolved by the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (Fermi). A correlation between the $\gamma$-ray luminosity and the radio-core luminosity is established and demonstrated to be physical by statistical tests, as well as compatible with upper limits based on Fermi-LAT data for a large sample of radio-loud MAGNs. We constrain the derived $\gamma$-ray luminosity function by means of the source-count distribution of the radio galaxies detected by the Fermi-LAT. We finally calculate the diffuse $\gamma$-ray flux due to the whole MAGN population. Our results demonstrate that MAGNs can contribute from 10% up to nearly the entire measured isotropic gamma-ray background. We evaluate a theoretical uncertainty on the flux of almost an order of magnitude. {\textcopyright} 2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1304.0908}, -author = {{Di Mauro}, M. and Calore, F. and Donato, F. and Ajello, M. and Latronico, L.}, -doi = {10.1088/0004-637X/780/2/161}, -eprint = {1304.0908}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {diffuse radiation,galaxies: active,galaxies: luminosity function, mass function}, -number = {2}, -pages = {161}, -title = {{Diffuse $\gamma$-ray emission from misaligned active galactic nuclei}}, -url = {http://stacks.iop.org/0004-637X/780/i=2/a=161?key=crossref.bb446baa482971ac7809fdc1d376d88f}, -volume = {780}, -year = {2014} -} -@article{Furlong:2017aa, -author = {Furlong, M and Bower, R.$\sim$G. and Crain, R.$\sim$A. and Schaye, J and Theuns, T and Trayford, J.$\sim$W. and Qu, Y and Schaller, M and Berthet, M and Helly, J.$\sim$C.}, -journal = {\mnras}, -month = {feb}, -pages = {722--738}, -title = {{Size evolution of normal and compact galaxies in the EAGLE simulation}}, -volume = {465}, -year = {2017} -} -@article{Oldham2016, -abstract = {We present a new sample of strong gravitational lens systems where both the foreground lenses and background sources are early-type galaxies. Using imaging from Hubble Space Telescope (HST)/Advanced Camera for Studies (ACS) andKeck/NIRC2, we model the surface brightness distributions and show that the sources form a distinct population ofmassive, compact galaxies at redshifts 0.4 ≲ z ≲ 0.7, lying systematically below the size-mass relation of the global elliptical galaxy population at those redshifts. These may therefore represent relics of highredshift red nuggets or their partly evolved descendants. We exploit the magnifying effect of lensing to investigate the structural properties, stellar masses and stellar populations of these objects with a view to understanding their evolution. We model these objects parametrically and find that they generally require two S{\'{e}}rsic components to properly describe their light profiles, with one more spheroidal component alongside a more envelope-like component, which is slightly more extended though still compact. This is consistent with the hypothesis of the inside-out growth of these objects via minor mergers. We also find that the sources can be characterized by red-to-blue colour gradients as a function of radius which are stronger at low redshift - indicative of ongoing accretion - but that their environments generally appear consistent with that of the general elliptical galaxy population, contrary to recent suggestions that these objects are pre-dominantly associated with clusters.}, -archivePrefix = {arXiv}, -arxivId = {1611.00008}, -author = {Oldham, Lindsay and Auger, Matthew W. and Fassnacht, Christopher D. and Treu, Tommaso and Brewer, Brendon J. and Koopmans, L. V.E. and Lagattuta, David and Marshall, Philip and McKean, John and Vegetti, Simona}, -doi = {10.1093/mnras/stw2832}, -eprint = {1611.00008}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oldham et al. - 2017 - Red nuggets grow inside-out Evidence from gravitational lensing.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong}, -number = {3}, -pages = {3185--3202}, -title = {{Red nuggets grow inside-out: Evidence from gravitational lensing}}, -volume = {465}, -year = {2017} -} -@article{Abazajian2003, -abstract = {The Sloan Digital Sky Survey (SDSS) has validated and made publicly available its First Data Release. This consists of 2099 deg(2) of five-band (u, g, r, i, z) imaging data, 186,240 spectra of galaxies, quasars, stars and calibrating blank sky patches selected over 1360 deg(2) of this area, and tables of measured parameters from these data. The imaging data go to a depth of r approximate to 22.6 and are photometrically and astrometrically calibrated to 2% rms and 100 mas rms per coordinate, respectively. The spectra cover the range 3800-9200 Angstrom, with a resolution of 1800-2100. This paper describes the characteristics of the data with emphasis on improvements since the release of commissioning data (the SDSS Early Data Release) and serves as a pointer to extensive published and on-line documentation of the survey.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0305492}, -author = {Abazajian, Kevork and Adelman-McCarthy, Jennifer K. and Ageros, Marcel A. and Allam, Sahar S. and Anderson, Scott F. and Annis, James and Bahcall, Neta A. and Baldry, Ivan K. and Bastian, Steven and Berlind, Andreas and Bernardi, Mariangela and Blanton, Michael R. and Blythe, Norman and {Bochanski, Jr.}, John J. and Boroski, William N. and Brewington, Howard and Briggs, John W. and Brinkmann, J. and Brunner, Robert J. and Budavri, Tams and Carey, Larry N. and Carr, Michael A. and Castander, Francisco J. and Chiu, Kuenley and Collinge, Matthew J. and Connolly, A. J. and Covey, Kevin R. and Csabai, Istvn and Dalcanton, Julianne J. and Dodelson, Scott and Doi, Mamoru and Dong, Feng and Eisenstein, Daniel J. and Evans, Michael L. and Fan, Xiaohui and Feldman, Paul D. and Finkbeiner, Douglas P. and Friedman, Scott D. and Frieman, Joshua A. and Fukugita, Masataka and Gal, Roy R. and Gillespie, Bruce and Glazebrook, Karl and Gonzalez, Carlos F. and Gray, Jim and Grebel, Eva K. and Grodnicki, Lauren and Gunn, James E. and Gurbani, Vijay K. and Hall, Patrick B. and Hao, Lei and Harbeck, Daniel and Harris, Frederick H. and Harris, Hugh C. and Harvanek, Michael and Hawley, Suzanne L. and Heckman, Timothy M. and Helmboldt, J. F. and Hendry, John S. and Hennessy, Gregory S. and Hindsley, Robert B. and Hogg, David W. and Holmgren, Donald J. and Holtzman, Jon A. and Homer, Lee and Hui, Lam and Ichikawa, Shin-ichi and Ichikawa, Takashi and Inkmann, John P. and eljko Ivezi and Jester, Sebastian and Johnston, David E. and Jordan, Beatrice and Jordan, Wendell P. and Jorgensen, Anders M. and Juri, Mario and Kauffmann, Guinevere and Kent, Stephen M. and Kleinman, S. J. and Knapp, G. R. and Kniazev, Alexei Y. and Kron, Richard G. and Krzesiski, Jurek and Kunszt, Peter Z. and Kuropatkin, Nickolai and Lamb, Donald Q. and Lampeitl, Hubert and Laubscher, Bryan E. and Lee, Brian C. and Leger, R. French and Li, Nolan and Lidz, Adam and Lin, Huan and Loh, Yeong-Shang and Long, Daniel C. and Loveday, Jon and Lupton, Robert H. and Malik, Tanu and Margon, Bruce and McGehee, Peregrine M. and McKay, Timothy A. and Meiksin, Avery and Miknaitis, Gajus A. and Moorthy, Bhasker K. and Munn, Jeffrey A. and Murphy, Tara and Nakajima, Reiko and Narayanan, Vijay K. and Nash, Thomas and {Neilsen, Jr.}, Eric H. and Newberg, Heidi Jo and Newman, Peter R. and Nichol, Robert C. and Nicinski, Tom and Nieto-Santisteban, Maria and Nitta, Atsuko and Odenkirchen, Michael and Okamura, Sadanori and Ostriker, Jeremiah P. and Owen, Russell and Padmanabhan, Nikhil and Peoples, John and Pier, Jeffrey R. and Pindor, Bartosz and Pope, Adrian C. and Quinn, Thomas R. and Rafikov, R. R. and Raymond, Sean N. and Richards, Gordon T. and Richmond, Michael W. and Rix, Hans-Walter and Rockosi, Constance M. and Schaye, Joop and Schlegel, David J. and Schneider, Donald P. and Schroeder, Joshua and Scranton, Ryan and Sekiguchi, Maki and Seljak, Uro and Sergey, Gary and Sesar, Branimir and Sheldon, Erin and Shimasaku, Kazu and Siegmund, Walter A. and Silvestri, Nicole M. and Sinisgalli, Allan J. and Sirko, Edwin and Smith, J. Allyn and Smoli, Vernesa and Snedden, Stephanie A. and Stebbins, Albert and Steinhardt, Charles and Stinson, Gregory and Stoughton, Chris and Strateva, Iskra V. and Strauss, Michael A. and SubbaRao, Mark and Szalay, Alexander S. and Szapudi, Istvn and Szkody, Paula and Tasca, Lidia and Tegmark, Max and Thakar, Aniruddha R. and Tremonti, Christy and Tucker, Douglas L. and Uomoto, Alan and {Vanden Berk}, Daniel E. and Vandenberg, Jan and Vogeley, Michael S. and Voges, Wolfgang and Vogt, Nicole P. and Walkowicz, Lucianne M. and Weinberg, David H. and West, Andrew A. and White, Simon D. M. and Wilhite, Brian C. and Willman, Beth and Xu, Yongzhong and Yanny, Brian and Yarger, Jean and Yasuda, Naoki and Yip, Ching-Wa and Yocum, D. R. and York, Donald G. and Zakamska, Nadia L. and Zehavi, Idit and Zheng, Wei and Zibetti, Stefano and Zucker, Daniel B.}, -doi = {10.1086/378165}, -eprint = {0305492}, -isbn = {1091-6490 (Electronic)\r0027-8424 (Linking)}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {4}, -pages = {2081--2086}, -pmid = {24639494}, -primaryClass = {astro-ph}, -title = {{The First Data Release of the Sloan Digital Sky Survey}}, -url = {http://stacks.iop.org/1538-3881/126/i=4/a=2081}, -volume = {126}, -year = {2003} -} -@article{Lacerna2020, -abstract = {We study the spatially resolved properties of 333 elliptical galaxies with the MaNGA/SDSS-IV survey. The aim is to understand the fundamental processes of formation and quenching of elliptical galaxies. We used the DESI Legacy Imaging Surveys for accurate morphological classification. Based on integrated spectroscopic properties and colors, we classified galaxies into classical "red and dead", recently quenched, and blue star-forming ellipticals (CLEs, RQEs, and BSFs corresponding to 75{\%}, 10{\%}, and 4{\%} of the sample, respectively). We inferred their stellar age and stellar metallicity gradients out to 1.5 effective radius, and reconstructed their global and radial histories of mass growth and star formation. We find the mass- and light-weighted age gradients of CLEs are nearly flat or mildly negative, with small differences between both ages. The respective metallicity gradients are negative, being flatter as less massive are the CLEs. The more massive CLEs assembled earlier and quenched faster than the less massive ones. The CLEs show a weak inside-out growth and a clear inside-out quenching. At masses {\textless} {\$}10{\^{}}{\{}11{\}}{\$} {\$}M{\_}{\{}\backslashbigodot{\}}{\$}, the age and {\$}Z{\$} gradients of the RQEs and BSFs are flatter than those of the CLEs but with larger scatters. They show very weak inside-out growth and quenching, being the quenching slow and even not completed at {\$}z\backslashsim{\$} 0 for the BSFs. Instead, the massive RQEs show an outside-in quenching, and positive gradients in the light-weighted age and stellar metallicities. Our results are consistent with a scenario where the inner parts of CLEs formed by an early and coeval dissipative collapse with a consequent burst of star formation and further quenching, whereas the outer parts continued their assembly likely by dry mergers. We also discuss some evolutionary scenarios for the RQE and BSF galaxies that would agree with their generic results presented here.}, -archivePrefix = {arXiv}, -arxivId = {2001.05506}, -author = {Lacerna, I and Ibarra-Medel, H and Avila-Reese, V and Hern{\'{a}}ndez-Toledo, H M and V{\'{a}}zquez-Mata, J A and S{\'{a}}nchez, S F}, -eprint = {2001.05506}, -keywords = {cd - galaxies,elliptical and lenticular,evolution - galaxies,formation - galaxies,galaxies,star formation,stellar content - galaxies,structure - galaxies}, -title = {{SDSS-IV MaNGA: global and local stellar population properties of elliptical galaxies and their assembly histories}}, -url = {http://arxiv.org/abs/2001.05506}, -year = {2020} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum {\$}j{\_}\backslashstar{\$} and the stellar mass {\$}M{\_}\backslashstar{\$} in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction {\$}f{\_}{\{}\backslashrm inf{\}}{\$} of baryons that infall toward the central regions of galaxies where star formation can occur. We find {\$}f{\_}{\{}\backslashrm inf{\}}\backslashapprox 1{\$} for LTGs and {\$}\backslashapprox 0.4{\$} for ETGs with an uncertainty of about {\$}0.25{\$} dex, consistent with a biased collapse. By comparing with the locally observed {\$}j{\_}\backslashstar{\$} vs. {\$}M{\_}\backslashstar{\$} relations for LTGs and ETGs we estimate the fraction {\$}f{\_}j{\$} of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find {\$}f{\_}j\backslashapprox 1.11{\^{}}{\{}+0.75{\}}{\_}{\{}-0.44{\}}{\$}, in line with the classic disc formation picture; for ETGs we infer {\$}f{\_}j\backslashapprox 0.64{\^{}}{\{}+0.20{\}}{\_}{\{}-0.16{\}}{\$}, that can be traced back to a {\$}z{\textless}1{\$} evolution via dry mergers. We also show that the observed scatter in the {\$}j{\_}{\{}\backslashstar{\}}{\$} vs. {\$}M{\_}{\{}\backslashstar{\}}{\$} relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at {\$}z\backslashsim 2{\$} is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, J and Lapi, A and Mancuso, C and Wang, H and Danese, L}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {2}, -pages = {105}, -title = {{Angular Momentum of Early- and Late-type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -volume = {843}, -year = {2017} -} -@article{Eisenstein2001, -abstract = {We describe the target selection and resulting properties of a spectroscopic sample of luminous, red galaxies (LRG) from the imaging data of the Sloan Digital Sky Survey (SDSS). These galaxies are selected on the basis of color and magnitude to yield a sample of luminous, intrinsically red galaxies that extends fainter and further than the main flux-limited portion of the SDSS galaxy spectroscopic sample. The sample is designed to impose a passively-evolving luminosity and rest-frame color cut to a redshift of 0.38. Additional, yet more luminous, red galaxies are included to a redshift of 0.5. Approximately 12 of these galaxies per square degree are targeted for spectroscopy, so the sample will number over 100,000 with the full survey. SDSS commissioning data indicate that the algorithm efficiently selects luminous (M{\_}g=-21.4), red galaxies, that the spectroscopic success rate is very high, and that the resulting set of galaxies is approximately volume-limited out to z=0.38. When the SDSS is complete, the LRG spectroscopic sample will fill over 1h{\^{}}-3 Gpc{\^{}}3 with an approximately homogeneous population of galaxies and will therefore be well suited to studies of large-scale structure and clusters out to z=0.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108153}, -author = {Eisenstein, Daniel J and Annis, James and Gunn, James E and Szalay, Alexander S and Connolly, Andrew J and Nichol, R C and Bahcall, Neta A and Bernardi, Mariangela and Burles, Scott and Castander, Francisco J and Fukugita, Masataka and Hogg, David W and Ivezi{\'{c}}, {\v{Z}}eljko and Knapp, G R and Lupton, Robert H and Narayanan, Vijay and Postman, Marc and Reichart, Daniel E and Richmond, Michael and Schneider, Donald P and Schlegel, David J and Strauss, Michael A and SubbaRao, Mark and Tucker, Douglas L and {Vanden Berk}, Daniel and Vogeley, Michael S and Weinberg, David H and Yanny, Brian}, -doi = {10.1086/323717}, -eprint = {0108153}, -isbn = {0004-6256}, -issn = {00046256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2267--2280}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample}}, -url = {http://arxiv.org/abs/astro-ph/0108153%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/323717}, -volume = {122}, -year = {2001} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {00160032}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -pages = {1--7}, -title = {{Spatially Resolved Patchy Lyman-{\$}\backslashalpha{\$} Emission Within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8}}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -year = {2017} -} -@article{Ding2016, -abstract = {The empirical correlation between the mass of a supermassive black hole (MBH) and its host galaxy properties is widely considered to be an evidence of their co-evolution. A powerful way to test the co-evolution scenario and learn about the feedback processes linking galaxies and nuclear activity is to measure these correlations as a function of redshift. Unfortunately, currently MBH can only be estimated in active galaxies at cosmological distances. At these distances, bright active galactic nuclei (AGNs) can outshine the host galaxy, making it extremely difficult to measure the host's luminosity. Strongly lensed AGNs provide in principle a great opportunity to improve the sensitivity and accuracy of the host galaxy luminosity measurements as the host galaxy is magnified and more easily separated from the point source, provided the lens model is sufficiently accurate. In order to measure the MBH-L correlation with strong lensing, it is necessary to ensure that the lens modelling is accurate, and that the host galaxy luminosity can be recovered to at least a precision and accuracy better than that of the typical MBH measurement. We carry out extensive and realistic simulations of deep Hubble Space Telescope observations of lensed AGNs obtained by our collaboration. We show that the host galaxy luminosity can be recovered with better accuracy and precision than the typical uncertainty in MBH({\$\sim${}}0.5 dex) for hosts as faint as 2-4 mag dimmer than the AGN itself. Our simulations will be used to estimate bias and uncertainties in the actual measurements to be presented in a future paper.}, -archivePrefix = {arXiv}, -arxivId = {1610.08504}, -author = {Ding, Xuheng and Liao, Kai and Treu, Tommaso and Suyu, Sherry H and Chen, Geoff C F and Auger, Matthew W and Marshall, Philip J and Agnello, Adriano and Courbin, Frederic and Nierenberg, Anna M and Rusu, Cristian E and Sluse, Dominique and Sonnenfeld, Alessandro and Wong, Kenneth C}, -doi = {10.1093/mnras/stw3078}, -eprint = {1610.08504}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: evolution}, -number = {4}, -pages = {4634--4649}, -title = {{H0LiCOW. VI. Testing the fidelity of lensed quasar host galaxy reconstruction}}, -url = {http://arxiv.org/abs/1610.08504}, -volume = {465}, -year = {2017} -} -@article{Pandya2017, -abstract = {We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M{\_}*/M{\_}sun) {\textgreater} 11.5 (M{\_}K {\textless} -25.3 mag) and distance D {\textless} 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38$\backslash$pm6{\%} down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80$\backslash$pm10{\%} and 28$\backslash$pm6{\%}, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R{\_}e), and the gas morphologies are diverse, with 17/28 = 61$\backslash$pm9{\%} being centrally concentrated, 8/28 = 29$\backslash$pm9{\%} exhibiting clear rotation out to several kpc, and 3/28 = 11$\backslash$pm6{\%} being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly {\$\sim${}}10{\^{}}5M{\_}sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers.}, -archivePrefix = {arXiv}, -arxivId = {1701.08772}, -author = {Pandya, Viraj and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Ene, Irina and Davis, Timothy A and Blakeslee, John P and Goulding, Andy D and McConnell, Nicholas J and Nyland, Kristina and Thomas, Jens}, -doi = {10.3847/1538-4357/aa5ebc}, -eprint = {1701.08772}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {ISM: kinematics and dynamics,ISM: lines and bands,cD,cd,dynamics,elliptical and lenticular,evolution,fi gure set,galaxies,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,ism,kinematics and,kinematics and dynamics,lines and bands,machine-readable table,supporting material}, -number = {1}, -pages = {40}, -title = {{The MASSIVE Survey. VI. The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies}}, -url = {http://stacks.iop.org/0004-637X/837/i=1/a=40?key=crossref.978f7a67a8a7e453f73aaa6941fcf7be}, -volume = {837}, -year = {2017} -} -@article{Despali2024, -abstract = {Strong gravitational lensing can detect the presence of low-mass haloes and subhaloes through their effect on the surface brightness of lensed arcs. We carry out an extended analysis of the density profiles and mass distributions of two detected subhaloes, intending to determine if their properties are consistent with the predictions of the cold dark matter (CDM) model. We analyse two gravitational lensing systems in which the presence of two low-mass subhaloes has been previously reported: SDSSJ0946+1006 and JVASB1938+66. We model these detections assuming four different models for their density profiles and compare our results with predictions from the IllustrisTNG50-1 simulation. We find that the detected subhaloes are well-modelled by steep inner density slopes, close to or steeper than isothermal. The NFW profile thus needs extremely high concentrations to reproduce the observed properties, which are outliers of the CDM predictions. We also find a characteristic radius within which the best-fitting density profiles predict the same enclosed mass. We conclude that the lens modelling can constrain this quantity more robustly than the inner slope. We find that the diversity of subhalo profiles in TNG50, consistent with tidally stripping and baryonic effects, is able to match the observed steep inner slopes, somewhat alleviating the tension reported by previous works even if the detections are not well fit by the typical subhalo. However, while we find simulated analogues of the detection in B1938+666, the stellar content required by simulations to explain the central density of the detection in J0946+1006 is in tension with the upper limit in luminosity estimated from the observations. New detections will increase our statistical sample and help us reveal more about the density profiles of these objects and the dark matter content of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {2407.12910}, -author = {Despali, Giulia and Heinze, Felix M. and Fassnacht, Christopher D. and Vegetti, Simona and Spingola, Cristiana and Klessen, Ralf}, -eprint = {2407.12910}, -file = {:C\:/Users/Jammy/Documents/Papers/Substructure/Despali2024SensitivityII.pdf:pdf}, -keywords = {dark matter,galaxies,gravitational lensing,simulations}, -number = {2016}, -title = {{Detecting low-mass haloes with strong gravitational lensing II: constraints on the density profiles of two detected subhaloes}}, -year = {2024} -} -@article{Laporte:2013aa, -author = {Laporte, C.$\sim$F.$\sim$P. and White, S.$\sim$D.$\sim$M. and Naab, T and Gao, L}, -journal = {\mnras}, -month = {oct}, -pages = {901--909}, -title = {{The growth in size and mass of cluster galaxies since z = 2}}, -volume = {435}, -year = {2013} -} -@article{Hopkins2011b, -abstract = {Feedback from massive stars is believed to play a critical role in shaping the galaxy mass function, the structure of the interstellar medium (ISM) and the low efficiency of star formation, but the exact form of the feedback is uncertain. In this paper, the first in a series, we present and test a novel numerical implementation of stellar feedback resulting from momentum imparted to the ISM by radiation, supernovae and stellar winds. We employ a realistic cooling function, and find that a large fraction of the gas cools to ≲100K, so that the ISM becomes highly inhomogeneous. Despite this, our simulated galaxies reach an approximate steady state, in which gas gravitationally collapses to form giant 'molecular' clouds (GMCs), dense clumps and stars; subsequently, stellar feedback disperses the GMCs, repopulating the diffuse ISM. This collapse and dispersal cycle is seen in models of Small Magellanic Cloud (SMC)-like dwarfs, the Milky Way and z$\sim$ 2 clumpy disc analogues. The simulated global star formation efficiencies are consistent with the observed Kennicutt-Schmidt relation. Moreover, the star formation rates are nearly independent of the numerically imposed high-density star formation efficiency, density threshold and density scaling. This is a consequence of the fact that, in our simulations, star formation is regulated by stellar feedback limiting the amount of very dense gas available for forming stars. In contrast, in simulations without stellar feedback, i.e. under the action of only gravity and gravitationally induced turbulence, the ISM experiences runaway collapse to very high densities. In these simulations without feedback, the global star formation rates exceed observed galactic star formation rates by 1-2 orders of magnitude, demonstrating that stellar feedback is crucial to the regulation of star formation in galaxies. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1101.4940}, -author = {Hopkins, Philip F. and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2011.19306.x}, -eprint = {1101.4940}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins, Quataert, Murray - 2011 - Self-regulated star formation in galaxies via momentum input from massive stars.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation}, -number = {2}, -pages = {950--973}, -title = {{Self-regulated star formation in galaxies via momentum input from massive stars}}, -volume = {417}, -year = {2011} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter (CDM) galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes possess a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a $\Lambda$CDM universe. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R. and Eke, Vincent R. and Frenk, Carlos S. and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lovell et al. - 2011 - The link between galactic satellite orbits and subhalo accretion(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{Khochfar2011a, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* > 1010.5M⊙ contributing $\sim$20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between $\sim$50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z > 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) > 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z < 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive (>1010M⊙) fast rotators being more than one order of magnitude more frequent at z$\sim$ 2. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R. and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M. and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Khochfar et al. - 2011 - The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies.pdf:pdf}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Galaxies: structure}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio M/L and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R,z) and characterized by the classic anisotropy parameter beta{\_}z=1-sigma{\_}z{\^{}}2/sigma{\_}R{\^{}}2. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters (beta{\_}z and the inclination) the models generally provide remarkably good descriptions of the shape of the first (V) and second (V{\_}rms=sqrt{\{}V{\^{}}2+sigma{\^{}}2{\}}) velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the simple dynamical structure of these objects. With the observationally-motivated assumption that beta{\_}z{\textgreater}0, the method is able to recover the inclination. The technique can be used to determine the dynamical mass-to-light ratios and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modeling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy, and multiple kinematic components.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Feroz2009, -abstract = {We present further development and the first public release of our multimodal nested sampling algorithm, called MultiNest. This Bayesian inference tool calculates the evidence, with an associated error estimate, and produces posterior samples from distributions that may contain multiple modes and pronounced (curving) degeneracies in high dimensions. The developments presented here lead to further substantial improvements in sampling efficiency and robustness, as compared to the original algorithm presented in Feroz and Hobson, which itself significantly outperformed existing Markov chain Monte Carlo techniques in a wide range of astrophysical inference problems. The accuracy and economy of the MultiNest algorithm are demonstrated by application to two toy problems and to a cosmological inference problem focusing on the extension of the vanilla $\Lambda$ cold dark matter model to include spatial curvature and a varying equation of state for dark energy. The MultiNest software, which is fully parallelized using MPI and includes an interface to CosmoMC, is available at http://www.mrao.cam.ac.uk/software/multinest/. It will also be released as part of the SuperBayeS package, for the analysis of supersymmetric theories of particle physics, at http://www.superbayes.org. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0809.3437}, -author = {Feroz, F. and Hobson, M. P. and Bridges, M.}, -doi = {10.1111/j.1365-2966.2009.14548.x}, -eprint = {0809.3437}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Methods: Data analysis,Methods: Statistical}, -number = {4}, -pages = {1601--1614}, -pmid = {29176}, -title = {{MultiNest: An efficient and robust Bayesian inference tool for cosmology and particle physics}}, -volume = {398}, -year = {2009} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 {\textless} z {\textless} 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J{\textless}inf{\textgreater}125{\textless}/inf{\textgreater}, i{\textless}inf{\textgreater}814{\textless}/inf{\textgreater}, v{\textless}inf{\textgreater}606{\textless}/inf{\textgreater} HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.1736}, -volume = {444}, -year = {2014} -} -@article{Alexander2019, -abstract = {Dark matter substructure has the potential to discriminate between broad classes of dark matter models. With this in mind, we construct novel solutions to the equations of motion governing condensate dark matter candidates, namely axion Bose-Einstein condensates and superfluids. These solutions are highly compressed along one axis and thus have a disk-like geometry. We discuss linear stability of these solutions, consider the astrophysical implications as a large-scale dark disk or as small scale substructure, and find a characteristic signal in strong gravitational lensing. This adds to the growing body of work that indicates that the morphology of dark matter substructure is a powerful probe of the nature of dark matter.}, -archivePrefix = {arXiv}, -arxivId = {1901.03694}, -author = {Alexander, Stephon and Bramburger, Jason J and McDonough, Evan}, -doi = {10.1016/j.physletb.2019.134871}, -eprint = {1901.03694}, -issn = {03702693}, -journal = {Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics}, -pages = {1--7}, -title = {{Dark disk substructure and superfluid dark matter}}, -url = {http://arxiv.org/abs/1901.03694}, -volume = {797}, -year = {2019} -} -@article{Herbert-Fort2007, -abstract = {We measure the distribution of velocities for prograde and retrograde satellite galaxies using a combination of published data and new observations for 78 satellites of 63 extremely isolated disc galaxies (169 satellites total). We find that the velocity distribution is non-Gaussian ({\textgreater}99.9 per cent confidence), but that it can be described as the sum of two Gaussians, one of which is broad ($\sigma$ = 176 ± 15 km s-1), has a mean prograde velocity of 86 ± 30 km s-1, and contains ∼55 per cent of the satellites, while the other is slightly retrograde with a mean velocity of -21 ± 22 km s-1 and $\sigma$ = 74 ± 18 km s-1 and contains ∼45 per cent of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy, and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Sales2012, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Gomer2018, -abstract = {The positions of multiple images in galaxy lenses are related to the galaxy mass distribution. Smooth elliptical mass profiles were previously shown to be inadequate in reproducing the quad population. In this paper, we explore the deviations from such smooth elliptical mass distributions. Unlike most other work, we use a model-free approach based on the relative polar image angles of quads, and their position in 3D space with respect to the fundamental surface of quads (FSQ). The FSQ is defined by quads produced by elliptical lenses. We have generated thousands of quads from synthetic populations of lenses with substructure consistent with Lambda cold dark matter ($\Lambda$CDM) simulations, and found that such perturbations are not sufficient to match the observed distribution of quads relative to the FSQ. The result is unchanged even when subhalo masses are increased by a factor of 10, and the most optimistic lensing selection bias is applied. We then produce quads from galaxies created using two components, representing baryons and dark matter. The transition from the mass being dominated by baryons in inner radii to being dominated by dark matter in outer radii can carry with it asymmetries, which would affect relative image angles. We run preliminary experiments using lenses with two elliptical mass components with non-identical axial ratios and position angles, perturbations from ellipticity in the form of non-zero Fourier coefficients a4 and a6, and artificially offset ellipse centres as a proxy for asymmetry at image radii. We show that combination of these effects is a promising way of accounting for quad population properties. We conclude that the quad population provides a unique and sensitive tool for constraining detailed mass distribution in the centres of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1712.07665}, -author = {Gomer, Matthew R and Williams, Liliya L R}, -doi = {10.1093/mnras/stx3294}, -eprint = {1712.07665}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {2}, -pages = {1987--2002}, -title = {{The impact of $\Lambda$CDM substructure and baryon-dark matter transition on the image positions of quad galaxy lenses}}, -volume = {475}, -year = {2018} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1 < z < 3. Our analysis is based on a bulge-disc decomposition of 396 galaxies with M* > 1011M⊙ uncovered from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/IR imaging within the Cosmological Evolution Survey (COSMOS) and UKIRT Infrared Deep Sky Survey (UKIDSS) UDS survey fields. We find that, by modelling the H160 image of each galaxy with a combination of a de Vaucouleurs bulge (S{\'{e}}rsic index n = 4) and an exponential disc (n = 1), we can then lock all derived morphological parameters for the bulge and disc components, and successfully reproduce the shorter-wavelength J125, i814, v606 HST images simply by floating the magnitudes of the two components. This then yields sub-divided four-band HST photometry for the bulge and disc components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information, we are able to properly determine themasses and star formation rates for the bulge and disc components, and find that: (i) from z = 3 to 1 the galaxies move from disc dominated to increasingly bulge dominated, but very few galaxies are pure bulges/ellipticals by z = 1; (ii) while most passive galaxies are bulge dominated, and most star-forming galaxies disc dominated, 18 ± 5 per cent of passive galaxies are disc dominated, and 11 ± 3 per cent of star-forming galaxies are bulge dominated, a result which needs to be explained by any model purporting to connect star formation quenching with morphological transformations; (iii) there exists a small but significant population of pure passive discs, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a ≃ 0.7); (iv) flatter/larger discs re-emerge at the highest star formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface density for star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V. A. and Dunlop, J. S. and McLure, R. J. and Cirasuolo, M. and Buitrago, F. and Bowler, R. A.A. and Targett, T. A. and Bell, E. F. and McIntosh, D. H. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Hartley, W. and Kocevski, D. D. and Koekemoer, A. M. and Koo, D. C. and McGrath, E. J.}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular, cD,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 < z < 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{Messias2019, -abstract = {Follow-up observations of (sub-)mm-selected gravitationally lensed systems have allowed a more detailed study of the dust-enshrouded phase of star formation up to very early cosmic times. Here, the case of the gravitationally lensed merger in HATLAS J142935.3-002836 (also known as H1429-0028; zlens = 0.218, zbkg = 1.027) is revisited following recent developments in the literature and new Atacama Pathfinder EXperiment (APEX) observations targeting two carbon monoxide (CO) rotational transitions Jup = 3 and 6. We show that the line profiles comprise three distinct velocity components, where the fainter high velocity one is less magnified and more compact. The modelling of the observed spectral line energy distribution of CO Jup = 2-6 and [C I] 3P1-3P0 assumes a large velocity gradient scenario, where the analysis is based on four statistical approaches. Since the detected gas and dust emission comes exclusively from only one of the two merging components (the one oriented north-south, NS), we are only able to determine upper limits for the companion. The molecular gas in the NS component in H1429-0028 is found to have a temperature of ∼70 K, a volume density of log (n[cm-3]) ∼ 3.7, to be expanding at ∼10 km s-1 pc-1, and amounts to MH2 = 4+3 -2 × 109M$\theta$. The CO to H2 conversion factor is estimated to be $\alpha$CO = 0.4+0.3 -0.2 M$\theta$/(K km s-1 pc2). The NS galaxy is expected to have a factor of ≳10× more gas than its companion (MH2 ≲ 3 × 108 M$\theta$). Nevertheless, the total amount of molecular gas in the system comprises only up to 15 per cent (1$\sigma$ upper limit) of the total (dynamical) mass.}, -archivePrefix = {arXiv}, -arxivId = {1904.00307}, -author = {Messias, Hugo and Nagar, Neil and Zhang, Zhi Yu and Oteo, Iv{\'{a}}n and Dye, Simon and Ibar, Eduardo and Timmons, Nicholas and {Van Der Werf}, Paul and Riechers, Dominik and Eales, Stephen and Ivison, Rob and Maresca, Jacob and Micha{\l}owski, Micha{\l}J. and Yang, Chentao}, -doi = {10.1093/mnras/stz945}, -eprint = {1904.00307}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {ISM: abundances,galaxies: interactions,gravitational lensing: strong,submillimetre: ISM.,submillimetre: galaxies}, -number = {2}, -pages = {2366--2378}, -title = {{The molecular gas properties in the gravitationally lensed merger HATLAS J142935.3-002836}}, -url = {http://arxiv.org/abs/1904.00307%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stz945}, -volume = {486}, -year = {2019} -} -@article{Governato2015, -abstract = {We use high-resolution Hydro+N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass $\sim$106-7 M⊙, total mass 1010 M⊙) in $\Lambda$-dominated cold dark matter (CDM) and 2 keV warm dark matter (WDM) cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the dark matter (DM) model, but proportionally to the SF efficiency, gas outflows lower the central mass density through 'dynamical heating', such that all realizations have circular velocities < 20 km s-1 at 500 pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial colour- magnitude diagrams and star formation histories (SFHs) in order to directly compare to available observations. The simulated galaxies formed most of their stars in many $\sim$10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including 'baryon physics' in simulations when (1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and (2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F. and Weisz, D. and Pontzen, A. and Loebman, S. and Reed, D. and Brooks, A. M. and Behroozi, P. and Christensen, C. and Madau, P. and Mayer, L. and Shen, S. and Walker, M. and Quinn, T. and Keller, B. W. and Wadsley, J.}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Governato et al. - 2015 - Faint dwarfs as a test of DM models WDM versus CDM.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Weinberg2007, -abstract = {A galaxy remains near equilibrium for most of its history. Only through resonances can non-axisymmetric features, such as spiral arms and bars, exert torques over large scales and change the overall structure of the galaxy. In this paper, we describe the resonant interaction mechanism in detail, derive explicit criteria for the particle number required to simulate these dynamical processes accurately using N-body simulations, and illustrate them with numerical experiments. To do this, we perform a direct numerical solution of perturbation theory, in short, by solving for each orbit in an ensemble and make detailed comparisons with N-body simulations. The criteria include: sufficient particle coverage in phase space near the resonance and enough particles to minimize gravitational potential fluctuations that will change the dynamics of the resonant encounter. These criteria are general in concept and can be applied to any dynamical interaction. We use the bar-halo interaction as our primary example owing to its technical simplicity and astronomical ubiquity. Some of our more surprising findings are as follows. First, the inner Lindblad like resonance, responsible for coupling the bar to the central halo cusp, requires more than script O sign (108) equal-mass particles within the virial radius or O(107) inside the bar radius for a Milky Way like bar in a Navarro, Frenk & White profile. Secondly, orbits that linger near the resonance receive more angular momentum than orbits that move through the resonance quickly. Small-scale fluctuations present in state-of-the-art particle-particle simulations can knock orbits out of resonance, preventing them from lingering and, thereby, decrease the torque per orbit. This can be offset by the larger number of orbits affected by the resonance due to the diffusion. However, noise from orbiting substructure remains at least an order of magnitude too small to be of consequence. Applied to N-body simulations, the required particle numbers are sufficiently high for scenarios of interest that apparent convergence in particle number is misleading: the convergence with N may still be in the noise-dominated regime. State-of-the-art simulations are not adequate to follow all aspects of secular evolution driven by the bar-halo interaction. It is not possible to derive particle number requirements that apply to all situations, for example, more subtle interactions may be even more difficult to simulate. Therefore, we present a procedure to test the requirements for individual N-body codes to the actual problem of interest. {\textcopyright} 2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508166}, -author = {Weinberg, Martin D. and Katz, Neal}, -doi = {10.1111/j.1365-2966.2006.11306.x}, -eprint = {0508166}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxy: structure,Stellar dynamics}, -month = {feb}, -number = {2}, -pages = {425--459}, -primaryClass = {astro-ph}, -title = {{The bar-halo interaction - I. From fundamental dynamics to revised N-body requirements}}, -volume = {375}, -year = {2007} -} -@article{Oh2017, -abstract = {We investigate two-dimensional image decomposition of nearby, morphologically selected early-type galaxies (ETGs). We are motivated by recent observational evidence of significant size growth of quiescent galaxies and theoretical development advocating a two-phase formation scenario for ETGs. We find that a significant fraction of nearby ETGs show changes in isophotal shape that require multi-component models. The characteristic sizes of the inner and outer component are $\sim 3$ and $\sim 15$ kpc. The inner component lies on the mass-size relation of ETGs at $z \sim 0.25-0.75$, while the outer component tends to be more elliptical and hints at a stochastic buildup process. We find real physical differences between the single- and double-component ETGs, with the double-component galaxies being younger and more metal-rich. The fraction of double component ETGs increases with increasing $\sigma$ and decreases in denser environments. We hypothesize that double-component systems were able to accrete gas and small galaxies until later times, boosting their central densities, building up their outer parts, and lowering their typical central ages. In contrast, the oldest galaxies, perhaps due to residing in richer environments, have no remaining hints of their last accretion episode.}, -archivePrefix = {arXiv}, -arxivId = {1612.06495}, -author = {Oh, Semyeong and Greene, Jenny E. and Lackner, Claire N.}, -doi = {10.3847/1538-4357/836/1/115}, -eprint = {1612.06495}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Oh, Greene, Lackner - 2017 - Testing the Presence of Multiple Photometric Components in Nearby Early-type Galaxies Using SDSS(4).pdf:pdf}, -issn = {1538-4357}, -journal = {ApJ}, -number = {1}, -pages = {115}, -title = {{Testing the Presence of Multiple Photometric Components in Nearby Early-type Galaxies Using SDSS}}, -url = {http://arxiv.org/abs/1612.06495%0Ahttp://dx.doi.org/10.3847/1538-4357/836/1/115}, -volume = {836}, -year = {2017} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Metcalf2018, -abstract = {Large-scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images, and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects, reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100 000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. Having multi-band, ground based data is found to be better for this purpose than single-band space based data with lower noise and higher resolution, suggesting that multi-colour data is crucial. Multi-band space based data will be superior to ground based data. The most difficult challenge for a lens finder is differentiating between rare, irregular and ring-like face-on galaxies and true gravitational lenses. The degree to which the efficiency and biases of lens finders can be quantified largely depends on the realism of the simulated data on which the finders are trained.}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R. B. and Meneghetti, M. and Avestruz, C. and Bellagamba, F. and Bom, C. R. and Bertin, E. and Cabanac, R. and Courbin, F. and Davies, A. and Decenci{\`{e}}re, E. and Flamary, R. and Gavazzi, R. and Geiger, M. and Hartley, P. and Huertas-Company, M. and Jackson, N. and Jacobs, C. and Jullo, E. and Kneib, J. P. and Koopmans, L. V.E. and Lanusse, F. and Li, C. L. and Ma, Q. and Makler, M. and Li, N. and Lightman, M. and Petrillo, C. E. and Serjeant, S. and Sch{\"{a}}fer, C. and Sonnenfeld, A. and Tagore, A. and Tortora, C. and Tuccillo, D. and Valent{\'{i}}n, M. B. and Velasco-Forero, S. and {Verdoes Kleijn}, G. A. and Vernardos, G.}, -doi = {10.1051/0004-6361/201832797}, -eprint = {1802.03609}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Metcalf et al. - 2019 - The strong gravitational lens finding challenge(2).pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Gravitational lensing: strong - methods: data anal}, -title = {{The strong gravitational lens finding challenge}}, -url = {http://arxiv.org/abs/1802.03609%0Ahttp://dx.doi.org/10.1051/0004-6361/201832797}, -volume = {625}, -year = {2019} -} -@article{Cohen2018, -abstract = {We present HST/ACS imaging of twenty-three very low surface brightness ($\mu_{e,V}$=25-27.5) galaxies detected in the fields of four nearby galaxy groups. These objects were selected from deep optical imaging obtained with the Dragonfly Telephoto Array. Seven are new discoveries, while most of the others had been identified previously in visual surveys of deep photographic plates and more recent surveys. Few have previously been studied in detail. From the ACS images, we measure distances to the galaxies using both the tip of the red giant branch method and the surface brightness fluctuations method. We demonstrate that the two methods are consistent with each other in the regime where both can be applied. The distances to 15 out of 20 galaxies with stable measurements are consistent with that of the targeted group within errors. This suggests that assuming group membership based solely on projected proximity is $\sim$75% successful in this regime. The galaxies are nearly round, with a median axis ratio of 0.85, and visually resemble dwarf spheroidal galaxies. The objects have a range of sizes, from $R_e$=0.4 kpc to $R_e$=1.8 kpc, with a median of 1.0 kpc. They range in luminosity from $M_V$=-11.4 to $M_V$=-15.6, with a median of -12.4. Galaxies with $R_e$$\sim$1 kpc and $M_V$$\sim$-12 are fairly rare in the Local Group but we find many of them in this relatively small sample. Four of the objects fall in the class of ultra diffuse galaxies (UDGs), with $R_e$>1.5 kpc and $\mu_{0,V}$>24 mag/arcsec^2, including the recently identified dark matter deficient galaxy NGC1052-DF2.}, -archivePrefix = {arXiv}, -arxivId = {1807.06016}, -author = {Cohen, Yotam and van Dokkum, Pieter and Danieli, Shany and Romanowsky, Aaron J. and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Mowla, Lamiya and Kruijssen, J. M. Diederik and Conroy, Charlie and Wasserman, Asher}, -doi = {10.3847/1538-4357/aae7c8}, -eprint = {1807.06016}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cohen et al. - 2018 - The Dragonfly Nearby Galaxies Survey. V. HST ACS Observations of 23 Low Surface Brightness Objects in the Field(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {Astrophysics,Astrophysics of Galaxies}, -number = {2}, -pages = {96}, -title = {{ The Dragonfly Nearby Galaxies Survey. V. HST /ACS Observations of 23 Low Surface Brightness Objects in the Fields of NGC 1052, NGC 1084, M96, and NGC 4258 }}, -url = {http://arxiv.org/abs/1807.06016%0Ahttp://dx.doi.org/10.3847/1538-4357/aae7c8}, -volume = {868}, -year = {2018} -} -@article{Wood2014, -abstract = {The goals of future space missions such as Euclid require unprecedented positional accuracy from the responsible detector. Charge coupled devices (CCDs) can be manufactured with exceptional charge transfer properties; however the harsh radiation environment of space leads to damage within the silicon lattice, predominantly through proton collisions. The resulting lattice defects can trap charge, degrading the positional accuracy and reducing the useful operating time of a detector. Mitigation of such effects requires precise knowledge of defects and their effects on charge transfer within a CCD. We have used the technique of single-trap "pumping" to study two such charge trapping defects; the silicon divacancy and the carbon interstitial, in a p-channel CCD. We show this technique can be used to give accurate information about trap parameters required for radiation damage models and correction algorithms. We also discuss some unexpected results from studying defects in this way.}, -author = {Wood, D. and Hall, D. J. and Murray, N. J. and Gow, J. P.D. and Holland, A. and Turner, P. and Burt, D.}, -doi = {10.1088/1748-0221/9/12/C12028}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wood et al. - 2014 - Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap pumping techn(2).pdf:pdf}, -issn = {17480221}, -journal = {Journal of Instrumentation}, -keywords = {Interaction of radiation with matter,Photon detectors for uv, visible and ir photons (s}, -number = {12}, -pages = {C12028--C12028}, -title = {{Studying charge-trapping defects within the silicon lattice of a p-channel CCD using a single-trap "pumping" technique}}, -url = {http://iopscience.iop.org/article/10.1088/1748-0221/9/12/C12028}, -volume = {9}, -year = {2014} -} -@article{Newton2011, -abstract = {We exploit the strong lensing effect to explore the properties of intrinsically faint and compact galaxies at intermediate redshift (z s ≃ 0.4-0.8) at the highest possible resolution at optical wavelengths. Our sample consists of 46 strongly lensed emission line galaxies (ELGs) discovered by the Sloan Lens ACS Survey (SLACS). The galaxies have been imaged at high resolution with the Hubble Space Telescope (HST) in three bands (VHST , I 814, and H 160), allowing us to infer their size, luminosity, and stellar mass using stellar population synthesis models. Lens modeling is performed using a new fast and robust code, KLENS, which we test extensively on real and synthetic non-lensed galaxies, and also on simulated galaxies multiply imaged by SLACS-like galaxy-scale lenses. Our tests show that our measurements of galaxy size, flux, and S{\'{e}}rsic index are robust and accurate, even for objects intrinsically smaller than the HST point-spread function. The median magnification is 8.8, with a long tail that extends to magnifications above 40. Modeling the SLACS sources reveals a population of galaxies with colors and S{\'{e}}rsic indices (median n ∼ 1) consistent with the galaxies detected with HST in the Galaxy Evolution from Morphology and SEDs (GEMS) and Hubble Ultra Deep Field (HUDF) surveys, but that are (typically) ∼2 mag fainter and ∼5 times smaller in apparent size than GEMS and ∼4 mag brighter than but similar in size to HUDF. The size-stellar-mass and size-luminosity relations for the SLACS sources are offset to smaller sizes with respect to both comparison samples. The closest analog are ultracompact ELGs identified by HST grism surveys. The lowest mass galaxies in our sample are comparable to the brightest Milky Way satellites in stellar mass (107 M⊙) and have well-determined half-light radii of 005 (0.3kpc). {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1104.2608}, -author = {Newton, Elisabeth R. and Marshall, Philip J. and Treu, Tommaso and Auger, Matthew W. and Gavazzi, Raph{\"{a}}el and Bolton, Adam S. and Koopmans, L{\'{e}}on V.E. and Moustakas, Leonidas A.}, -doi = {10.1088/0004-637X/734/2/104}, -eprint = {1104.2608}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: fundamental parameters,gravitational lensing: strong}, -month = {jun}, -number = {2}, -pages = {104}, -title = {{The sloan lens ACS Survey. XI. beyond hubble resolution: Size, luminosity, and stellar mass of compact lensed galaxies at intermediate redshift}}, -url = {http://arxiv.org/abs/1104.2608%0Ahttp://dx.doi.org/10.1088/0004-637X/734/2/104}, -volume = {734}, -year = {2011} -} -@article{Li2017, -abstract = {We perform Jeans anisotropic modeling (JAM) on elliptical and spiral galaxies from the MaNGA DR13 sample. By comparing the stellar mass-to-light ratios estimated from stellar population synthesis (SPS) and from JAM, we find a similar systematic variation of the initial mass function (IMF) as in the earlier $\rm ATLAS^{3D}$ results. Early type galaxies (elliptical and lenticular) with lower velocity dispersions within one effective radius are consistent with a Chabrier-like IMF while galaxies with higher velocity dispersions are consistent with a more bottom heavy IMF such as the Salpeter IMF. Spiral galaxies have similar systematic IMF variations, but with slightly different slopes and larger scatters, due to the uncertainties caused by higher gas fractions and extinctions for these galaxies. Furthermore, we examine the effects of stellar mass-to-light ratio gradients on our JAM modeling, and find that the trends from our results becomes stronger after considering the gradients.}, -archivePrefix = {arXiv}, -arxivId = {1703.04894}, -author = {Li, Hongyu and Ge, Junqiang and Mao, Shude and Cappellari, Michele and Long, R. J. and Li, Ran and Emsellem, Eric and Dutton, Aaron A. and Li, Cheng and Bundy, Kevin and Thomas, Daniel and Drory, Niv and Lopes, Alexandre Roman}, -doi = {10.3847/1538-4357/aa662a}, -eprint = {1703.04894}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Li et al. - 2017 - SDSS-IV MaNGA Variation of the Stellar Initial Mass Function in Spiral and Early-type Galaxies.pdf:pdf}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {77}, -title = {{SDSS-IV MaNGA: Variation of the Stellar Initial Mass Function in Spiral and Early-type Galaxies}}, -url = {http://arxiv.org/abs/1703.04894%0Ahttp://dx.doi.org/10.3847/1538-4357/aa662a}, -volume = {838}, -year = {2017} -} -@article{Liao2016, -abstract = {The standard galaxy formation theory assumes that baryons and dark matter are initially well mixed before becoming segregated due to radiative cooling. We use non-radiative hydrodynamical simulations to explicitly examine this assumption and find that baryons and dark matter can also be segregated due to different characteristics of gas and dark matter during the buildup of the halo. As a result, baryons in many haloes do not originate from the same Lagrangian region as the dark matter. When using the fraction of corresponding dark matter and gas particles in the initial conditions (the 'paired fraction') as a proxy of the dark matter and gas segregation strength of a halo, on average about 25 per cent of the baryonic and dark matter of the final halo are segregated in the initial conditions. This is at odds with the assumption of the standard galaxy formation model. A consequence of this effect is that the baryons and dark matter of the same halo initially experience different tidal torques and thus their angular momentum vectors are often misaligned. The degree of the misalignment is largely preserved during later halo assembly and can be understood with the tidal torque theory. The result challenges the precision of some semi-analytical approaches that utilize dark matter halo merger trees to infer properties of gas associated with dark matter haloes.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.07592}, -author = {Liao, Shihong and Gao, Liang and Frenk, Carlos S and Guo, Qi and Wang, Jie}, -doi = {10.1093/mnras/stx1391}, -eprint = {1610.07592}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {2}, -pages = {2262--2269}, -title = {{The segregation of baryons and dark matter during halo assembly}}, -url = {http://arxiv.org/abs/1610.07592}, -volume = {470}, -year = {2017} -} -@article{Oser:2010aa, -author = {Oser, L and Ostriker, J.$\sim$P. and Naab, T and Johansson, P.$\sim$H. and Burkert, A}, -journal = {\apj}, -month = {dec}, -pages = {2312--2323}, -title = {{The Two Phases of Galaxy Formation}}, -volume = {725}, -year = {2010} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo {\textgreater}1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from ˜30° to 10° for M ˜ 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by a global driving force and a local positive feedback mechanism, which creates regular geometric and/or temporal patterns, and decreases the entropy locally, in contrast to random processes. Here we investigate for the first time a comprehensive number of (17) self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous “order out of randomness”, during the evolution from an initially disordered system to an ordered quasi-stationary system, mostly by quasi-periodic limit-cycle dynamics, but also by harmonic (mechanical or gyromagnetic) resonances. The global driving force can be due to gravity, electromagnetic forces, mechanical forces (e.g., rotation or differential rotation), thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational (Balbus-Hawley) instability, the convective (Rayleigh-B{\'{e}}nard) instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or a loss-cone instability. Physical models of astrophysical self-organization processes require hydrodynamic, magneto-hydrodynamic (MHD), plasma, or N-body simulations. Analytical formulations of self-organizing systems generally involve coupled differential equations with limit-cycle solutions of the Lotka-Volterra or Hopf-bifurcation type.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C M and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G and Scargle, Jeffrey D and Melatos, Andrew and Wagoner, Robert V and Trimble, Virginia and Green, William H}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Hopkins2011b, -abstract = {Feedback from massive stars is believed to play a critical role in shaping the galaxy mass function, the structure of the interstellar medium (ISM) and the low efficiency of star formation, but the exact form of the feedback is uncertain. In this paper, the first in a series, we present and test a novel numerical implementation of stellar feedback resulting from momentum imparted to the ISM by radiation, supernovae and stellar winds. We employ a realistic cooling function, and find that a large fraction of the gas cools to ≲100K, so that the ISM becomes highly inhomogeneous. Despite this, our simulated galaxies reach an approximate steady state, in which gas gravitationally collapses to form giant 'molecular' clouds (GMCs), dense clumps and stars; subsequently, stellar feedback disperses the GMCs, repopulating the diffuse ISM. This collapse and dispersal cycle is seen in models of Small Magellanic Cloud (SMC)-like dwarfs, the Milky Way and z{\$\sim${}} 2 clumpy disc analogues. The simulated global star formation efficiencies are consistent with the observed Kennicutt-Schmidt relation. Moreover, the star formation rates are nearly independent of the numerically imposed high-density star formation efficiency, density threshold and density scaling. This is a consequence of the fact that, in our simulations, star formation is regulated by stellar feedback limiting the amount of very dense gas available for forming stars. In contrast, in simulations without stellar feedback, i.e. under the action of only gravity and gravitationally induced turbulence, the ISM experiences runaway collapse to very high densities. In these simulations without feedback, the global star formation rates exceed observed galactic star formation rates by 1-2 orders of magnitude, demonstrating that stellar feedback is crucial to the regulation of star formation in galaxies. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1101.4940}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2011.19306.x}, -eprint = {1101.4940}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation}, -number = {2}, -pages = {950--973}, -title = {{Self-regulated star formation in galaxies via momentum input from massive stars}}, -volume = {417}, -year = {2011} -} -@article{2001fa, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Greene2013, -abstract = {We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity dispersions sigma* {\textgreater}150 km/s. We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2 R{\_}e is old ({\$\sim${}}10 Gyr), relatively metal poor ([Fe/H] -0.5), and alpha-enhanced ([Mg/Fe]{\$\sim${}}0.3). The stars were made rapidly at z{\$\sim${}}1.5-2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to Milky Way thick disk stars. Our observations are thus consistent with a picture in which the stellar outskirts are built up through minor mergers with disky galaxies whose star formation is truncated early (z{\$\sim${}}1.5-2).}, -archivePrefix = {arXiv}, -arxivId = {1308.2682}, -author = {Greene, Jenny E and Murphy, Jeremy D and Graves, Genevieve J and Gunn, James E and Raskutti, Sudhir and Comerford, Julia M and Gebhardt, Karl}, -doi = {10.1088/0004-637X/776/2/64}, -eprint = {1308.2682}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: abundances,galaxies: elliptical and lenticular,galaxies: evolution}, -number = {2}, -title = {{The stellar halos of massive elliptical galaxies. II. Detailed abundance ratios at large radius}}, -volume = {776}, -year = {2013} -} -@article{Christensen2014, -abstract = {We present a detailed comparison between the photometric properties of the bulges of two simulated galaxies and those of a uniform sample of observed galaxies. This analysis shows that the simulated galaxies have bulges with realistic surface brightnesses for their sizes and magnitude. These two field disc galaxies have rotational velocities {\$\sim${}} 100 km/s and were integrated to a redshift of zero in a fully cosmological Lambda cold dark matter context as part of high-resolution smoothed particle hydrodynamic simulations. We performed bulge-disc decompositions of the galaxies using artificial observations, in order to conduct a fair comparison to observations. We also dynamically decomposed the galaxies and compared the star formation histories of the bulges to those of the entire galaxies. These star formation histories showed that the bulges were primarily formed before z = 1 and during periods of rapid star formation. Both galaxies have large amounts of early star formation, which is likely related to the relatively high bulge-to-disc ratios also measured for them. Unlike almost all previous cosmological simulations, the realistically concentrated bulges of these galaxies do not lead to unphysically high rotational velocities, causing them to naturally lie along the observed Tully-Fisher relation.}, -archivePrefix = {arXiv}, -arxivId = {1402.2702}, -author = {Christensen, C R and Brooks, A M and Fisher, D B and Governato, F and McCleary, J and Quinn, T R and Shen, S and Wadsley, J}, -doi = {10.1093/mnrasl/slu020}, -eprint = {1402.2702}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Bulges,Formation,Galaxies,Methods,Numerical,Spiral,Structure}, -number = {1}, -pages = {1--6}, -title = {{Simulating disc galaxy bulges that are consistent with observed scaling relations}}, -volume = {440}, -year = {2014} -} -@article{Shi2015, -abstract = {We study how halo intrinsic dynamical properties are linked to their formation processes for halos in two mass ranges, 1012-1012.5 h-1M⊙ and ≥1013 h-1M⊙, and how both are correlated with the large-scale tidal field within which the halos reside at present. We identify infall halos that are about to merge with their hosts. We find that the tangential infall velocity increases significantly with the strength of the tidal field, but no strong correlation is found for the radial component. These results can be used to explain the environmental dependence of internal velocity anisotropy and spin of halos. The position vectors and velocities of infall halos are aligned with the principal axes of the tidal field, and the alignment depends on the strength of the tidal field. Opposite accretion patterns are found in weak and strong tidal fields, showing that in a weak field the accretion flow is dominated by radial motion within the local structure, while a large tangential component is present in a strong field. These findings can be used to understand the strong alignments we find between the principal axes of the internal velocity ellipsoids of halos and the tidal field, and their dependence on the strength of the tidal field. We further find that only in weak tidal fields does the spin-tidal field alignment follow the prediction of the tidal torque theory. We discuss how our results may be used to understand the spins of disk galaxies and velocity structures of elliptical galaxies and their correlations with large-scale structure.}, -archivePrefix = {arXiv}, -arxivId = {1501.07764}, -author = {Shi, Jingjing and Wang, Huiyuan and Mo, H J}, -doi = {10.1088/0004-637X/807/1/37}, -eprint = {1501.07764}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: halos,large-scale structure of universe,methods: statistical}, -number = {1}, -title = {{Flow Patterns Around Dark Matter Halos: the Link Between Halo Dynamical Properties and Large-Scale Tidal Field}}, -volume = {807}, -year = {2015} -} -@article{Gadotti2008a, -abstract = {We have performed 2D bulge/bar/disc decompositions using g, r and i-band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for bulge-to-total ratio than the global Sersic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour-magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between bulge Sersic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass-size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass-size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs.}, -archivePrefix = {arXiv}, -arxivId = {0810.1953}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2008.14257.x}, -eprint = {0810.1953}, -isbn = {0372-9311 (Print){\$}\backslash{\$}r0372-9311 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {1531--1552}, -pmid = {20063786}, -title = {{Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: A Sloan Digital Sky Survey perspective}}, -url = {http://arxiv.org/abs/0810.1953%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2008.14257.x}, -volume = {393}, -year = {2009} -} -@article{Reines2015, -archivePrefix = {arXiv}, -arxivId = {arXiv:1508.06274v2}, -author = {Reines, Amy E and Volonteri, Marta}, -eprint = {arXiv:1508.06274v2}, -title = {{RELATIONS BETWEEN CENTRAL BLACK HOLE MASS AND TOTAL GALAXY STELLAR MASS IN THE and}}, -year = {2015} -} -@article{Xie:2015aa, -author = {Xie, L and Guo, Q and Cooper, A.$\sim$P. and Frenk, C.$\sim$S. and Li, R and Gao, L}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xie et al. - 2015 - The size evolution of elliptical galaxies(4).pdf:pdf}, -journal = {\mnras}, -month = {feb}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Hsu2018, -abstract = {We present a new framework to characterize the occurrence rates of planet candidates identified by Kepler based on hierarchical Bayesian modeling, Approximate Bayesian Computing (ABC), and sequential importance sampling. For this study we adopt a simple 2-D grid in planet radius and orbital period as our model and apply our algorithm to estimate occurrence rates for Q1-Q16 planet candidates orbiting around solar-type stars. We arrive at significantly increased planet occurrence rates for small planet candidates ($R_p<1.25 R_{\oplus}$) at larger orbital periods ($P>80$d) compared to the rates estimated by the more common inverse detection efficiency method. Our improved methodology estimates that the occurrence rate density of small planet candidates in the habitable zone of solar-type stars is $1.6^{+1.2}_{-0.5}$ per factor of 2 in planet radius and orbital period. Additionally, we observe a local minimum in the occurrence rate for strong planet candidates marginalized over orbital period between 1.5 and 2$R_{\oplus}$ that is consistent with previous studies. For future improvements, the forward modeling approach of ABC is ideally suited to incorporating multiple populations, such as planets, astrophysical false positives and pipeline false alarms, to provide accurate planet occurrence rates and uncertainties. Furthermore, ABC provides a practical statistical framework for answering complex questions (e.g., frequency of different planetary architectures) and providing sound uncertainties, even in the face of complex selection effects, observational biases, and follow-up strategies. In summary, ABC offers a powerful tool for accurately characterizing a wide variety of astrophysical populations.}, -archivePrefix = {arXiv}, -arxivId = {1803.10787}, -author = {Hsu, Danley C. and Ford, Eric B. and Ragozzine, Darin and Morehead, Robert C.}, -doi = {10.3847/1538-3881/aab9a8}, -eprint = {1803.10787}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hsu et al. - 2018 - Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation(2).pdf:pdf}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -keywords = {catalogs,data analysis,methods,planetary systems,stars,statistical,statistics}, -number = {5}, -pages = {205}, -title = {{ Improving the Accuracy of Planet Occurrence Rates from Kepler Using Approximate Bayesian Computation }}, -url = {http://arxiv.org/abs/1803.10787%0Ahttp://dx.doi.org/10.3847/1538-3881/aab9a8}, -volume = {155}, -year = {2018} -} -@article{MacKay1992, -abstract = {In this work, we present the results of ab-initio theoretical calculations concerning the electronic and optical properties of Si(001) surface covered by small hydrocarbon molecules, namely acetylene and ethylene. As a result of the adsorption process, both molecules are covalently bonded to the surface, and we point out analogies and differences of the two systems under study. The most stable configurations have been taken into account at different coverages. We will show how band structure and reflectance anisotropy spectra calculations supply additional indirect information concerning the adsorption geometry and the saturation coverage, that have been longly debated. {\textcopyright} 2008 Elsevier Ltd. All rights reserved.}, -author = {Marsili, Margherita and Pulci, Olivia and Palummo, Maurizia and Silvestrelli, Pier Luigi and {Del Sole}, Rodolfo}, -doi = {10.1016/j.spmi.2008.12.009}, -isbn = {9781467385879}, -issn = {07496036}, -journal = {Superlattices and Microstructures}, -keywords = {Acetylene,Adsorbates,Band structure,Cycloaddition,DFT,Ethylene,RAS,Si(100),Surfaces}, -number = {1-2}, -pages = {240--245}, -pmid = {22530192}, -title = {{Electronic and optical properties of acetylene and ethylene on Si(001)}}, -url = {http://citeseerx.ist.psu.edu/viewdoc/download?doi=10.1.1.31.4284&rep=rep1&type=pdf}, -volume = {46}, -year = {2009} -} -@article{Bacon2001, -abstract = {A new integral-field spectrograph, SAURON, is described. It is based on the TIGER principle, and uses a lenslet array. SAURON has a large field of view and high throughput, and allows simultaneous sky subtraction. Its design is optimized for studies of the stellar kinematics, gas kinematics, and line-strength distributions of nearby early-type galaxies. The instrument design and specifications are described, as well as the extensive analysis software which was developed to obtain fully calibrated spectra, and the associated kinematic and line-strength measurements. A companion paper will report on the first results obtained with SAURON on the William Herschel Telescope.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0103451}, -author = {Bacon, R. and Copin, Y. and Monnet, G. and Miller, Bryan W. and Allington-Smith, J. R. and Bureau, M. and Carollo, C. Marcella and Davies, Roger L. and Emsellem, Eric and Kuntschner, Harald and Peletier, Reynier F. and Verolme, E. K. and {De Zeeuw}, P. Tim}, -doi = {10.1046/j.1365-8711.2001.04612.x}, -eprint = {0103451}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bacon et al. - 2001 - The SAURON project - I. The panoramic integral-field spectrograph.pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: individual: NGC 3377,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content,Instrumentation: spectrographs}, -number = {1}, -pages = {23--35}, -pmid = {612842016}, -primaryClass = {astro-ph}, -title = {{The SAURON project - I. The panoramic integral-field spectrograph}}, -volume = {326}, -year = {2001} -} -@article{Agertz2011, -abstract = {We study the formation of disc galaxies in a fully cosmological framework using adaptive mesh refinement simulations. We perform an extensive parameter study of the main subgrid processes that control how gas is converted into stars and the coupled effect of supernovae feedback. We argue that previous attempts to form disc galaxies have been unsuccessful because of the universal adoption of strong feedback combined with high star formation efficiencies. Unless extreme amounts of energy are injected into the interstellar medium during supernovae events, these star formation parameters result in bulge-dominated S0/Sa galaxies as star formation is too efficient at z$\sim$ 3. We show that a low efficiency of star formation more closely models the subparsec physical processes, especially at high redshift. We highlight the successful formation of extended disc galaxies with scalelengths rd= 4-5 kpc, flat rotation curves and bulge-to-disc ratios of B/D $\sim$ 1/4. Not only do we resolve the formation of a Milky Way-like spiral galaxy, we also observe the secular evolution of the disc as it forms a pseudo-bulge. The disc properties agree well with observations and are compatible with the photometric and baryonic Tully-Fisher relations, the $\Sigma$SFR-$\Sigma$gas (Kennicutt-Schmidt) relation and the observed angular momentum content of spiral galaxies. We conclude that the underlying small-scale star formation physics plays a greater role than previously considered in simulations of galaxy formation. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1004.0005}, -author = {Agertz, Oscar and Teyssier, Romain and Moore, Ben}, -doi = {10.1111/j.1365-2966.2010.17530.x}, -eprint = {1004.0005}, -isbn = {0710305311}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes,Galaxies: spiral,Methods: numerical}, -month = {jan}, -number = {2}, -pages = {1391--1408}, -pmid = {619}, -title = {{The formation of disc galaxies in a $\Lambda$CDM universe}}, -volume = {410}, -year = {2011} -} -@article{Bullock2005a, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted $\sim$100-200 luminous satellite galaxies in the past \$\sim$12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ($\sim$80%) coming from the \$\sim$15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of $\sim$9 Gyr in the past, while surviving satellite systems have median accretion times of $\sim$5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S. and Johnston, Kathryn V.}, -doi = {10.1086/497422}, -eprint = {0506467}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bullock, Johnston - 2005 - Tracing Galaxy Formation with Stellar Halos. I. Methods.pdf:pdf}, -isbn = {0272-9490 (Print)\r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A. and Birnboim, Y. and Engel, G. and Freundlich, J. and Goerdt, T. and Mumcuoglu, M. and Neistein, E. and Pichon, C. and Teyssier, R. and Zinger, E.}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel et al. - 2009 - Cold streams in early massive hot haloes as the main mode of galaxy formation.pdf:pdf}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/19158792}, -volume = {457}, -year = {2009} -} -@article{Prodhomme2011, -abstract = {Current optical space telescopes rely upon silicon charge-coupled devices (CCDs) to detect and image the incoming photons. The performance of a CCD detector depends on its ability to transfer electrons through the silicon efficiently, so that the signal from every pixel may be read out through a single amplifier. This process of electron transfer is highly susceptible to the effects of solar proton damage (or non-ionizing radiation damage). This is because charged particles passing through the CCD displace silicon atoms, introducing energy levels into the semiconductor band gap which act as localized electron traps. The reduction in charge transfer efficiency (CTE) leads to signal loss and image smearing. The European Space Agency's astrometric Gaia mission will make extensive use of CCDs to create the most complete and accurate stereoscopic map to date of the Milky Way. In the context of the Gaia mission CTE is referred to with the complementary quantity charge transfer inefficiency (CTI = 1-CTE). CTI is an extremely important issue that threatens Gaia's performances: the CCDs are very large so that the electrons need to be transferred a long way; the focal plane is also very large and difficult to shield; the mission will operate at second Lagrange point where the direct solar protons are highly energetic (penetrating) and the science requirements on image quality are very stringent. In order to tackle this issue, in depth experimental studies and modelling efforts are being conducted to explore the possible consequences and to mitigate the anticipated effects of radiation damage. We present here a detailed Monte Carlo model that has been developed to simulate the operation of a damaged CCD at the pixel electrode level. This model implements a new approach to both the charge density distribution within a pixel and the charge capture and release probabilities, which allows the reproduction of CTI effects on a variety of measurements for a large signal level range in particular for signals of the order of a few electrons. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1103.3630}, -author = {Prod'homme, T. and Brown, A. G.A. and Lindegren, L. and Short, A. D.T. and Brown, S. W.}, -doi = {10.1111/j.1365-2966.2011.18537.x}, -eprint = {1103.3630}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Prod'homme et al. - 2011 - Electrode level Monte Carlo model of radiation damage effects on astronomical CCDs.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: data analysis,Methods: numerical,Space vehicles}, -number = {3}, -pages = {2215--2228}, -title = {{Electrode level Monte Carlo model of radiation damage effects on astronomical CCDs}}, -volume = {414}, -year = {2011} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M * = 1010.2 to 1012.0 M . We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority (≳75%) of elliptical galaxies is not well described by a single S{\'{e}}rsic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (Re ∼ 1 kpc) inner component with luminosity fraction f 0.1-0.15; an intermediate-scale (Re 2.5 kpc) middle component with f 0.2-0.25; and a dominant (f = 0.6), extended (Re 10 kpc) outer envelope. All subcomponents have average S{\'{e}}rsic indices n 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C. and Peng, Chien Y. and Li, Zhao Yu and Barth, Aaron J.}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2013 - The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{deZeeuw2002, -abstract = {Early results are reported from the SAURON survey of the kinematics and stellar populations of a representative sample of nearby E, S0 and Sa galaxies. The survey is aimed at determining the intrinsic shape of the galaxies, their orbital structure, the mass-to-light ratio as a function of radius, the age and metallicity of the stellar populations, and the frequency of kinematically decoupled cores and nuclear black holes. The construction of the representative sample is described, and its properties are illustrated. A comparison with long-slit spectroscopic data establishes that the SAURON measurements are comparable to, or better than, the highest-quality determinations. Comparisons are presented for NGC 3384 and 4365, where stellar velocities and velocity dispersions are determined to a precision of 6 km s-1, and the h3 and h4 parameters of the line-of-sight velocity distribution to a precision of better than 0.02. Extraction of accurate gas emission-line intensities, velocities and linewidths from the data cubes is illustrated for NGC 5813. Comparisons with published line strengths for NGC 3384 and 5813 reveal uncertainties of ≲ 0.1 {\AA} on the measurements of the H$\beta$, Mg b and Fe5270 indices. Integral-field mapping uniquely connects measurements of the kinematics and stellar populations to the galaxy morphology. The maps presented here illustrate the rich stellar kinematics, gaseous kinematics, and line-strength distributions of early-type galaxies. The results include the discovery of a thin, edge-on, disc in NGC 3623, confirm the axisymmetric shape of the central region of M32, illustrate the LINER nucleus and surrounding counter-rotating star-forming ring in NGC 7742, and suggest a uniform stellar population in the decoupled core galaxy NGC 5813.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0109511}, -author = {{De Zeeuw}, P. Tim and Bureau, M. and Emsellem, Eric and Bacon, R. and Carollo, Marcella C. and Copin, Y. and Davies, Roger L. and Kuntschner, Harald and Miller, Bryan W. and Monnet, G. and Peletier, Reynier F. and Verolme, E. K.}, -doi = {10.1046/j.1365-8711.2002.05059.x}, -eprint = {0109511}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: kinematics and dynamics,Galaxies: spiral,Galaxies: stellar content}, -number = {3}, -pages = {513--530}, -pmid = {25246403}, -primaryClass = {astro-ph}, -title = {{The SAURON project - II. Sample and early results}}, -volume = {329}, -year = {2002} -} -@article{Shi2015, -abstract = {We study how halo intrinsic dynamical properties are linked to their formation processes for halos in two mass ranges, 1012-1012.5 h-1M⊙ and ≥1013 h-1M⊙, and how both are correlated with the large-scale tidal field within which the halos reside at present. We identify infall halos that are about to merge with their hosts. We find that the tangential infall velocity increases significantly with the strength of the tidal field, but no strong correlation is found for the radial component. These results can be used to explain the environmental dependence of internal velocity anisotropy and spin of halos. The position vectors and velocities of infall halos are aligned with the principal axes of the tidal field, and the alignment depends on the strength of the tidal field. Opposite accretion patterns are found in weak and strong tidal fields, showing that in a weak field the accretion flow is dominated by radial motion within the local structure, while a large tangential component is present in a strong field. These findings can be used to understand the strong alignments we find between the principal axes of the internal velocity ellipsoids of halos and the tidal field, and their dependence on the strength of the tidal field. We further find that only in weak tidal fields does the spin-tidal field alignment follow the prediction of the tidal torque theory. We discuss how our results may be used to understand the spins of disk galaxies and velocity structures of elliptical galaxies and their correlations with large-scale structure.}, -archivePrefix = {arXiv}, -arxivId = {1501.07764}, -author = {Shi, Jingjing and Wang, Huiyuan and Mo, H J}, -doi = {10.1088/0004-637X/807/1/37}, -eprint = {1501.07764}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {dark matter,galaxies: halos,large-scale structure of universe,methods: statistical}, -number = {1}, -title = {{Flow Patterns Around Dark Matter Halos: the Link Between Halo Dynamical Properties and Large-Scale Tidal Field}}, -volume = {807}, -year = {2015} -} -@article{Vegetti2010, -abstract = {We report the detection of a dark substructure - undetected in the Hubble Space Telescope-HST ACS F814W image - in the gravitational lens galaxy SDSSJ0946+1006 (the 'double Einstein ring'), through direct gravitational imaging. The detection of a small mass concentration in the surface density maps, at 4.3 kpc from the galaxy centre, has a strong statistical significance. We confirm this detection by modelling the substructure with a tidally truncated pseudo-Jaffe density profile; in that case the substructure mass is Msub= (3.51 ± 0.15) × 109 M⊙, precisely where also the surface density map shows a strong convergence peak (Bayes factor; equivalent to a ∼16$\sigma$ detection). The result is robust under substantial changes in the model. We set a lower limit of (/L)V,⊙⊙ 120⊙ M⊙/LV,⊙ (3$\sigma$) inside a sphere of 0.3 kpc centred on the substructure (rtidal= 1.1 kpc). The mass and luminosity limit of this substructure are consistent with Local Group results if the substructure had a virial mass of ∼1010M⊙ before accretion and formed at z≳10. Our detection implies a projected dark matter mass fraction in substructure at the radius of the inner Einstein ring of f= 2.15+2.05-1.25 per cent [68 per cent confidence level (CL)] in the mass range 4 × 106- 4 × 109M⊙, assuming $\alpha$= 1.9 ± 0.1 (with dN/dm $\alpha$ m-$\alpha$). Assuming a flat prior on $\alpha$, between 1.0 and 3.0, increases this to f= 2.56+3.26-1.50 per cent (68 per cent CL). The likelihood ratio is ∼0.5 between these fractions and that from simulations (fN-body≈ 0.003). Hence the inferred dark matter mass fraction in substructure, admittedly based on a single-lens system, is large but still consistent with predictions. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0910.0760}, -author = {Vegetti, S. and Koopmans, L. V.E. and Bolton, A. and Treu, T. and Gavazzi, R.}, -doi = {10.1111/j.1365-2966.2010.16865.x}, -eprint = {0910.0760}, -isbn = {063114806X}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -month = {nov}, -number = {4}, -pages = {1969--1981}, -title = {{Detection of a dark substructure through gravitational imaging}}, -volume = {408}, -year = {2010} -} -@article{2001ex, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Barro2013, -abstract = {We combine high-resolution HST/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (log(M*) {\textgreater}10) galaxies at redshifts z = 1.4 - 3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5 - 3. At z {\textgreater}2 most cSFGs have specific star-formation rates (sSFR = 10{\^{}}-9 yr{\^{}}-1) half that of typical, massive SFGs at the same epoch, and host X-ray luminous AGN 30 times ({\$\sim${}}30{\%}) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 10{\^{}}8 yr). The cSFGs are continuously being formed at z = 2 - 3 and fade to cQGs by z = 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary scenarios of QG formation: an early (z {\textgreater}2), fast-formation path of rapidly-quenched cSFGs that evolve into cQGs that later enlarge within the quiescent phase, and a slow, late-arrival (z {\textless}2) path for SFGs to form QGs without passing through a compact state.}, -archivePrefix = {arXiv}, -arxivId = {1206.5000}, -author = {Barro, Guillermo and Faber, S M and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Koo, David C and Williams, Christina C and Kocevski, Dale D and Trump, Jonathan R and Mozena, Mark and McGrath, Elizabeth and {Van Der Wel}, Arjen and Wuyts, Stijn and Bell, Eric F and Croton, Darren J and Daniel, Ceverino and Dekel, Avishai and Ashby, M L N and Cheung, Edmond and Ferguson, Henry C and Fontana, Adriano and Fang, Jerome and Giavalisco, Mauro and Grogin, Norman A and Guo, Yicheng and Hathi, Nimish P and Hopkins, Philip F and Huang, Kuang Han and Koekemoer, Anton M and Kartaltepe, Jeyhan S and Lee, Kyoung Soo and Newman, Jeffrey A and Porter, Lauren A and Primack, Joel R and Ryan, Russell E and Rosario, David and Somerville, Rachel S and Salvato, Mara and Hsu, Li Ting}, -doi = {10.1088/0004-637X/765/2/104}, -eprint = {1206.5000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: high-redshift,galaxies: photometry,galaxies: starburst}, -number = {2}, -pmid = {7117407}, -title = {{Candels: The progenitors of compact quiescent galaxies at Z ∼ 2}}, -volume = {765}, -year = {2013} -} -@article{Hezaveh2016, -abstract = {We study the abundance of substructure in the matter density near galaxies using ALMA Science Verification observations of the strong lensing system SDP.81. We present a method to measure the abundance of subhalos around galaxies using interferometric observations of gravitational lenses. Using simulated ALMA observations, we explore the effects of various systematics, including antenna phase errors and source priors, and show how such errors may be measured or marginalized. We apply our formalism to ALMA observations of SDP.81. We find evidence for the presence of a $M=10^{8.96\pm 0.12} M_{\odot}$ subhalo near one of the images, with a significance of $6.9\sigma$ in a joint fit to data from bands 6 and 7; the effect of the subhalo is also detected in both bands individually. We also derive constraints on the abundance of dark matter subhalos down to $M\sim 2\times 10^7 M_{\odot}$, pushing down to the mass regime of the smallest detected satellites in the Local Group, where there are significant discrepancies between the observed population of luminous galaxies and predicted dark matter subhalos. We find hints of additional substructure, warranting further study using the full SDP.81 dataset (including, for example, the spectroscopic imaging of the lensed carbon monoxide emission). We compare the results of this search to the predictions of $\Lambda$CDM halos, and find that given current uncertainties in the host halo properties of SDP.81, our measurements of substructure are consistent with theoretical expectations. Observations of larger samples of gravitational lenses with ALMA should be able to improve the constraints on the abundance of galactic substructure.}, -archivePrefix = {arXiv}, -arxivId = {1601.01388}, -author = {Hezaveh, Yashar D. and Dalal, Neal and Marrone, Daniel P. and Mao, Yao-Yuan and Morningstar, Warren and Wen, Di and Blandford, Roger D. and Carlstrom, John E. and Fassnacht, Christopher D. and Holder, Gilbert P. and Kemball, Athol and Marshall, Philip J. and Murray, Norman and Levasseur, Laurence Perreault and Vieira, Joaquin D. and Wechsler, Risa H.}, -doi = {10.3847/0004-637x/823/1/37}, -eprint = {1601.01388}, -issn = {1538-4357}, -journal = {ApJ}, -keywords = {Astrophysics - Cosmology and Nongalactic Astrophys}, -month = {jan}, -number = {1}, -pages = {37}, -title = {{Detection of Lensing Substructure Using Alma Observations of the Dusty Galaxy Sdp.81}}, -url = {http://arxiv.org/abs/1601.01388%0Ahttp://dx.doi.org/10.3847/0004-637X/823/1/37}, -volume = {823}, -year = {2016} -} -@article{Gadotti2011, -abstract = {I present results from the modelling of stellar bars in nearly 300 barred galaxies in the local universe through parametric multicomponent multiband image fitting. The surface brightness radial profile of bars is described using a S{\'{e}}rsic function and parameters, such as the bar effective radius, ellipticity, boxiness, length and mass, and bar-to-total luminosity and mass ratios, are determined, which is unprecedented for a sample of this size. The properties of bars in galaxies with classical bulges and pseudo-bulges are compared. For a fixed bar-to-total mass ratio, pseudo-bulges are on average significantly less massive than classical bulges, indicating that, if pseudo-bulges are formed through bars, further processes are necessary to build a classical bulge. I find a correlation between bar ellipticity and boxiness, and define a new parameter as the product of these two quantities. I also find correlations between this product and the normalized bar size, between the sizes of bars and bulges, and between the normalized bar size and bulge-to-total ratio. Bars with different ellipticities follow parallel lines in the latter two correlations. These correlations can arise if, starting off with different normalized sizes and ellipticities, bars grow longer and stronger with dynamical age, as a result of angular momentum exchange between the inner and outer parts of galaxies, consistent with previous theoretical predictions. A plausible consequence is that bar pattern speeds should become lower with bar dynamical age and towards galaxies with more prominent bulges. {\textcopyright}2011 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1003.1719}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2011.18945.x}, -eprint = {1003.1719}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {3308--3318}, -title = {{Secular evolution and structural properties of stellar bars in galaxies}}, -volume = {415}, -year = {2011} -} -@article{Jin2017, -abstract = {We report the results from a recent 133 ks XMM-Newton observation of a highly super-Eddington narrow-line Type-1 QSO RX J0439.6-5311. This source has one of the steepest AGN hard X-ray slopes, in addition to a prominent and smooth soft X-ray excess. Strong variations are found throughout the 0.3 to 10 keV energy range on all time-scales covered by the observation, with the soft excess mainly showing low frequency variations below 0.1 mHz while the hard X-rays show stronger variability at higher frequencies. We perform a full set of spectral-timing analysis on the X-ray data, including a simultaneous modelling of the time-average spectra, frequency-dependent RMS and covariance spectra, lag-frequency and lag-energy spectra. Especially, we find a significant time-lag signal in the low frequency band, which indicates that the soft X-rays lead the hard by {\$}\backslashbackslashsim{\{}\backslash{\$}{\}}4 ks, with a broad continuum-like profile in the lag spectrum. Our analysis strongly supports the model where the soft X-ray excess is dominated by a separate low temperature, optically thick Comptonisation component rather than relativistic reflection or a jet. This soft X-ray emitting region is several tens or hundreds of {\$}R{\_}{\{}g{\}}{\$} away from the hot corona emitting hard X-rays, and is probably associated with a geometrically thick (`puffed-up') inner disc region.}, -archivePrefix = {arXiv}, -arxivId = {1703.07118}, -author = {Jin, Chichuan and Done, Chris and Ward, Martin}, -doi = {10.1093/mnras/stx718}, -eprint = {1703.07118}, -issn = {0035-8711}, -keywords = {accretion,accretion discs - galaxies,active - galaxies,nuclei}, -number = {June}, -pages = {1--17}, -title = {{Super-Eddington QSO RX J0439.6-5311. I. Origin of the Soft X-ray Excess and Structure of the Inner Accretion Flow}}, -url = {http://arxiv.org/abs/1703.07118%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx718}, -volume = {17}, -year = {2017} -} -@article{Warren2003, -abstract = {We describe a new method for analyzing gravitational lens images, for the case where the source light distribution is pixelized. The method is suitable for high resolution, high S/N data of a multiply-imaged extended source. For a given mass distribution, we show that the step of inverting the image to obtain the deconvolved pixelized source light distribution, and the uncertainties, is a linear one. This means that the only parameters of the non-linear problem are those required to model the mass distribution. This greatly simplifies the search for a min.-chi{\^{}}2 fit to the data and speeds up the inversion. The method is extended in a straightforward way to include linear regularization. We apply the method to simulated Einstein ring images and demonstrate the effectiveness of the inversion for both the unregularized and regularized cases.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0302587}, -author = {Warren, Steve and Dye, Simon}, -doi = {10.1086/375132}, -eprint = {0302587}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {COSMOLOGY: GRAVITATIONAL LENSING}, -month = {jun}, -pages = {673}, -primaryClass = {astro-ph}, -title = {{Semi-linear gravitational lens inversion}}, -url = {http://arxiv.org/abs/astro-ph/0302587%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/375132}, -volume = {590}, -year = {2003} -} -@article{DiazRivero2020, -abstract = {Strong gravitational lensing is a promising way of uncovering the nature of dark matter, by finding perturbations to images that cannot be accounted for well by modeling the lens galaxy without additional structure, be it subhalos (smaller halos within the smooth lens) or line-of-sight (LOS) halos. We present results attempting to infer the presence of substructure from images without requiring an intermediate step in which a smooth model has to be subtracted, using a simple convolutional neural network (CNN). We find that the network is only able to infer the presence of subhalos with greater than 75{\%} accuracy when they have masses of greater than or equal to 5×109M if they lie within the main lens galaxy. Since less massive foreground LOS halos can have the same effect as higher-mass subhalos, the CNN can probe lower masses in the halo mass function. The accuracy does not improve significantly if we add a population of less massive subhalos. With the expectation of experiments such as Hubble Space Telescope and Euclid yielding thousands of high-quality strong lensing images in the next years, having a way of analyzing images quickly to identify candidates that merit further analysis to determine individual subhalo properties while preventing extensive resources being used for images that would yield null detections could be very useful. By understanding the sensitivity as a function of substructure mass, nondetections could be combined with the information from images with substructure to constrain the cold dark matter scenario, in particular if the sensitivity can be pushed to lower masses.}, -archivePrefix = {arXiv}, -arxivId = {1910.00015}, -author = {{Diaz Rivero}, Ana and Dvorkin, Cora}, -doi = {10.1103/PhysRevD.101.023515}, -eprint = {1910.00015}, -issn = {24700029}, -journal = {Physical Review D}, -number = {2}, -pages = {1--17}, -title = {{Direct detection of dark matter substructure in strong lens images with convolutional neural networks}}, -volume = {101}, -year = {2020} -} -@article{Aguero2016, -abstract = {We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75{\%} of the hosts), with a bar (44{\%} weak, 37{\%} strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem not to be important for the appearance of CNRs, which appear to be more related to intrinsic properties of the host galaxies or to minor merger processes; 2) the proportion of weak bars in galaxies with a CNR is higher than expected; 3) the incidence of Seyfert (Sy) activity coeval with CNRs is significantly larger than the rate expected from the morphological distribution of the host galaxies; 4) the rate of Sy 2 to Sy 1 type galaxies with CNRs is about three times larger than the expected ratio for galaxies without CNRs and is opposite to that predicted by the geometric paradigm of the classical unified model for AGNs, although it does support the hypothesis that Sy 2 activity is linked to circumnuclear star formation. The possible selection effects of the sample are discussed, and we conclude that the detected trends are strong enough to justify high quality observations of as large as possible set of galaxies with circumnuclear rings and their matched control samples.}, -author = {Ag{\"{u}}ero, Mar{\'{i}}a P and D{\'{i}}az, Rub{\'{e}}n J and Dottori, Horacio}, -doi = {10.4236/ijaa.2016.63018}, -issn = {2161-4717}, -journal = {International Journal of Astronomy and Astrophysics}, -keywords = {active,dynamics,galaxies,nuclei,spiral,structure}, -number = {03}, -pages = {219--235}, -title = {{Nuclear Activity in Circumnuclear Ring Galaxies}}, -url = {http://www.scirp.org/journal/doi.aspx?DOI=10.4236/ijaa.2016.63018}, -volume = {06}, -year = {2016} -} -@article{James2018, -abstract = {We present the first spatially resolved rest-frame ultraviolet (UV) study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z = 2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each {\$\sim${}}4-8 kpc2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with C III] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. Themapped C III] emission shows distinct kinematical structure, with velocity offsets of {\$\sim${}}±50 km s-1 between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionization parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing in the range -200 ≲ v (km s-1) ≲ -50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star formation rates remain relatively constant ({\$\sim${}}8-16M⊙ yr-1), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced.We measure electron densities with a range of log (Ne)= 3.92-4.36 cm-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large-scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially resolved rest-frame UV studies expected with future observatories, such as James Webb Space Telescope.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L and Auger, Matt and Pettini, Max and Stark, Daniel P and Belokurov, V and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified {\$\sim${}}17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M {\textless}10{\^{}}9 M*), low-metallicity (Z{\$\sim${}}1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He $\backslash$ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A and Erb, Dawn K and Auger, Matthew W and Pettini, Max and Brammer, Gabriel B}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {164}, -title = {{ A Window on the Earliest Star Formation: Extreme Photoionization Conditions of a High-ionization, Low-metallicity Lensed Galaxy at z ∼ 2* }}, -url = {http://arxiv.org/abs/1803.02340}, -volume = {859}, -year = {2018} -} -@article{Handley2015, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Spavone2017, -abstract = {Observations of diffuse starlight in the outskirts of galaxies are thought to be a fundamental source of constraint on the cosmological context of galaxy assembly in the $\Lambda$CDM model. Such observations are not trivial because of the extreme faintness of such regions. In this work, we investigated the photometric properties of six massive early-type galaxies (ETGs) in the VEGAS sample (NGC 1399, NGC 3923, NGC 4365, NGC 4472, NGC 5044, and NGC 5846) out to extremely low surface brightness levels with the goal of characterizing the global structure of their light profiles for comparison to state-of-the-art galaxy formation models. We carried out deep and detailed photometric mapping of our ETG sample taking advantage of deep imaging with VST/OmegaCAM in the g and i bands. By fitting the light profiles, and comparing the results to simulations of elliptical galaxy assembly, we have identified signatures of a transition between relaxed and unrelaxed accreted components and can constrain the balance between in situ and accreted stars. The very good agreement of our results with predictions from theoretical simulations demonstrates that the full VEGAS sample of $\sim$100 ETGs will allow us to use the distribution of diffuse light as a robust statistical probe of the hierarchical assembly of massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1703.10835}, -author = {Spavone, Marilena and Capaccioli, Massimo and Napolitano, Nicola R. and Iodice, Enrichetta and Grado, Aniello and Limatola, Luca and Cooper, Andrew P. and Cantiello, Michele and Forbes, Duncan A. and Paolillo, Maurizio and Schipani, Pietro}, -doi = {10.1051/0004-6361/201629111}, -eprint = {1703.10835}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Spavone et al. - 2017 - VEGAS A VST Early-type GAlaxy Survey II. Photometric study of giant ellipticals and their stellar halos(2).pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: halos,Techniques: image processing}, -number = {3}, -pages = {A38}, -title = {{VEGAS: A VST Early-type GAlaxy Survey: II. Photometric study of giant ellipticals and their stellar halos}}, -url = {http://www.aanda.org/10.1051/0004-6361/201629111}, -volume = {603}, -year = {2017} -} -@article{Cooper2013, -abstract = {We have combined the semi-analytic galaxy formation model of Guo et al. with the particletagging technique of Cooper et al. to predict galaxy surface brightness profiles in a representative sample of {\$\sim${}}1900 massive dark matter haloes (1012-1014M⊙) from the Millennium II $\lambda$ cold dark matter N-body simulation. Here, we present our method and basic results focusing on the outer regions of galaxies, consisting of stars accreted in mergers. These simulations cover scales from the stellar haloes of MilkyWay-like galaxies to the 'cD envelopes' of groups and clusters, and resolve low surface brightness substructure such as tidal streams. We find that the surface density of accreted stellar mass around the central galaxies of dark matter haloes is well described by a S{\`{e}}rsic profile, the radial scale and amplitude of which vary systematically with halo mass (M200). The total stellar mass surface density profile breaks at the radius where accreted stars start to dominate over stars formed in the galaxy itself. This break disappears with increasing M200 because accreted stars contribute more of the total mass of galaxies, and is less distinct when the same galaxies are averaged in bins of stellar mass, because of scatter in the relation between M* and M200. To test our model, we have derived average stellar mass surface density profiles for massive galaxies at z ≈ 0.08 by stacking Sloan Digital Sky Survey images. Our model agrees well with these stacked profiles and with other data from the literature and makes predictions that can be more rigorously tested by future surveys that extend the analysis of the outer structure of galaxies to fainter isophotes. We conclude that it is likely that the outer structure of the spheroidal components of galaxies is largely determined by collisionless merging during their hierarchical assembly. {\textcopyright}2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.6283}, -author = {Cooper, Andrew P and D'Souza, Richard and Kauffmann, Guinevere and Wang, Jing and Boylan-Kolchin, Michael and Guo, Qi and Frenk, Carlos S and White, Simon D M}, -doi = {10.1093/mnras/stt1245}, -eprint = {1303.6283}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {4}, -pages = {3348--3367}, -title = {{Galactic accretion and the outer structure of galaxies in the CDM model}}, -volume = {434}, -year = {2013} -} -@article{Gomer2021, -abstract = {Galaxy lenses are frequently modeled as an elliptical mass distribution with external shear and isothermal spheres to account for secondary and line-of-sight galaxies. There is statistical evidence that some fraction of observed quads are inconsistent with these assumptions, and require a dipole-like contribution to the mass with respect to the light. Simplifying assumptions about the shape of mass distributions can lead to the incorrect recovery of parameters such as $H_0$. We create several tests of synthetic quad populations with different deviations from an elliptical shape, then fit them with an ellipse+shear model, and measure the recovered values of $H_0$. Kinematic constraints are not included. We perform two types of fittings -- one with a single point source and one with an array of sources emulating an extended source. We carry out two model-free comparisons between our mock quads and the observed population. One result of these comparisons is a statistical inconsistency not yet mentioned in the literature: the image distance ratios with respect to the lens center of observed quads appear to span a much wider range than those of synthetic or simulated quads. Bearing this discrepancy in mind, our mock populations can result in biases on $H_0$ $\sim10\%$.}, -archivePrefix = {arXiv}, -arxivId = {2103.16359}, -author = {Gomer, Matthew R. and Williams, Liliya L. R.}, -eprint = {2103.16359}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Gomer2021ShearEllipseDegen.pdf:pdf}, -keywords = {distance scale,galaxies,gravitational lensing,haloes,stellar,strong}, -number = {March}, -pages = {1--15}, -title = {{Galaxy-lens determination of $H_0$: the effect of the ellipse+shear modeling assumption}}, -url = {http://arxiv.org/abs/2103.16359}, -volume = {15}, -year = {2021} -} -@article{Behroozi2010, -abstract = {Urgent and heavy demand of high energy/power density lithium-ion batteries (LIBs) challenges the ultimate limit of commercial anodes. Herein, enlightened by the extra capacity on transition metal oxides (TMO) anodes derived from the transition metal (TM) catalytic effect on reversible solid-electrolyte interface (SEI) films, a ternary composite consisting of TM, TMO, and carbon matrix, namely TM/TMO/carbon, is proposed as a novel and high-efficiency anode prototype. In this electrode design, TMO not only serve as active material but also pulverizes the TM nanoparticles via the conversion reaction during cycling. Pulverized TM nanoparticles can activate and/or promote the reversible transformation of SEI films more efficiently. And carbon matrix ensures the electronic conductivity and integrity of the overall electrode during multiple electrochemical reactions. As a proof-of-concept demonstration, NiCo-NiCo2O4@carbon nanotubes (NC-NCO@CNTs) is synthesized by a bottom-up strategy via in-situ growth on a simplified chemical vapor deposition (CVD) process. As designed, the NC-NCO@CNTs keeps gaining extra capacity upon cycling, delivering an unceasingly increased capacity up to 1324 mAh g−1 (500 mA g−1), splendid rate performance (945 mAh g−1 at 1000 mA g−1, 696 mAh g−1 at 2000 mA g−1), and ultralong lifespan (2200 cycles). Detailed electrochemical investigation reveals a transformation of lithium storage mechanism from battery-type conversion reaction to pseudocapacitive electrochemical interfacial reaction arising from SEI films. It is believed that our work offers a novel and effective prototype for designing high energy/power density anodes for LIBs.}, -archivePrefix = {arXiv}, -arxivId = {1001.0015}, -author = {Ding, Chunyan and Wang, Lijuan and Zhou, Weiwei and Wang, Dong and Du, Yu and Wen, Guangwu}, -doi = {10.1016/j.cej.2018.07.125}, -eprint = {1001.0015}, -isbn = {10.1088/0004-637X/717/1/379}, -issn = {13858947}, -journal = {Chemical Engineering Journal}, -keywords = {CNTs,Chemical vapor deposition,Lithium-ion battery,NiCo2O4,Pseudocapacitive electrode,Reversible SEI films}, -month = {jul}, -number = {1}, -pages = {340--349}, -title = {{New design on Li-ion battery anode of ternary complex metal/metal oxide@CNT: A case study of hierarchical NiCo-NiCo2O4@CNTs}}, -url = {http://arxiv.org/abs/1001.0015}, -volume = {353}, -year = {2018} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-$\alpha$ emission from the host galaxy of SDSS$\sim$J2222+2745, a strongly lensed quasar at $z = 2.8$. Spectroscopic follow-up clearly reveals extended Lyman-$\alpha$ in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as $\sim$200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-$\alpha$ emission to its physical origin on one side of the host galaxy at radii $\sim$0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-$\alpha$ and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-$\alpha$, host galaxy Lyman-$\alpha$, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B. and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D. and Rigby, Jane R. and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bayliss et al. - 2017 - Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy(2).pdf:pdf}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani} and Caldwell, Nelson}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M * = 1010.2 to 1012.0 M . We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority (≳75%) of elliptical galaxies is not well described by a single S{\'{e}}rsic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (Re ∼ 1 kpc) inner component with luminosity fraction f 0.1-0.15; an intermediate-scale (Re 2.5 kpc) middle component with f 0.2-0.25; and a dominant (f = 0.6), extended (Re 10 kpc) outer envelope. All subcomponents have average S{\'{e}}rsic indices n 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C. and Peng, Chien Y. and Li, Zhao Yu and Barth, Aaron J.}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2013 - The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies.pdf:pdf}, -issn = {15384357}, -journal = {ApJ}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{Velliscig2015b, -abstract = {We report results for the alignments of galaxies in the EAGLE and cosmo-OWLS hydrodynamical cosmological simulations as a function of galaxy separation (-1 ≤ log10(r/[h-1Mpc]) ≤ 2) and halo mass (10.7 ≤ log10(M200/[h-1M⊙]) ≤ 15). We focus on two classes of alignments: the orientations of galaxies with respect to either the directions to, or the orientations of, surrounding galaxies. We find that the strength of the alignment is a strongly decreasing function of the distance between galaxies. For galaxies hosted by the mostmassive haloes in our simulations the alignment can remain significant up to $\sim$ 100Mpc. Galaxies hosted by more massive haloes show stronger alignment. At a fixed halo mass, more aspherical or prolate galaxies exhibit stronger alignments. The spatial distribution of satellites is anisotropic and significantly aligned with the major axis of the main host halo. The major axes of satellite galaxies, when all stars are considered, are preferentially aligned towards the centre of themain host halo. The predicted projected direction-orientation alignment, Εg+(rp), is in broad agreement with recent observations.We find that the orientation-orientation alignment is weaker than the orientation-direction alignment on all scales. Overall, the strength of galaxy alignments depends strongly on the subset of stars that are used to measure the orientations of galaxies and it is always weaker than the alignment of dark matter haloes. Thus, alignment models that use halo orientation as a direct proxy for galaxy orientation overestimate the impact of intrinsic galaxy alignments.}, -archivePrefix = {arXiv}, -arxivId = {1507.06996}, -author = {Velliscig, Marco and Cacciato, Marcello and Schaye, Joop and Hoekstra, Henk and Bower, Richard G. and Crain, Robert A. and van Daalen, Marcel P. and Furlong, Michelle and McCarthy, I. G. and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stv2198}, -eprint = {1507.06996}, -isbn = {1326-5377 (Electronic)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: large-scale structure of the Universe,Cosmology: theory,Galaxies: formation,galaxies: haloes}, -month = {dec}, -number = {3}, -pages = {3328--3340}, -title = {{Intrinsic alignments of galaxies in the EAGLE and cosmo-OWLS simulations}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.454.3328V}, -volume = {454}, -year = {2015} -} -@article{Belfiore2017, -abstract = {We study radial profiles in Ha equivalent width and specific star formation rate (sSFR) derived from spatially resolved SDSS-IV MaNGA spectroscopy to gain insight on the physical mechanisms that suppress star formation and determine a galaxy's location in the SFR-M* diagram. Even within the star-forming 'main sequence', the measured sSFR decreases with stellar mass, in both an integrated and spatially resolved sense. Flat sSFR radial profiles are observed for log(M*/M⊙) < 10.5, while star-forming galaxies of higher mass show a significant decrease in sSFR in the central regions, a likely consequence of both larger bulges and an inside-out growth history. Our primary focus is the green valley, constituted by galaxies lying below the star formation main sequence, but not fully passive. In the green valley we find sSFR profiles that are suppressed with respect to star-forming galaxies of the same mass at all galactocentric distances out to 2 effective radii. The responsible quenching mechanism therefore appears to affect the entire galaxy, not simply an expanding central region. The majority of green valley galaxies of log(M*/M⊙) > 10.0 are classified spectroscopically as central low-ionization emission-line regions (cLIERs). Despite displaying a higher central stellar mass concentration, the sSFR suppression observed in cLIER galaxies is not simply due to the larger mass of the bulge. Drawing a comparison sample of star-forming galaxies with the sameM* and $\Sigma$1 kpc (the mass surface density within 1 kpc), we show that a high $\Sigma$1 kpc is not a sufficient condition for determining central quiescence.}, -archivePrefix = {arXiv}, -arxivId = {1710.05034}, -author = {Belfiore, Francesco and Maiolino, Roberto and Bundy, Kevin and Masters, Karen and Bershady, Matthew and Oyarz{\'{u}}n, Grecco A. and Lin, Lihwai and Cano-Diaz, Mariana and Wake, David and Spindler, Ashley and Thomas, Daniel and Brownstein, Joel R. and Drory, Niv and Yan, Renbin}, -doi = {10.1093/mnras/sty768}, -eprint = {1710.05034}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Belfiore et al. - 2018 - SDSS IV MaNGA - sSFR profiles and the slow quenching of discs in green valley galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Evolution,Galaxies: Fundamental parameters,Galaxies: ISM}, -number = {3}, -pages = {3014--3029}, -title = {{SDSS IV MaNGA - sSFR profiles and the slow quenching of discs in green valley galaxies}}, -url = {http://arxiv.org/abs/1710.05034}, -volume = {477}, -year = {2018} -} -@article{Skottfelt2017a, -abstract = {The VISible imager instrument (VIS) on board the Euclid mission will deliver high resolution shape measurements of galaxies down to very faint limits (R ∼ 25 at 10$\sigma$) in a large part of the sky, in order to infer the distribution of dark matter in the Universe. To help mitigate radiation damage effects that will accumulate in the detectors over the mission lifetime, the properties of the radiation induced traps needs to be known with as high precision as possible. For this purpose the trap pumping method will be employed as part of the in-orbit calibration routines. Using trap pumping it is possible to identify and characterise single traps in a Charge-Coupled Device (CCD), thus providing information such as the density, emission time constants and sub-pixel positions of the traps in the detectors. This paper presents the trap pumping algorithms used for the radiation testing campaign of the CCD273 detectors, performed by the Centre for Electronic Imaging (CEI) at the Open University, that will be used for the VIS instrument. The CCD273 is a four-phase device with uneven phase widths, which complicates the trap pumping analysis. However, we find that by optimising the trap pumping algorithms and analysis routines, it is possible to obtain sub-pixel and even sub-phase positional information about the traps. Further, by comparing trap pumping data with simulations, it is possible to gain more information about the effective electrode widths of the device.}, -author = {Skottfelt, J. and Hall, D. J. and Dryer, B. and Bush, N. and Campa, J. and Gow, J. P.D. and Holland, A. D. and Jordan, D. and Burt, D.}, -doi = {10.1088/1748-0221/12/12/C12033}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Skottfelt et al. - 2017 - Trap pumping schemes for the Euclid CCD273 detector Characterisation of electrodes and defects.pdf:pdf}, -issn = {17480221}, -journal = {J. Instrum.}, -keywords = {Data analysis,Detector modelling and simulations II (electric fi,Detectors for UV,Space instrumentation,visible and IR photons}, -number = {12}, -title = {{Trap pumping schemes for the Euclid CCD273 detector: Characterisation of electrodes and defects}}, -volume = {12}, -year = {2017} -} -@article{Lauer2005, -abstract = {We present observations of 77 early-type galaxies imaged with the PC1 CCD of the Hubble Space Telescope (HST) WFPC2. "Nuker-law" parametric fits to the surface brightness profiles are used to classify the central structure into "core" or "power-law" forms. Core galaxies are typically rounder than power-law galaxies. Nearly all power-law galaxies with central ellipticities $\epsilon$ ≥ 0.3 have stellar disks, implying that disks are present in power-law galaxies with $\epsilon$ < 0.3 but are not visible because of unfavorable geometry. A few low-luminosity flattened core galaxies also have disks; these may be transition forms from power-law galaxies to more luminous core galaxies, which lack disks. Several core galaxies have strong isophote twists interior to their break radii, although power-law galaxies have interior twists of similar physical significance when the photometric perturbations implied by the twists are evaluated. Central color gradients are typically consistent with the envelope gradients; core galaxies have somewhat weaker color gradients than power-law galaxies. Nuclei are found in 29% of the core galaxies and 60% of the power-law galaxies. Nuclei are typically bluer than the surrounding galaxy. While some nuclei are associated with active galactic nuclei (AGNs), just as many are not; conversely, not all galaxies known to have a low-level AGN exhibit detectable nuclei in the broadband filters. NGC 4073 and 4382 are found to have central minima in their intrinsic starlight distributions; NGC 4382 resembles the double nucleus of M31. In general, the peak brightness location is coincident with the photocenter of the core to a typical physical scale of < 1 pc. Five galaxies, however, have centers significantly displaced from their surrounding cores; these may be unresolved asymmetric double nuclei. Finally, as noted by previous authors, central dust is visible in about half of the galaxies. The presence and strength of dust correlates with nuclear emission; thus, dust may outline gas that is falling into the central black hole. The prevalence of dust and its morphology suggest that dust clouds form, settle to the center, and disappear repeatedly on ∼ 10 8 yr timescales. We discuss the hypothesis that cores are created by the decay of a massive black hole binary formed in a merger. Apart from their brightness profiles, there are no strong differences between core galaxies and power-law galaxies that demand this scenario; however, the rounder shapes of core, their lack of disks, and their reduced color gradients may be consistent with it. {\textcopyright} 2005. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0412040}, -author = {Lauer, Tod R. and Faber, S. M. and Gebhardt, Karl and Richstone, Douglas and Tremaine, Scott and Ajhar, Edward A. and Aller, M. C. and Bender, Ralf and Dressler, Alan and Filippenko, Alexei V. and Green, Richard and Grillmair, Carl J. and Ho, Luis C. and Kormendy, John and Magorrian, John and Pinkney, Jason and Siopis, Christos}, -doi = {10.1086/429565}, -eprint = {0412040}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lauer et al. - 2005 - The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry.pdf:pdf}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2138--2185}, -primaryClass = {arXiv:astro-ph}, -title = {{ The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry }}, -url = {http://stacks.iop.org/1538-3881/129/i=5/a=2138}, -volume = {129}, -year = {2005} -} -@article{Liao2016, -abstract = {The standard galaxy formation theory assumes that baryons and dark matter are initially well mixed before becoming segregated due to radiative cooling. We use non-radiative hydrodynamical simulations to explicitly examine this assumption and find that baryons and dark matter can also be segregated due to different characteristics of gas and dark matter during the buildup of the halo. As a result, baryons in many haloes do not originate from the same Lagrangian region as the dark matter. When using the fraction of corresponding dark matter and gas particles in the initial conditions (the 'paired fraction') as a proxy of the dark matter and gas segregation strength of a halo, on average about 25 per cent of the baryonic and dark matter of the final halo are segregated in the initial conditions. This is at odds with the assumption of the standard galaxy formation model. A consequence of this effect is that the baryons and dark matter of the same halo initially experience different tidal torques and thus their angular momentum vectors are often misaligned. The degree of the misalignment is largely preserved during later halo assembly and can be understood with the tidal torque theory. The result challenges the precision of some semi-analytical approaches that utilize dark matter halo merger trees to infer properties of gas associated with dark matter haloes.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.07592}, -author = {Liao, Shihong and Gao, Liang and Frenk, Carlos S and Guo, Qi and Wang, Jie}, -doi = {10.1093/mnras/stx1391}, -eprint = {1610.07592}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: structure,Methods: numerical}, -number = {2}, -pages = {2262--2269}, -title = {{The segregation of baryons and dark matter during halo assembly}}, -url = {http://arxiv.org/abs/1610.07592}, -volume = {470}, -year = {2017} -} -@article{Geometryeq, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Du2020, -abstract = {We recently developed an automated method, auto-GMM, to kinematically decompose simulated galaxies. It extracts the kinematic structures in an accurate, efficient, and unsupervised way. Here we use auto-GMM to study the stellar kinematic structures of disk galaxies from the TNG100 run of the cosmological suite IllustrisTNG. We identify four to five kinematic structures that are commonly present among the diverse galaxy population. Structures having strong to moderate rotation are defined as cold and warm disks, respectively. Spheroidal structures dominated by random motions are classified as bulges or stellar halos, depending on how tightly bound they are. Disky bulges are defined as structures that have moderate rotation but compact morphology. TNG100 returns multiple structures that have reasonable properties, qualitatively consistent with our general expectations. Across all disky galaxies and accounting for the stellar mass within 3 half-mass radii, the kinematic spheroidal structures, obtained by summing up stars of bulges and halos, contribute {\$}\backslashsim 45\backslash{\%}{\$} of the total stellar mass, while the disky structures constitute {\$}\backslashsim 55\backslash{\%}{\$}. This study also provides important insights about the relationship between kinematically and morphologically derived galactic structures. Comparing the morphology of kinematic structures with that of traditional bulge+disk decomposition, we conclude: (1) the morphologically decomposed bulges are composite structures comprised of a slowly rotating bulge, an inner halo, and a disky bulge; (2) kinematically disky bulges, akin to what are commonly called pseudo bulges in observations, are compact disk-like components that have rotation similar to warm disks; (3) halos contribute almost {\$}30\backslash{\%}{\$} of the surface density of the outer part of morphological disks when viewed face-on; and (4) both cold and warm disks are often truncated in central regions.}, -archivePrefix = {arXiv}, -arxivId = {2002.04182}, -author = {Du, Min and Ho, Luis C and Debattista, Victor P and Pillepich, Annalisa and Nelson, Dylan and Zhao, Dongyao and Hernquist, Lars}, -eprint = {2002.04182}, -keywords = {391,591,602,622,767,corresponding author,disk galaxies,galaxy dynamics,galaxy kinematics,galaxy structure,hydrodynamical simulations,min du}, -number = {3}, -title = {{Kinematic decomposition of IllustrisTNG disk galaxies: morphology and relation with morphological structures}}, -url = {http://arxiv.org/abs/2002.04182}, -year = {2020} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9602085}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}$\backslash${\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashsigma{\$} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and {P{\'{e}}rez Gonz{\'{a}}lez}, Pablo G and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {112}, -title = {{ CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z ∼ 2 }}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -volume = {846}, -year = {2017} -} -@article{Smith2018, -abstract = {Strong gravitational lensing can provide accurate measurements of the stellar mass-to-light ratio ϒ in low-redshift (z≲0.05) early-type galaxies, and hence probe for possible variations in the stellar initial mass function (IMF). However, true multiple imaging lens systems are rare, hindering the construction of large nearby lens samples. Here, we present a method to derive upper limits on ϒ in galaxies with single close-projected background sources, where no counter-image is detected, down to some relative flux limit. We present a proof-of-principle application to three galaxies with integral field observations from different instruments. In our first case study, only a weak constraint on ϒ is obtained. In the second, the absence of a detectable counter-image excludes stellar masses higher than expected for a Salpeter IMF. In the third system, the current observations do not yield a useful limit, but our analysis indicates that deeper observations should reveal a counter-image if the stellar mass is any larger than expected for a Milky Way IMF. We discuss how our method can help enlarge the current samples of low-redshift galaxies with lensing constraints, both by adding upper limits on ϒ and by guiding follow-up of promising single-image systems in search of fainter counter-images.}, -archivePrefix = {arXiv}, -arxivId = {1808.08235}, -author = {Smith, Russell J. and Lucey, John R. and Collier, William P.}, -doi = {10.1093/MNRAS/STY2328}, -eprint = {1808.08235}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Smith2018UpperLimit.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Gravitational lensing: strong,cD,galaxies: elliptical and lenticular}, -number = {2}, -pages = {2115--2124}, -title = {{'Upper-limit lensing': Constraining galaxy stellar masses with singly imaged background sources}}, -volume = {481}, -year = {2018} -} -@article{Xie2014, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P. and Frenk, Carlos S. and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Xie et al. - 2015 - The size evolution of elliptical galaxies(4).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stu2487}, -volume = {447}, -year = {2015} -} -@article{Veale2017a, -abstract = {We analyse the environmental properties of 370 local early-type galaxies (ETGs) in the MASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute {\$}K{\$}-band magnitude {\$}-21.5 {\textgreater} M{\_}K {\textgreater} -26.6{\$}, or stellar mass {\$}8 \backslashtimes 10{\^{}}{\{}9{\}} {\textless} M{\_}* {\textless} 2 \backslashtimes 10{\^{}}{\{}12{\}} M{\_}\backslashodot{\$}. We find these galaxies to reside in a diverse range of environments measured by four methods: group membership (whether a galaxy is a brightest group/cluster galaxy, satellite, or isolated), halo mass, large-scale mass density (measured over a few Mpc), and local mass density (measured within the {\$}N{\$}th neighbour). The spatially resolved IFS stellar kinematics provide robust measurements of the spin parameter {\$}\backslashlambda{\_}e{\$} and enable us to examine the relationship among {\$}\backslashlambda{\_}e{\$}, {\$}M{\_}*{\$}, and galaxy environment. We find a strong correlation between {\$}\backslashlambda{\_}e{\$} and {\$}M{\_}*{\$}, where the average {\$}\backslashlambda{\_}e{\$} decreases from {\$}\backslashsim 0.4{\$} to below 0.1 with increasing mass, and the fraction of slow rotators {\$}f{\_}{\{}\backslashrm slow{\}}{\$} increases from {\$}\backslashsim 10{\$}{\%} to 90{\%}. We show for the first time that at fixed {\$}M{\_}*{\$}, there are almost no trends between galaxy spin and environment; the apparent kinematic morphology-density relation for ETGs is therefore primarily driven by {\$}M{\_}*{\$} and is accounted for by the joint correlations between {\$}M{\_}*{\$} and spin, and between {\$}M{\_}*{\$} and environment. A possible exception is that the increased {\$}f{\_}{\{}\backslashrm slow{\}}{\$} at high local density is slightly more than expected based only on these joint correlations. Our results suggest that the physical processes responsible for building up the present-day stellar masses of massive galaxies are also very efficient at reducing their spin, in any environment.}, -archivePrefix = {arXiv}, -arxivId = {1703.08573}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and McConnell, Nicholas and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/mnras/stx1639}, -eprint = {1703.08573}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {2}, -pages = {1428--1445}, -title = {{The MASSIVE Survey - VII. The relationship of angular momentum, stellar mass and environment of early-type galaxies}}, -url = {http://arxiv.org/abs/1703.08573%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1639}, -volume = {471}, -year = {2017} -} -@article{Sonnenfeld2018b, -abstract = {The Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) is an excellent survey for the search for strong lenses, thanks to its area, image quality, and depth. We use three different methods to look for lenses among 43000 luminous red galaxies from the Baryon Oscillation Spectroscopic Survey (BOSS) sample with photometry from the S16A internal data release of the HSC-SSP. The first method is a newly developed algorithm, named YATTALENS, which looks for arc-like features around massive galaxies and then estimates the likelihood of an object being a lens by performing a lens model fit. The second method, CHITAH, is a modeling-based algorithm originally developed to look for lensed quasars. The third method makes use of spectroscopic data to look for emission lines from objects at a different redshift from that of the main galaxy. We find 15 definite lenses, 36 highly probable lenses, and 282 possible lenses. Among the three methods, YATTALENS, which was developed specifically for this study, performs best in terms of both completeness and purity. Nevertheless, five highly probable lenses were missed by YATTALENS but found by the other two methods, indicating that the three methods are highly complementary. Based on these numbers, we expect to find ∼300 definite or probable lenses by the end of the HSC-SSP.}, -archivePrefix = {arXiv}, -arxivId = {1704.01585}, -author = {Sonnenfeld, Alessandro and Chan, James H.H. and Shu, Yiping and More, Anupreeta and Oguri, Masamune and Suyu, Sherry H. and Wong, Kenneth C. and Lee, Chien Hsiu and Coupon, Jean and Yonehara, Atsunori and Bolton, Adam S. and Jaelani, Anton T. and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/pasj/psx062}, -eprint = {1704.01585}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnenfeld2018Yattalens.pdf:pdf}, -issn = {2053051X}, -journal = {PASJ}, -keywords = {CD-gravitational lensing,Elliptical and lenticular,Galaxies,Strong-surveys}, -number = {Special Issue 1}, -pages = {1--18}, -title = {{Survey of Gravitationally-lensed Objects in HSC Imaging (SuGOHI). I. Automatic search for galaxy-scale strong lenses}}, -volume = {70}, -year = {2018} -} -@article{Guo2008a, -abstract = {We use galaxy and dark halo data from the public database for the Millennium Simulation to study the growth of galaxies in the De Lucia et al. model for galaxy formation. Previous work has shown this model to reproduce many aspects of the systematic properties and the clustering of real galaxies, both in the nearby universe and at high redshift. It assumes the stellar masses of galaxies to increase through three processes, major mergers, the accretion of smaller satellite systems and star formation. We show the relative importance of these three modes to be a strong function of stellar mass and redshift. Galaxy growth through major mergers depends strongly on stellar mass, but only weakly on redshift. Except for massive systems, minor mergers contribute more to galaxy growth than major mergers at all redshifts and stellar masses. For galaxies significantly less massive than the Milky Way, star formation dominates the growth at all epochs. For galaxies significantly more massive than the Milky Way, growth through mergers is the dominant process at all epochs. At a stellar mass of 6 × 1010 M⊙, about that of the Milk Way, star formation dominates at z > 1 and mergers at later times. At every stellar mass, the growth rates through star formation increase rapidly with increasing redshift. Specific star formation rates are the decreasing function of stellar mass not only at z = 0 but also at all higher redshifts. For comparison, we carry out a similar analysis of the growth of dark matter haloes. In contrast to the galaxies, growth rates depend strongly on redshift, but only weakly on mass. They agree qualitatively with analytic predictions for halo growth. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0708.1814}, -author = {Guo, Q. and White, S. D.M.}, -doi = {10.1111/j.1365-2966.2007.12619.x}, -eprint = {0708.1814}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Guo, White - 2008 - Galaxy growth in the concordance $\Lambda$cDM cosmology.pdf:pdf}, -isbn = {0311325823}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: evolution,Galaxies: formation,Galaxies: high-redshift,Galaxies: interactions}, -number = {1}, -pages = {2--10}, -title = {{Galaxy growth in the concordance $\Lambda$cDM cosmology}}, -volume = {384}, -year = {2008} -} -@article{Eisenstein2001, -abstract = {We describe the target selection and resulting properties of a spectroscopic sample of luminous, red galaxies (LRG) from the imaging data of the Sloan Digital Sky Survey (SDSS). These galaxies are selected on the basis of color and magnitude to yield a sample of luminous, intrinsically red galaxies that extends fainter and further than the main flux-limited portion of the SDSS galaxy spectroscopic sample. The sample is designed to impose a passively-evolving luminosity and rest-frame color cut to a redshift of 0.38. Additional, yet more luminous, red galaxies are included to a redshift of 0.5. Approximately 12 of these galaxies per square degree are targeted for spectroscopy, so the sample will number over 100,000 with the full survey. SDSS commissioning data indicate that the algorithm efficiently selects luminous (M{\_}g=-21.4), red galaxies, that the spectroscopic success rate is very high, and that the resulting set of galaxies is approximately volume-limited out to z=0.38. When the SDSS is complete, the LRG spectroscopic sample will fill over 1h{\^{}}-3 Gpc{\^{}}3 with an approximately homogeneous population of galaxies and will therefore be well suited to studies of large-scale structure and clusters out to z=0.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0108153}, -author = {Eisenstein, D J and Annis, J and Gunn, J E and Szalay, A S and Connolly, A J and Nichol, R C and Bahcall, N A and Bernardi, M and Burles, S and Castander, F J and Fukugita, M and Hogg, D W and Ivezic, Z and Knapp, G R and Lupton, R H and Narayanan, V and Postman, M and Riechart, D E and Richmond, M and Schneider, D P and Schlegel, D J and Strauss, M A and SubbaRao, M and Tucker, D L and Berk, D Vanden and Vogeley, M S and Weinberg, D H and Yanny, B}, -doi = {10.1086/323717}, -eprint = {0108153}, -isbn = {0004-6256}, -issn = {00046256}, -pages = {1--30}, -primaryClass = {astro-ph}, -title = {{Spectroscopic Target Selection for the Sloan Digital Sky Survey: The Luminous Red Galaxy Sample}}, -url = {http://arxiv.org/abs/astro-ph/0108153%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/323717}, -year = {2001} -} -@article{Birnboim2003, -abstract = {We investigate the conditions for the existence of an expanding virial shock in the gas falling within a spherical dark matter halo. The shock relies on pressure support by the shock-heated gas behind it. When the radiative cooling is efficient compared with the infall rate, the post-shock gas becomes unstable; it collapses inwards and cannot support the shock. We find for a monatomic gas that the shock is stable when the post-shock pressure and density obey $\gamma$eff ≡ (d ln P/dt)/(d ln $\rho$/dt) > 10/7. When expressed in terms of the pre-shock gas properties at radius r it reads as $\rho$r$\Lambda$(T)/u3 < 0.0126, where $\rho$ is the gas density, u is the infall velocity and $\Lambda$(T) is the cooling function, with the post-shock temperature T ∝ u2. This result is confirmed by hydrodynamical simulations, using an accurate spheri-symmetric Lagrangian code. When the stability analysis is applied in cosmology, we find that a virial shock does not develop in most haloes that form before z ∼ 2, and it never forms in haloes less massive than a few 1011 M⊙. In such haloes, the infalling gas is not heated to the virial temperature until it hits the disc, thus avoiding the cooling-dominated quasi-static contraction phase. The direct collapse of the cold gas into the disc should have non-trivial effects on the star formation rate and on outflows. The soft X-ray produced by the shock-heated gas in the disc is expected to ionize the dense disc environment, and the subsequent recombination would result in a high flux of L$\alpha$ emission. This may explain both the puzzling low flux of soft X-ray background and the L$\alpha$ emitters observed at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0302161}, -author = {Birnboim, Yuval and Dekel, Avishai}, -doi = {10.1046/j.1365-8711.2003.06955.x}, -eprint = {0302161}, -isbn = {9788578110796}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Dark matter,Galaxies: ISM,Galaxies: formation,Hydrodynamics,Shock waves}, -month = {oct}, -number = {1}, -pages = {349--364}, -pmid = {25246403}, -primaryClass = {astro-ph}, -title = {{Virial shocks in galactic haloes?}}, -volume = {345}, -year = {2003} -} -@inproceedings{Short2010, -abstract = {The European Space Agency's Gaia mission1 is scheduled for launch in 2012. It will operate at L2 for 5 years, rotating slowly so that its two optical telescopes will repeatedly observe more than one billion stars. The resulting data set will be iteratively reduced to solve for the relative position, parallax-distance and proper motion of every observed star, yielding a three dimensional dynamical model of our galaxy. The focal plane contains 106 large area silicon CCDs continuously operating in TDI mode at a line rate synchronised with the satellite rotation.2 One of the greatest challenges facing the mission is radiation damage in the CCDs which will cause charge loss and image distortion. This is particularly severe because the large focal plane is difficult to shield and because the launch will coincide with solar maximum. Despite steps taken to minimize the effects of radiation (e.g. regular use of charge injection), the residual distortion will need to be calibrated during the pipeline data processing. Due to the volume of data involved, this requires a trapping model which is physically realistic, yet fast enough and simple enough to implement in the pipeline. The current prototype Charge Distortion Model will be presented. This model was developed specifically for Gaia in TDI mode. However, an imaging mode version has already been applied to other missions, for example, to indicate the potential impact of radiation damage on the proposed Euclid mission.}, -author = {Short, Alexander and Prod'homme, Thibaut and Weiler, Michael and Brown, Scott and Brown, Anthony}, -booktitle = {High Energy, Optical, and Infrared Detectors for Astronomy IV}, -doi = {10.1117/12.856386}, -isbn = {9780819482327}, -issn = {0277786X}, -keywords = {Astronomy,CCD,Charge loss,Data processing,Data sets,Detectors,Distortion model,Dynamical model,Electron trapping,Euclid,European Space Agency,FAST model,Focal Plane,Focusing,Gaia,Gaia mission,Geometrical optics,High energy physics,Image distortions,Imaging modes,Infrared detectors,Launching,Line rate,Optical telescopes,Pipeline processing systems,Potential impacts,Proper motion,Radiation,Radiation damage,Radiation-induced,Relative positions,Residual distortions,Rotation,Solar maxima,Three dimensional,Trapping model,modelling,radiation damage}, -month = {jul}, -pages = {774212}, -series = {\procspie}, -title = {{A fast model of radiation-induced electron trapping in CCDs for implementation in the Gaia data processing}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.856386}, -volume = {7742}, -year = {2010} -} -@article{Cooper:2015aa, -abstract = {We study the formation of stellar haloes in three MilkyWay-mass galaxies using cosmological smoothed particle hydrodynamics simulations, focusing on the subset of halo stars that form in situ, as opposed to those accreted from satellites. In situ stars in our simulations dominate the stellar halo out to 20 kpc and account for 30-40 per cent of its total mass. We separate in situ halo stars into three straightforward, physically distinct categories according to their origin: stars scattered from the disc of the main galaxy ('heated disc'), stars formed from gas smoothly accreted on to the halo ('smooth' gas) and stars formed in streams of gas stripped from infalling satellites ('stripped' gas).We find that most belong to the stripped gas category. Those originating in smooth gas outside the disc tend to form at the same time and place as the stripped-gas population, suggesting that their formation is associated with the same gas-rich accretion events. The scattered disc star contribution is negligible overall but significant in the solar neighbourhood, where ≳90 per cent of stars on eccentric orbits once belonged to the disc. However, the distinction between halo and thick disc in this region is highly ambiguous. The chemical and kinematic properties of the different components are very similar at the present day, but the global properties of the in situ halo differ substantially between the three galaxies in our study. In our simulations, the hierarchical buildup of structure is the driving force behind not only the accreted stellar halo, but also those halo stars formed in situ.}, -archivePrefix = {arXiv}, -arxivId = {1501.04630}, -author = {Cooper, Andrew P. and Parry, Owen H. and Lowing, Ben and Cole, Shaun and Frenk, Carlos}, -doi = {10.1093/mnras/stv2057}, -eprint = {1501.04630}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cooper et al. - 2015 - Formation of in situ stellar haloes in Milky Way-mass galaxies(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxies: haloes,Galaxies: structure,Methods: numerical}, -month = {dec}, -number = {3}, -pages = {3185--3199}, -title = {{Formation of in situ stellar haloes in Milky Way-mass galaxies}}, -volume = {454}, -year = {2015} -} -@article{Wang2018a, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}} \backslashleqslant M{\_}{\{}\backslashast{\}} \backslashleqslant 10{\^{}}{\{}11.9{\}}\backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashlangle\backslashgamma{\^{}}{\{}\backslashprime{\}}\backslashrangle = 2.003 \backslashpm 0.008{\$} and a standard deviation of {\$}\backslashsigma{\_}{\{}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashgamma{\^{}}{\{}\backslashprime{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashgamma{\_}{\{}\backslashmathrm{\{}mw{\}}{\}}{\^{}}{\{}\backslashprime{\}}-f{\_}{\{}\backslashmathrm{\{}DM{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -year = {2018} -} -@article{2001er, -author = {عامر, د. وفاء محروس}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/عامر - 2001 - No Title المعالجة الحيوية للمولوثات البيئية(10).pdf:pdf}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Sawala2016, -abstract = {Since reionization prevents star formation in most haloes less massive than 3 × 109M⊙, dwarf galaxies only populate a fraction of existing dark matter haloes. We use hydrodynamic cosmological simulations of the Local Group to study the discriminating factors for galaxy formation in the early Universe and connect them to the present-day properties of galaxies and haloes. A combination of selection effects related to reionization, and the subsequent evolution of haloes in different environments, introduces strong biases between the population of haloes that host dwarf galaxies, and the total halo population. Haloes that host galaxies formed earlier and are more concentrated. In addition, haloes more affected by tidal stripping are more likely to host a galaxy for a given mass or maximum circular velocity, vmax, today. Consequently, satellite haloes are populated more frequently than field haloes, and satellite haloes of 108-109M⊙ or vmax of 12-20 km s-1, compatible with stellar kinematics of Local Group dwarf spheroidals, have experienced a greater than average reduction in both mass and vmax after infall. They are on closer, more radial orbits with higher infall velocities and earlier infall times. Together, these effects make dwarf galaxies highly biased tracers of the underlying dark matter distribution.}, -archivePrefix = {arXiv}, -arxivId = {1406.6362}, -author = {Sawala, Till and Frenk, Carlos S. and Fattahi, Azadeh and Navarro, Julio F. and Theuns, Tom and Bower, Richard G. and Crain, Robert A. and Furlong, Michelle and Jenkins, Adrian and Schaller, Matthieu and Schaye, Joop}, -doi = {10.1093/mnras/stv2597}, -eprint = {1406.6362}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sawala et al. - 2016 - The chosen few The low-mass haloes that host faint galaxies.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmology: theory,Galaxies: dwarf,Galaxies: formation,Local group,Methods: numerical}, -number = {1}, -pages = {85--97}, -title = {{The chosen few: The low-mass haloes that host faint galaxies}}, -volume = {456}, -year = {2016} -} -@article{Hopkins2011b, -abstract = {Feedback from massive stars is believed to play a critical role in shaping the galaxy mass function, the structure of the interstellar medium (ISM) and the low efficiency of star formation, but the exact form of the feedback is uncertain. In this paper, the first in a series, we present and test a novel numerical implementation of stellar feedback resulting from momentum imparted to the ISM by radiation, supernovae and stellar winds. We employ a realistic cooling function, and find that a large fraction of the gas cools to ≲100K, so that the ISM becomes highly inhomogeneous. Despite this, our simulated galaxies reach an approximate steady state, in which gas gravitationally collapses to form giant 'molecular' clouds (GMCs), dense clumps and stars; subsequently, stellar feedback disperses the GMCs, repopulating the diffuse ISM. This collapse and dispersal cycle is seen in models of Small Magellanic Cloud (SMC)-like dwarfs, the Milky Way and z$\sim$ 2 clumpy disc analogues. The simulated global star formation efficiencies are consistent with the observed Kennicutt-Schmidt relation. Moreover, the star formation rates are nearly independent of the numerically imposed high-density star formation efficiency, density threshold and density scaling. This is a consequence of the fact that, in our simulations, star formation is regulated by stellar feedback limiting the amount of very dense gas available for forming stars. In contrast, in simulations without stellar feedback, i.e. under the action of only gravity and gravitationally induced turbulence, the ISM experiences runaway collapse to very high densities. In these simulations without feedback, the global star formation rates exceed observed galactic star formation rates by 1-2 orders of magnitude, demonstrating that stellar feedback is crucial to the regulation of star formation in galaxies. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1101.4940}, -author = {Hopkins, Philip F. and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2011.19306.x}, -eprint = {1101.4940}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins, Quataert, Murray - 2011 - Self-regulated star formation in galaxies via momentum input from massive stars.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation}, -number = {2}, -pages = {950--973}, -title = {{Self-regulated star formation in galaxies via momentum input from massive stars}}, -volume = {417}, -year = {2011} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in {\$\sim${}}10 dynamical times, or {\$\sim${}}0.5Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, {\$\sim${}}100 Msun/yr, and each clump converts into stars in {\$\sim${}}0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z{\$\sim${}}3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z{\$\sim${}}1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Lovell2018, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of {\$}10{\^{}}{\{}10.7{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}} \backslashbackslashleqslant M{\_}{\{}\backslashbackslashast{\{}\backslash{\}}{\}} \backslashbackslashleqslant 10{\^{}}{\{}11.9{\}}\backslashbackslashmathrm{\{}\backslash{\{}{\}}M{\{}\backslash{\}}{\}}{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$} at {\$}z = 0{\$}, the total power-law slope has a mean of {\$}\backslashbackslashlangle\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}\backslashbackslashrangle = 2.003 \backslashbackslashpm 0.008{\$} and a standard deviation of {\$}\backslashbackslashsigma{\{}\backslash{\_}{\}}{\{}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\}} = 0.175{\$} over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and {\$}\backslashbackslashgamma{\{}\backslash{\^{}}{\{}{\}}{\}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}{\$} is almost constant with redshift below {\$}z = 2{\$}. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter {\$}c{\_}{\{}200{\}}{\$} in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, {\$}\backslashbackslashgamma{\{}\backslash{\_}{\}}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}mw{\{}\backslash{\}}{\}}{\}}{\^{}}{\{}\backslashbackslashprime{\{}\backslash{\}}{\}}-f{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}DM{\{}\backslash{\}}{\}}{\}}{\$}, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {dm,galaxies,galaxy,kinematic and dynamic,structure}, -number = {2}, -pages = {1950--1975}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {481}, -year = {2018} -} -@article{Cirasuolo2007, -abstract = {ABSTRACT We present new results on the cosmological evolution of the near-infrared (near-IR) galaxy luminosity function (LF), derived from the analysis of a new sample of ∼22 000 KAB ≤ 22.5 galaxies selected over an area of 0.6 deg2 from the Early Data Release of the UKIDSS Ultra Deep Survey (UDS). Our study has exploited the multiwavelength coverage of the UDS field provided by the new UKIDSS WFCAM K- and J-band imaging, the Subaru/XMM-Newton Deep Survey and the Spitzer Wide-Area Infrared Extragalactic survey. The unique combination of large area and depth provided by this new survey minimizes the complicating effect of cosmic variance and has allowed us, for the first time, to trace the evolution of the brightest sources out to z ≃ 2 with good statistical accuracy. In agreement with previous studies, we find that the characteristic luminosity of the near-IR LF brightens by ≃1 mag between z = 0 and z ≃ 2, while the total density decreases by a factor of ≃2. Using the rest-frame (U - B) colour to split the sample into red and blue galaxies, we confirm the classic luminosity-dependent colour bimodality at z ≲ 1. However, the strength of the colour bimodality is found to be a decreasing function of redshift, and seems to disappear by z ≳ 1.5. Due to the large size of our sample, we are able to investigate the differing cosmological evolution of the red and blue galaxy populations. It is found that the space density of the brightest red galaxies (MK ≤ - 23) stays approximately constant with redshift, and that these sources dominate the bright end of the LF at redshifts z ≲ 1. In contrast, the brightening of the characteristic luminosity and mild decrease in space density displayed by the blue galaxy population leads them to dominate the bright end of the LF at redshifts z ≳ 1. {\textcopyright} 2007 The Authors. Journal compilation {\textcopyright} 2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0609287}, -author = {Cirasuolo, M. and McLure, R. J. and Dunlop, J. S. and Almaini, O. and Foucaud, S. and Smail, Ian and Sekiguchi, K. and Simpson, C. and Eales, S. and Dye, S. and Watson, M. G. and Page, M. J. and Hirst, P.}, -doi = {10.1111/j.1365-2966.2007.12038.x}, -eprint = {0609287}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Galaxies: evolution,Galaxies: formation}, -month = {sep}, -number = {2}, -pages = {585--595}, -primaryClass = {astro-ph}, -title = {{The evolution of the near-infrared galaxy luminosity function and colour bimodality up to z ≃ 2 from the UKIDSS Ultra Deep Survey Early Data Release}}, -volume = {380}, -year = {2007} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for {\$\sim${}}20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Wong2019, -abstract = {We present a measurement of the Hubble constant (H0) and other cosmological parameters from a joint analysis of six gravitationally lensed quasars with measured time delays. All lenses except the first are analyzed blindly with respect to the cosmological parameters. In a flat $\Lambda$CDM cosmology, we find {\$}H{\_}{\{}0{\}} = 73.3{\_}{\{}-1.8{\}}{\^{}}{\{}+1.7{\}}{\\sim{}}\backslashmathrm{\{}km{\\sim{}}s{\^{}}{\{}-1{\}}{\\sim{}}Mpc{\^{}}{\{}-1{\}}{\}}{\$}, a {\$}2.4{\{}{\{}\backslash \backslashrm per\backslash cent{\}}{\}}{\$} precision measurement, in agreement with local measurements of H0 from type Ia supernovae calibrated by the distance ladder, but in 3.1$\sigma$ tension with Planck observations of the cosmic microwave background (CMB). This method is completely independent of both the supernovae and CMB analyses. A combination of time-delay cosmography and the distance ladder results is in 5.3$\sigma$ tension with Planck CMB determinations of H0 in flat $\Lambda$CDM. We compute Bayes factors to verify that all lenses give statistically consistent results, showing that we are not underestimating our uncertainties and are able to control our systematics. We explore extensions to flat $\Lambda$CDM using constraints from time-delay cosmography alone, as well as combinations with other cosmological probes, including CMB observations from Planck, baryon acoustic oscillations, and type Ia supernovae. Time-delay cosmography improves the precision of the other probes, demonstrating the strong complementarity. Allowing for spatial curvature does not resolve the tension with Planck. Using the distance constraints from time-delay cosmography to anchor the type Ia supernova distance scale, we reduce the sensitivity of our H0 inference to cosmological model assumptions. For six different cosmological models, our combined inference on H0 ranges from ∼73–78 km s−1 Mpc−1, which is consistent with the local distance ladder constraints.}, -archivePrefix = {arXiv}, -arxivId = {1907.04869}, -author = {Wong, Kenneth C and Suyu, Sherry H and Chen, Geoff C-F and Rusu, Cristian E and Millon, Martin and Sluse, Dominique and Bonvin, Vivien and Fassnacht, Christopher D and Taubenberger, Stefan and Auger, Matthew W and Birrer, Simon and Chan, James H H and Courbin, Frederic and Hilbert, Stefan and Tihhonova, Olga and Treu, Tommaso and Agnello, Adriano and Ding, Xuheng and Jee, Inh and Komatsu, Eiichiro and Shajib, Anowar J and Sonnenfeld, Alessandro and Blandford, Roger D and Koopmans, L{\'{e}}on V E and Marshall, Philip J and Meylan, Georges}, -doi = {10.1093/mnras/stz3094}, -eprint = {1907.04869}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {cosmological parameters,cosmology,dis-,gravitational lensing,observations,strong,tance scale}, -number = {November}, -title = {{H0LiCOW XIII. A 2.4{\%} measurement of H0 from lensed quasars: 5.3$\sigma$ tension between early and late-Universe probes}}, -url = {http://arxiv.org/abs/1907.04869}, -year = {2020} -} -@article{Rusu2019, -abstract = {We present the lens mass model of the quadruply-imaged gravitationally lensed quasar WFI2033−4723, and perform a blind cosmographical analysis based on this system. Our analysis combines (1) time-delay measurements from 14 years of data obtained by the COSmological MOnitoring of GRAvItational Lenses (COSMOGRAIL) collaboration, (2) high-resolution Hubble Space Telescope imaging, (3) a measurement of the velocity dispersion of the lens galaxy based on ESO-MUSE data, and (4) multi-band, wide-field imaging and spectroscopy characterizing the lens environment. We account for all known sources of systematics, including the influence of nearby perturbers and complex line-of-sight structure, as well as the parametrization of the light and mass profiles of the lensing galaxy. After unblinding, we determine the effective time-delay distance to be {\$}4784{\_}{\{}-248{\}}{\^{}}{\{}+399{\}}{\\sim{}}\backslashmathrm{\{}Mpc{\}}{\$}, an average precision of {\$}6.6{\{}{\{}\backslash \backslashrm per\backslash cent{\}}{\}}{\$}. This translates to a Hubble constant {\$}H{\_}{\{}0{\}} = 71.6{\_}{\{}-4.9{\}}{\^{}}{\{}+3.8{\}}{\\sim{}}\backslashmathrm{\{}km{\\sim{}}s{\^{}}{\{}-1{\}}{\\sim{}}Mpc{\^{}}{\{}-1{\}}{\}}{\$}, assuming a flat $\Lambda$CDM cosmology with a uniform prior on $\Omega$m in the range [0.05, 0.5]. This work is part of the H0 Lenses in COSMOGRAIL's Wellspring (H0LiCOW) collaboration, and the full time-delay cosmography results from a total of six strongly lensed systems are presented in a companion paper (H0LiCOW XIII).}, -archivePrefix = {arXiv}, -arxivId = {1905.09338}, -author = {Rusu, Cristian E and Wong, Kenneth C and Bonvin, Vivien and Sluse, Dominique and Suyu, Sherry H and Fassnacht, Christopher D and Chan, James H H and Hilbert, Stefan and Auger, Matthew W and Sonnenfeld, Alessandro and Birrer, Simon and Courbin, Frederic and Treu, Tommaso and Chen, Geoff C-F and Halkola, Aleksi and Koopmans, L{\'{e}}on V E and Marshall, Philip J and Shajib, Anowar J}, -doi = {10.1093/mnras/stz3451}, -eprint = {1905.09338}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmological parameters,cosmology,distance scale}, -pages = {0--29}, -title = {{H0LiCOW XII. Lens mass model of WFI2033−4723and blind measurement of its time-delay distance and H0}}, -url = {http://arxiv.org/abs/1905.09338}, -year = {2020} -} -@article{Gadotti2008a, -abstract = {We have performed 2D bulge/bar/disc decompositions using g, r and i-band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for the bulge-to-total ratio than the global S{\'{e}}rsic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour-magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between the bulge S{\'{e}}rsic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass-size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass-size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0810.1953}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2008.14257.x}, -eprint = {0810.1953}, -isbn = {0372-9311 (Print){\$}\backslash{\$}r0372-9311 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {1531--1552}, -pmid = {20063786}, -title = {{Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: A Sloan Digital Sky Survey perspective}}, -url = {http://arxiv.org/abs/0810.1953%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2008.14257.x}, -volume = {393}, -year = {2009} -} -@article{Amorisco:2017aa, -abstract = {The accreted component of stellar halos is composed of the contributions of several satellites, falling onto their host with their different masses, at different times, on different orbits. This work uses a suite of idealised, collisionless N-body simulations of minor mergers and a particle tagging technique to understand how these different ingredients shape each contribution to the accreted halo, in both density and kinematics. I find that more massive satellites deposit their stars deeper into the gravitational potential of the host, with a clear segregation enforced by dynamical friction. Earlier accretion events contribute more to the inner regions of the halo; more concentrated subhaloes sink deeper through increased dynamical friction. The orbital circularity of the progenitor at infall is only important for low-mass satellites: dynamical friction efficiently radialises the most massive minor mergers erasing the imprint of the infall orbit for satellite-to-host virial mass ratios {\$}\backslashgtrsim1/20{\$}. The kinematics of the stars contributed by each satellite is also ordered with satellite mass: low-mass satellites contribute fast-moving populations, in both ordered rotation and radial velocity dispersion. In turn, contributions by massive satellites have lower velocity dispersion and lose their angular momentum to dynamical friction, resulting in a strong radial anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {1511.08806}, -author = {Amorisco, N C}, -doi = {10.1093/mnras/stw2229}, -eprint = {1511.08806}, -journal = {$\backslash$mnras}, -month = {jan}, -pages = {2882--2895}, -title = {{Contributions to the accreted stellar halo: an atlas of stellar deposition}}, -url = {http://arxiv.org/abs/1511.08806%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2229}, -volume = {464}, -year = {2015} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/19158792}, -volume = {457}, -year = {2009} -} -@article{Bluck2014, -abstract = {We investigate the origin of galaxy bimodality by quantifying the relative role of intrinsic and environmental drivers to the cessation (or 'quenching') of star formation in over half a million local Sloan Digital Sky Survey galaxies. Our sample contains a wide variety of galaxies at z = 0.02-0.2, with stellar masses of 8 < log(M*/M⊙) < 12, spanning the entire morphological range from pure discs to spheroids, and over four orders of magnitude in local galaxy density and halo mass. We utilize published star formation rates and add to this recent GIM2D photometric and stellar mass bulge + disc decompositions from our group.We find that the passive fraction of galaxies increases steeply with stellar mass, halo mass, and bulge mass, with a less steep dependence on local galaxy density and bulge-to-total stellarmass ratio (B/T). At fixed internal properties, we find that central and satellite galaxies have different passive fraction relationships. For centrals, we conclude that there is less variation in the passive fraction at a fixed bulge mass, than for any other variable, including total stellar mass, halo mass, and B/T. This implies that the quenching mechanism must be most tightly coupled to the bulge.We argue that radio-mode active galactic nucleus feedback offers the most plausible explanation of the observed trends. {\textcopyright} 2014 The Author Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.5269}, -author = {Bluck, Asa F.L. and {Trevor Mendel}, J. and Ellison, Sara L. and Moreno, Jorge and Simard, Luc and Patton, David R. and Starkenburg, Else}, -doi = {10.1093/mnras/stu594}, -eprint = {1403.5269}, -isbn = {1529-2401 (Electronic)\r0270-6474 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: haloes,Galaxies: star formation,Galaxies: structure}, -month = {jun}, -number = {1}, -pages = {599--629}, -pmid = {21307233}, -title = {{Bulge mass is king: The dominant role of the bulge in determining the fraction of passive galaxies in the sloan digital sky survey}}, -url = {http://adsabs.harvard.edu/abs/2014MNRAS.441..599B}, -volume = {441}, -year = {2014} -} -@article{Dye2008a, -abstract = {We model the extremely massive and luminous lens galaxy in the Cosmic Horseshoe Einstein ring system J1004+4112, recently discovered in the Sloan Digital Sky Survey. We use the semilinear method of Warren & Dye, which pixelizes the source surface brightness distribution, to invert the Einstein ring for sets of parametrized lens models. Here, the method is refined by exploiting Bayesian inference to optimise adaptive pixelization of the source plane and to choose between three differently parametrized models: a singular isothermal ellipsoid, a power-law model and a Navarro, Frenk & White (NFW) profile. The most probable lens model is the power law with a volume mass density $\rho$ ∝ r-1.96±0.02 and an axis ratio of $\sim$0.8. The mass within the Einstein ring (i.e. within a cylinder with projected distance of $\sim$30 kpc from the centre of the lens galaxy) is (5.02 ± 0.09) × 1012 MȮ, and the mass-to-light ratio is $\sim$30. Even though the lens lies in a group of galaxies, the preferred value of the external shear is almost zero. This makes the Cosmic Horseshoe unique amongst large separation lenses, as almost all the deflection comes from a single, very massive galaxy with little boost from the environment. {\textcopyright} 2008 The Authors. Journal compilation {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:0804.4002v2}, -author = {Dye, S. and Evans, N. W. and Belokurov, V. and Warren, S. J. and Hewett, P.}, -doi = {10.1111/j.1365-2966.2008.13401.x}, -eprint = {arXiv:0804.4002v2}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Dye2009Horseshoe.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: structure,Gravitational lensing}, -number = {1}, -pages = {384--392}, -title = {{Models of the Cosmic Horseshoe gravitational lens J1004+4112}}, -volume = {388}, -year = {2008} -} -@article{Zavala2012, -abstract = {We use the combined data sets of the Millennium I and II cosmological simulations to revisit the impact of mergers in the growth of bulges in central galaxies in the $\Lambda$ cold dark matter ($\Lambda$CDM) scenario. We seed galaxies within the growing CDM haloes using semi-empirical relations to assign stellar and gaseous masses, and an analytic treatment to estimate the transfer of stellar mass to the bulge of the remnant after a galaxy merger. We find that this model roughly reproduces the observed correlation between the bulge-to-total mass (B/T) ratio and stellar mass (M *) in present-day central galaxies as well as their observed demographics, although low-mass B/T < 0.1 (bulgeless) galaxies might be scarce relative to the observed abundance. In our merger-driven scenario, bulges have a composite stellar population made of (i) stars acquired from infalling satellites, (ii) stars transferred from the primary disc due to merger-induced perturbations and (iii) newly formed stars in starbursts triggered by mergers. We find that the first two are the main channels of mass assembly, with the first one being dominant for massive galaxies, creating large bulges with different stellar populations than those of the inner discs, while the second is dominant for intermediate/low-mass galaxies and creates small bulges with similar stellar populations to the inner discs. We associate the dominion of the first (second) channel to classical (pseudo) bulges, and compare the predicted fractions to observations. We emphasize that our treatment does not include other mechanisms of bulge growth such as intrinsic secular processes in the disc or misaligned gas accretion. Interestingly, we find that the evolution of the stellar and gaseous contents of the satellite as it spirals towards the central galaxy is a key ingredient in setting the morphology of the remnant galaxy, and that a good match to the observed bulge demographics occurs when this evolution proceeds closely to that of the central galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1204.0516}, -author = {Zavala, Jesus and Avila-Reese, Vladimir and Firmani, Claudio and Boylan-Kolchin, Michael}, -doi = {10.1111/j.1365-2966.2012.22100.x}, -eprint = {1204.0516}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: interactions,Galaxies: structure}, -number = {2}, -pages = {1503--1516}, -title = {{The growth of galactic bulges through mergers in $\Lambda$ CDM haloes revisited - I. Present-day properties}}, -volume = {427}, -year = {2012} -} -@article{Roy:2018aa, -author = {Roy, N and Napolitano, N.$\sim$R. and {La Barbera}, F and Tortora, C and Getman, F and Radovich, M and Capaccioli, M and Brescia, M and Cavuoti, S and Longo, G and Raj, M.$\sim$A. and Puddu, E and Covone, G and Amaro, V and Vellucci, C and Grado, A and Kuijken, K and {Verdoes Kleijn}, G and Valentijn, E}, -journal = {\mnras}, -month = {oct}, -pages = {1057--1080}, -title = {{Evolution of galaxy size-stellar mass relation from the Kilo-Degree Survey}}, -volume = {480}, -year = {2018} -} -@article{Bentabol2016, -abstract = {We examine a sample of 1495 galaxies in the CANDELS fields to determine the evolution of two-component galaxies, including bulges and discs, within massive galaxies at the epoch 1 < z <3 when the Hubble sequence forms. We fit all of our galaxies' light profiles with a single S{\'{e}}rsic fit, as well as with a combination of exponential and S{\'{e}}rsic profiles. The latter is done in order to describe a galaxy with an inner and an outer component, or bulge and disc component. We develop and use three classification methods (visual, F-test and the residual flux fraction) to separate our sample into one-component galaxies (disc/spheroidslike galaxies) and two-component galaxies (galaxies formed by an 'inner part' or bulge and an 'outer part' or disc). We then compare the results from using these three different ways to classify our galaxies.We find that the fraction of galaxies selected as two-component galaxies increases on average 50 per cent from the lowest mass bin to the most massive galaxies, and decreases with redshift by a factor of 4 from z = 1 to 3. We find that single S{\'{e}}rsic 'disc-like' galaxies have the highest relative number densities at all redshifts, and that two-component galaxies have the greatest increase and become at par with S{\'{e}}rsic discs by z = 1. We also find that the systems we classify as two-component galaxies have an increase in the sizes of their outer components, or 'discs', by about a factor of 3 from z = 3 to 1.5, while the inner components or 'bulges' stay roughly the same size. This suggests that these systems are growing from the inside out, whilst the bulges or protobulges are in place early in the history of these galaxies. This is also seen to a lesser degree in the growth of single 'disc-like' galaxies versus 'spheroid-like' galaxies over the same epoch.}, -archivePrefix = {arXiv}, -arxivId = {1606.07405}, -author = {Margalef-Bentabol, Berta and Conselice, Christopher J. and Mortlock, Alice and Hartley, Will and Duncan, Kenneth and Ferguson, Harry C. and Dekel, Avishai and Primack, Joel R.}, -doi = {10.1093/mnras/stw1451}, -eprint = {1606.07405}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Margalef-Bentabol et al. - 2016 - The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z 3(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure}, -number = {3}, -pages = {1--21}, -title = {{The formation of bulges, discs and two-component galaxies in the CANDELS Survey at z < 3}}, -volume = {461}, -year = {2016} -} -@article{Wong2019, -abstract = {We present a measurement of the Hubble constant (H0) and other cosmological parameters from a joint analysis of six gravitationally lensed quasars with measured time delays. All lenses except the first are analyzed blindly with respect to the cosmological parameters. In a flat $\Lambda$CDM cosmology, we find $H_{0} = 73.3_{-1.8}^{+1.7}\sim\mathrm{km\sims^{-1}\simMpc^{-1}}$, a $2.4{{\ \rm per\ cent}}$ precision measurement, in agreement with local measurements of H0 from type Ia supernovae calibrated by the distance ladder, but in 3.1$\sigma$ tension with Planck observations of the cosmic microwave background (CMB). This method is completely independent of both the supernovae and CMB analyses. A combination of time-delay cosmography and the distance ladder results is in 5.3$\sigma$ tension with Planck CMB determinations of H0 in flat $\Lambda$CDM. We compute Bayes factors to verify that all lenses give statistically consistent results, showing that we are not underestimating our uncertainties and are able to control our systematics. We explore extensions to flat $\Lambda$CDM using constraints from time-delay cosmography alone, as well as combinations with other cosmological probes, including CMB observations from Planck, baryon acoustic oscillations, and type Ia supernovae. Time-delay cosmography improves the precision of the other probes, demonstrating the strong complementarity. Allowing for spatial curvature does not resolve the tension with Planck. Using the distance constraints from time-delay cosmography to anchor the type Ia supernova distance scale, we reduce the sensitivity of our H0 inference to cosmological model assumptions. For six different cosmological models, our combined inference on H0 ranges from ∼73–78 km s−1 Mpc−1, which is consistent with the local distance ladder constraints.}, -archivePrefix = {arXiv}, -arxivId = {1907.04869}, -author = {Wong, Kenneth C and Suyu, Sherry H and Chen, Geoff C-F and Rusu, Cristian E and Millon, Martin and Sluse, Dominique and Bonvin, Vivien and Fassnacht, Christopher D and Taubenberger, Stefan and Auger, Matthew W and Birrer, Simon and Chan, James H H and Courbin, Frederic and Hilbert, Stefan and Tihhonova, Olga and Treu, Tommaso and Agnello, Adriano and Ding, Xuheng and Jee, Inh and Komatsu, Eiichiro and Shajib, Anowar J and Sonnenfeld, Alessandro and Blandford, Roger D and Koopmans, L{\'{e}}on V E and Marshall, Philip J and Meylan, Georges}, -doi = {10.1093/mnras/stz3094}, -eprint = {1907.04869}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wong et al. - 2020 - H0LiCOW XIII. A 2.4% measurement of H0 from lensed quasars 5.3$\sigma$ tension between early and late-Universe probes.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {cosmological parameters,cosmology,dis-,gravitational lensing,observations,strong,tance scale}, -number = {November}, -title = {{H0LiCOW XIII. A 2.4% measurement of H0 from lensed quasars: 5.3$\sigma$ tension between early and late-Universe probes}}, -url = {http://arxiv.org/abs/1907.04869}, -year = {2020} -} -@article{Rudnick2006, -author = {Trujillo\, I and {\F\$\backslash$"o\rster Schreiber\}, N.\$\sim$M. and \Rudnick\, G and \Barden\, M and \Franx\, M and \Rix\, H.-W. and \Caldwell\, J.\$\sim$A.\$\sim$R. and \McIntosh\, D.\$\sim$H. and \Toft\, S and \H\$\backslash$"a\ussler\, B and \Zirm\, A and {\van Dokkum\}, P.\$\sim$G. and \Labb\$\backslash$'e\, L}, -title = {{{\textless}JiaoWen1.pdf{\textgreater}}}, -year = {2006} -} -@article{Agazie2023, -abstract = {The NANOGrav 15 yr data set shows evidence for the presence of a low-frequency gravitational-wave background (GWB). While many physical processes can source such low-frequency gravitational waves, here we analyze the signal as coming from a population of supermassive black hole (SMBH) binaries distributed throughout the Universe. We show that astrophysically motivated models of SMBH binary populations are able to reproduce both the amplitude and shape of the observed low-frequency gravitational-wave spectrum. While multiple model variations are able to reproduce the GWB spectrum at our current measurement precision, our results highlight the importance of accurately modeling binary evolution for producing realistic GWB spectra. Additionally, while reasonable parameters are able to reproduce the 15 yr observations, the implied GWB amplitude necessitates either a large number of parameters to be at the edges of expected values or a small number of parameters to be notably different from standard expectations. While we are not yet able to definitively establish the origin of the inferred GWB signal, the consistency of the signal with astrophysical expectations offers a tantalizing prospect for confirming that SMBH binaries are able to form, reach subparsec separations, and eventually coalesce. As the significance grows over time, higher-order features of the GWB spectrum will definitively determine the nature of the GWB and allow for novel constraints on SMBH populations.}, -archivePrefix = {arXiv}, -arxivId = {2306.16220}, -author = {Agazie, Gabriella and Anumarlapudi, Akash and Archibald, Anne M. and Baker, Paul T. and B{\'{e}}csy, Bence and Blecha, Laura and Bonilla, Alexander and Brazier, Adam and Brook, Paul R. and Burke-Spolaor, Sarah and Burnette, Rand and Case, Robin and Casey-Clyde, J. Andrew and Charisi, Maria and Chatterjee, Shami and Chatziioannou, Katerina and Cheeseboro, Belinda D. and Chen, Siyuan and Cohen, Tyler and Cordes, James M. and Cornish, Neil J. and Crawford, Fronefield and Cromartie, H. Thankful and Crowter, Kathryn and Cutler, Curt J. and D'Orazio, Daniel J. and DeCesar, Megan E. and DeGan, Dallas and Demorest, Paul B. and Deng, Heling and Dolch, Timothy and Drachler, Brendan and Ferrara, Elizabeth C. and Fiore, William and Fonseca, Emmanuel and Freedman, Gabriel E. and Gardiner, Emiko and Garver-Daniels, Nate and Gentile, Peter A. and Gersbach, Kyle A. and Glaser, Joseph and Good, Deborah C. and G{\"{u}}ltekin, Kayhan and Hazboun, Jeffrey S. and Hourihane, Sophie and Islo, Kristina and Jennings, Ross J. and Johnson, Aaron and Jones, Megan L. and Kaiser, Andrew R. and Kaplan, David L. and Kelley, Luke Zoltan and Kerr, Matthew and Key, Joey S. and Laal, Nima and Lam, Michael T. and Lamb, William G. and {W. Lazio}, T. Joseph and Lewandowska, Natalia and Littenberg, Tyson B. and Liu, Tingting and Luo, Jing and Lynch, Ryan S. and Ma, Chung-Pei and Madison, Dustin R. and McEwen, Alexander and McKee, James W. and McLaughlin, Maura A. and McMann, Natasha and Meyers, Bradley W. and Meyers, Patrick M. and Mingarelli, Chiara M. F. and Mitridate, Andrea and Natarajan, Priyamvada and Ng, Cherry and Nice, David J. and Ocker, Stella Koch and Olum, Ken D. and Pennucci, Timothy T. and Perera, Benetge B. P. and Petrov, Polina and Pol, Nihan S. and Radovan, Henri A. and Ransom, Scott M. and Ray, Paul S. and Romano, Joseph D. and Runnoe, Jessie C. and Sardesai, Shashwat C. and Schmiedekamp, Ann and Schmiedekamp, Carl and Schmitz, Kai and Schult, Levi and Shapiro-Albert, Brent J. and Siemens, Xavier and Simon, Joseph and Siwek, Magdalena S. and Stairs, Ingrid H. and Stinebring, Daniel R. and Stovall, Kevin and Sun, Jerry P. and Susobhanan, Abhimanyu and Swiggum, Joseph K. and Taylor, Jacob and Taylor, Stephen R. and Turner, Jacob E. and Unal, Caner and Vallisneri, Michele and Vigeland, Sarah J. and Wachter, Jeremy M. and Wahl, Haley M. and Wang, Qiaohong and Witt, Caitlin A. and Wright, David and Young, Olivia}, -doi = {10.3847/2041-8213/ace18b}, -eprint = {2306.16220}, -file = {:C\:/Users/Jammy/Documents/Papers/GWB/NANOGrav152024SMBHB.pdf:pdf}, -issn = {2041-8205}, -journal = {ApJ}, -number = {2}, -pages = {L37}, -title = {{The NANOGrav 15 yr Data Set: Constraints on Supermassive Black Hole Binaries from the Gravitational-wave Background}}, -volume = {952}, -year = {2023} -} -@article{Bullock2005, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print)$\backslash$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos I: Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Ding2019, -abstract = {Correlations between the mass of a supermassive black hole and the properties of its host galaxy (e.g., total stellar mass (M*), luminosity (Lhost)) suggest an evolutionary connection. A powerful test of a co-evolution scenario is to measure the relations MBH-Lhost and MBH-M* at high redshift and compare with local estimates. For this purpose, we acquired HST imaging with WFC3 of 32 X-ray-selected broad-line AGN at 1.2{\textless}z{\textless}1.7 in deep survey fields. By applying state-of-the-art tools to decompose the HST images including available ACS data, we measured the host galaxy luminosity and stellar mass along with other properties through the 2D model fitting. The black hole mass was determined using the broad Halpha line, detected in the near-infrared with Subaru/FMOS, which potentially minimizes systematic effects using other indicators. We find that the observed ratio of MBH to total M* is 2.7 times larger at z{\$\sim${}}1.5 than in the local universe, while the scatter is equivalent between the two epochs. A non-evolving mass ratio is consistent with the data at the 2-3 sigma confidence level when accounting for selection effects and their uncertainties. The relationship between MBH-Lhost paints a similar picture. Therefore, our results cannot distinguish whether SMBHs and their total M* and Lhost proceed in lockstep or whether the growth of the former somewhat overshoots the latter, given the uncertainties. Based on a statistical estimate of the bulge-to-total mass fraction, the ratio MBH/M* is offset from the local value by a factor of {\$\sim${}}7 which is significant even accounting for selection effects. Taken together, these observations are consistent with a scenario in which stellar mass is subsequently transferred from an angular momentum supported component of the galaxy to the pressure supported one through secular processes or minor mergers at a faster rate than mass accretion onto the SMBH.}, -archivePrefix = {arXiv}, -arxivId = {1910.11875}, -author = {Ding, Xuheng and Silverman, John and Treu, Tommaso and Schulze, Andreas and Schramm, Malte and Birrer, Simon and Park, Daeseong and Jahnke, Knud and Bennert, Vardha N and Kartaltepe, Jeyhan S and Koekemoer, Anton M and Malkan, Matthew A and Sanders, David}, -doi = {10.3847/1538-4357/ab5b90}, -eprint = {1910.11875}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {37}, -title = {{ The Mass Relations between Supermassive Black Holes and Their Host Galaxies at 1 {\textless} z {\textless} 2 with HST -WFC3 }}, -url = {http://arxiv.org/abs/1910.11875}, -volume = {888}, -year = {2020} -} -@article{Goulding2016a, -abstract = {Studies of the physical properties of local elliptical galaxies (e.g., gas temperatures, halo masses, stellar kinematics) are shedding new light on galaxy formation. Here we present the hot X-ray gas properties of 33 early-type systems within the MASSIVE galaxy survey sample that have archival Chandra X-ray observations. Through careful X-ray spectral modeling, we derive X-ray luminosities (L_X) and plasma temperatures (T_gas) for the diffuse gas components in these galaxies. We combine the MASSIVE sample with 41 galaxies from the ATLAS^3D survey to investigate the X-ray and optical properties of a statistically significant sample of nearby early-type galaxies across a wide-range of environments. We deduce that all early-type galaxies (independent of galaxy mass and rotational support) follow a universal scaling law such that L_X$\sim$T_gas^4.5. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, the wide-scale environment does not contribute to the intrinsic scatter ($\sim$0.5dex) within the scaling relation. We further demonstrate that the scatter in L_X around both K-band luminosity (L_K) and the galaxy stellar velocity dispersion is primarily driven by T_gas, with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the origin of the gas directly to either the stellar mass or the galaxy potential. Indeed, our data require a steeper relation between L_X, L_K, and sigma_e than predicted by standard mass-loss models. Finally, we find a statistically significant correlation between sigma_e and T_gas, suggesting that T_gas is set by the galaxy potential inside the optical effective radius. We conclude that within the inner-most 10-30kpc region, early-types maintain pressure-supported hot gas, with a minimum T_gas set by the virial temperature, but the majority show evidence for some additional heating.}, -archivePrefix = {arXiv}, -arxivId = {1604.01764}, -author = {Goulding, Andy D. and Greene, Jenny E. and Ma, Chung-Pei and Veale, Melanie and Bogdan, Akos and Nyland, Kristina and Blakeslee, John P. and McConnell, Nicholas J. and Thomas, Jens}, -doi = {10.3847/0004-637x/826/2/167}, -eprint = {1604.01764}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Goulding et al. - 2016 - the Massive Survey. Iv. the X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {167}, -title = {{the Massive Survey. Iv. the X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe}}, -url = {http://arxiv.org/abs/1604.01764%0Ahttp://dx.doi.org/10.3847/0004-637X/826/2/167}, -volume = {826}, -year = {2016} -} -@article{Hardy1998, -abstract = {We have performed detailed measurements of the charge transfer efficiency (CTE) in a thinned, backside-illuminated imaging charge-coupled device (CCD). The device had been damaged in three separate sections by proton radiation typical of that which a CCD would receive in space-borne experiments, nuclear imaging, or particle detection. We examined CTE as a function of signal level, temperature, and radiation dose. The dominant factor affecting the CTE in radiation-damaged CCD's is seen to be trapping by bulk states. We present a simple physical model for trapping as a function of transfer rate, trap concentration, and temperature. We have made calculations using this model and arrived at predictions which closely match the measured results. The CTE was also observed to have a nonlinear dependence on signal level. Using two-dimensional device simulations to examine the distribution of the charge packets in the CCD channel over a range of signal levels, we were able to explain the observed variation. {\textcopyright} 1998 IEEE.}, -author = {Hardy, T. and Murowinski, R. and Deen, M. J.}, -doi = {10.1109/23.664167}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {Ccd's,Charge transfer efficiency,Imaging detectors,Proton damage,Radiation}, -month = {apr}, -number = {2}, -pages = {154--163}, -title = {{Charge transfer efficiency in proton damaged CCD's}}, -volume = {45}, -year = {1998} -} -@article{Miller2007, -abstract = {The principles of measuring the shapes of galaxies by a model-fitting approach are discussed in the context of shape measurement for surveys of weak gravitational lensing. It is argued that such an approach should be optimal, allowing measurement with maximal signal-to-noise ratio, coupled with estimation of measurement errors. The distinction between likelihood-based and Bayesian methods is discussed. Systematic biases in the Bayesian method may be evaluated as part of the fitting process, and overall such an approach should yield unbiased shear estimation without requiring external calibration from simulations. The principal disadvantage of model fitting for large surveys is the computational time required, but here an algorithm is presented that enables large surveys to be analysed in feasible computation times. The method and algorithm is tested on simulated galaxies from the Shear TEsting Programme (STEP). {\textcopyright} 2007 The Authors.}, -archivePrefix = {arXiv}, -arxivId = {0708.2340}, -author = {Miller, L. and Kitching, T. D. and Heymans, C. and Heavens, A. F. and {Van Waerbeke}, L.}, -doi = {10.1111/j.1365-2966.2007.12363.x}, -eprint = {0708.2340}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Miller et al. - 2007 - Bayesian galaxy shape measurement for weak lensing surveys - I. Methodology and a fast-fitting algorithm.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Gravitational lensing,Methods: data analysis,Methods: statistical,Techniques: miscellaneous}, -number = {1}, -pages = {315--324}, -title = {{Bayesian galaxy shape measurement for weak lensing surveys - I. Methodology and a fast-fitting algorithm}}, -volume = {382}, -year = {2007} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful number of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag limit of ∼24. However, gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z ∼ 5-7 for LSST. We find that the LSST Wide Fast Deep survey could detect up to 120 lensed Population (Pop) I and II SNe but no lensed Pop III SNe. Deep-drilling programs in 10 deg2 fields could detect Pop I and II core-collapse SNe at AB magnitudes of 27-28 and 26, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes Erik and Whalen, Daniel J. and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S.}, -doi = {10.1093/mnras/stz3203}, -eprint = {1805.02662}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rydberg et al. - 2020 - Detecting strongly lensed supernovae at z ∼ 5-7 with LSST(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: dark ages,Cosmology: observations,First stars: early universe,Galaxies: high,Gravitational lensing: strong,Redshift,Reionization,Stars: Population III,Supernovae: general}, -number = {2}, -pages = {2447--2459}, -title = {{Detecting strongly lensed supernovae at z ∼ 5-7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {491}, -year = {2020} -} -@article{Genel2017, -abstract = {We analyse scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, star formation rate and redshift are reproduced, and a quantitative comparison of projected r band sizes at 0 ≲ z ≲ 2 shows agreement to much better than 0.25 dex. We follow populations of z = 0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M*, z = 0 ≳ 109.5 M⊙, the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z = 0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M*, M*, z = 0 ≳ 109.5 M⊙ experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies withM*, z = 0 ≳ 1011 M⊙, the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z = 0.}, -archivePrefix = {arXiv}, -arxivId = {1707.05327}, -author = {Genel, Shy and Nelson, Dylan and Pillepich, Annalisa and Springel, Volker and Pakmor, R{\"{u}}diger and Weinberger, Rainer and Hernquist, Lars and Naiman, Jill and Vogelsberger, Mark and Marinacci, Federico and Torrey, Paul}, -doi = {10.1093/mnras/stx3078}, -eprint = {1707.05327}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Genel et al. - 2018 - The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Galaxies: structure,Methods: numerical}, -number = {3}, -pages = {3976--3996}, -title = {{The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation}}, -url = {http://arxiv.org/abs/1707.05327}, -volume = {474}, -year = {2018} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work conducted to interpret this phenomenon has found that it is due to the non-spherical nature of dark matter halos. However, most studies overpredict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shapes of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations where satellite galaxies without associated subhalos ("orphan galaxies") are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region. {\textcopyright}2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W P and Kang, X and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%7B%5C%25%7D5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem%7B%5C&%7Dsid=IOPP%7B%5C%25%7D3Ajnl%7B%5C_%7Dref%7B%5C&%7Dspage=305%7B%5C&%7Dtitle=ArA%7B%5C&%7Dvolume=5%7B%5C&%7Ddate=1969%7B%5C&%7Dv%7B%5C}, -volume = {786}, -year = {2014} -} -@article{Buitrago2017a, -abstract = {Using the exquisite depth of the Hubble Ultra Deep Field (HUDF12 programme) data set, we explore the ongoing assembly of the outermost regions of the most massive galaxies (Mstellar ≥ 5× 1010 M) at z ≤ 1. The outskirts of massive objects, particularly early-type Galaxies (ETGs), are expected to suffer a dramatic transformation across cosmic time due to continuous accretion of small galaxies. HUDF imaging allows us to study this process at intermediate redshifts in six massive galaxies, exploring the individual surface brightness profiles out to ∼25 effective radii. We find that 5–20 per cent of the total stellar mass for the galaxies in our sample is contained within 10 < R < 50 kpc. These values are in close agreement with numerical simulations, and higher than those reported for local late-type galaxies (5 per cent). The fraction of stellar mass stored in the outer envelopes/haloes of massive ETGs increases with decreasing redshift, being 28.7 per cent at = 0.1, 15.1 per cent at = 0.65 and 3.5 per cent at = 2. The fraction of mass in diffuse features linked with ongoing minor merger events is >1–2 per cent, very similar to predictions based on observed close pair counts. Therefore, the results for our small albeit meaningful sample suggest that the size and mass growth of the most massive galaxies have been solely driven by minor and major merging from z = 1 to today.}, -archivePrefix = {arXiv}, -arxivId = {1602.01846}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Curtis-Lake, Emma and Montes, Mireia and Cooper, Andrew P. and Bruce, Victoria A. and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G. and Cirasuolo, Michele}, -doi = {10.1093/mnras/stw3382}, -eprint = {1602.01846}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buitrago et al. - 2017 - The cosmic assembly of stellar haloes in massive early-type Galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: haloes,Galaxies: high-redshift,Galaxies: structure}, -number = {4}, -pages = {4888--4903}, -title = {{The cosmic assembly of stellar haloes in massive early-type Galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3382}, -volume = {466}, -year = {2017} -} -@article{Alexander2019a, -abstract = {Strong gravitational lensing is a promising probe of the substructure of dark matter halos. Deep learning methods have the potential to accurately identify images containing substructure, and differentiate WIMP dark matter from other well motivated models, including vortex substructure of dark matter condensates and superfluids. This is crucial in future efforts to identify the true nature of dark matter. We implement, for the first time, a classification approach to identifying dark matter substructure based on simulated strong lensing images with different substructure. Utilizing convolutional neural networks trained on sets of simulated images, we demonstrate the feasibility of deep neural networks to reliably distinguish among different types of dark matter substructure. With thousands of strong lensing images anticipated with the coming launch of LSST, we expect that supervised and unsupervised deep learning models will play a crucial role in determining the nature of dark matter.}, -archivePrefix = {arXiv}, -arxivId = {1909.07346}, -author = {Alexander, Stephon and Gleyzer, Sergei and McDonough, Evan and Toomey, Michael W. and Usai, Emanuele}, -doi = {10.3847/1538-4357/ab7925}, -eprint = {1909.07346}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Alexander et al. - 2020 - Deep Learning the Morphology of Dark Matter Substructure.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {15}, -title = {{Deep Learning the Morphology of Dark Matter Substructure}}, -url = {http://arxiv.org/abs/1909.07346}, -volume = {893}, -year = {2020} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M>10^11 M_sun) galaxies at 1.72, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n<2) and spheroid-like (n>2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z$\sim$2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z>2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ($\sim$2x10^10 M_sun kpc^-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J. and Bouwens, Rychard J. and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buitrago et al. - 2008 - Size Evolution of the Most Massive Galaxies at 1.7 z 3 from GOODS NICMOS Survey Imaging.pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61--L64}, -title = {{ Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging }}, -url = {http://arxiv.org/abs/0807.4141%0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Xia2017, -abstract = {In this paper we use high-resolution cosmological simulations to study halo intrinsic alignment and its dependence on mass, formation time and large-scale environment. In agreement with previous studies using N-body simulations, it is found that massive halos have stronger alignment. For given mass, older halos have stronger alignment than younger ones. By identifying the cosmic environment of halo using Hessian matrix, we find that for given mass, halos in cluster regions also have stronger alignment than those in filament. The existing theory has not addressed these dependencies explicitly. In this work we extend the linear alignment model with inclusion of halo bias and find that the halo alignment with its mass and formation time dependence can be explained by halo bias. However, the model can not account for the environment dependence, as it is found that halo bias is lower in cluster and higher in filament. Our results suggest that halo bias and environment are independent factors in determining halo alignment. We also study the halo alignment correlation function and find that halos are strongly clustered along their major axes and less clustered along the minor axes. The correlated halo alignment can extend to scale as large as {\$}100h{\^{}}{\{}-1{\}}{\$}Mpc where its feature is mainly driven by the baryon acoustic oscillation effect.}, -archivePrefix = {arXiv}, -arxivId = {1706.07814}, -author = {Xia, Qianli and Kang, Xi and Wang, Peng and Luo, Yu and Yang, Xiaohu and Jing, Yipeng and Wang, Huiyuan and Mo, Houjun}, -doi = {10.3847/1538-4357/aa8d17}, -eprint = {1706.07814}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {22}, -title = {{Halo Intrinsic Alignment: Dependence on Mass, Formation Time, and Environment}}, -url = {http://arxiv.org/abs/1706.07814%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8d17}, -volume = {848}, -year = {2017} -} -@article{Geometryee, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(13).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Cautun2015, -abstract = {The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model ($\Lambda$ cold dark matter - $\Lambda$CDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of theMWand M31 planes in $\Lambda$CDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high-resolution cosmological simulations. We find that planar structures are very common, and that $\sim$10 per cent of $\Lambda$CDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small-scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and $\Lambda$CDM predictions. In fact, $\sim$10 per cent of $\Lambda$CDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1506.04151}, -author = {Cautun, Marius and Bose, Sownak and Frenk, Carlos S. and Guo, Qi and Han, Jiaxin and Hellwing, Wojciech A. and Sawala, Till and Wang, Wenting}, -doi = {10.1093/mnras/stv1557}, -eprint = {1506.04151}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cautun et al. - 2015 - Planes of satellite galaxies When exceptions are the rule(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {4}, -pages = {3838--3852}, -title = {{Planes of satellite galaxies: When exceptions are the rule}}, -volume = {452}, -year = {2015} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}$\backslash${\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashsigma{\$} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and {P{\'{e}}rez Gonz{\'{a}}lez}, Pablo G and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {112}, -title = {{ CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z ∼ 2 }}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -volume = {846}, -year = {2017} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashbackslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}{\$}\backslash{\$}{\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashbackslashsigma{\{}\backslash{\$}{\}} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and Gonzalez, Pablo G Perez and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -title = {{CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z{\$\sim${}}2}}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -year = {2017} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a $\Lambda$CDM concordance cosmology. To that extent we use a large N-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as a function of halo mass and galaxy colour. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by ∼40° (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the colour of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the colour of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion. {\textcopyright}2007 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X and {Van Den Bosch}, Frank C and Yang, Xiaohu and Mao, Shude and Mo, H J and Li, Cheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@article{Xia2017, -abstract = {In this paper we use high-resolution cosmological simulations to study halo intrinsic alignment and its dependence on mass, formation time and large-scale environment. In agreement with previous studies using N-body simulations, it is found that massive halos have stronger alignment. For given mass, older halos have stronger alignment than younger ones. By identifying the cosmic environment of halo using Hessian matrix, we find that for given mass, halos in cluster regions also have stronger alignment than those in filament. The existing theory has not addressed these dependencies explicitly. In this work we extend the linear alignment model with inclusion of halo bias and find that the halo alignment with its mass and formation time dependence can be explained by halo bias. However, the model can not account for the environment dependence, as it is found that halo bias is lower in cluster and higher in filament. Our results suggest that halo bias and environment are independent factors in determining halo alignment. We also study the halo alignment correlation function and find that halos are strongly clustered along their major axes and less clustered along the minor axes. The correlated halo alignment can extend to scale as large as {\$}100h{\^{}}{\{}-1{\}}{\$}Mpc where its feature is mainly driven by the baryon acoustic oscillation effect.}, -archivePrefix = {arXiv}, -arxivId = {1706.07814}, -author = {Xia, Qianli and Kang, Xi and Wang, Peng and Luo, Yu and Yang, Xiaohu and Jing, Yipeng and Wang, Huiyuan and Mo, Houjun}, -doi = {10.3847/1538-4357/aa8d17}, -eprint = {1706.07814}, -number = {2010}, -title = {{Halo intrinsic alignment: dependence on mass, formation time and environment}}, -url = {http://arxiv.org/abs/1706.07814%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8d17}, -year = {2017} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centres of typical {\$\sim${}} L* and lower mass spheroids exhibit power-law 'cusps' with $\Sigma$ $\alpha$ R-$\eta$, where 0.5 ≲ $\eta$ ≲ 1 for radii {\$\sim${}} 1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for, or strongly modify, the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m = 1 lopsided/eccentric disc instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*({\textless} R) « MBH. When the stellar surface density profile is comparatively shallow with $\eta$ {\textless} 1/2, the modes cannot efficiently propagate to R = 0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than $\eta$ = 1, the inward propagation of eccentricity is strongly damped, suppressing inflow and bringing $\eta$ down again. Together these results produce an equilibrium slope of 1/2 ≲ $\eta$ ≲ 1 in the potential of the central black hole. These physical arguments are supported by non-linear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies. {\textcopyright}2010 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Greco2017, -abstract = {We present a catalog of extended low-surface-brightness galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first {\$}{\{}\backslashsim{\}}{\$}200 deg{\$}{\^{}}2{\$} of the survey, we have uncovered 781 LSBGs, spanning red ({\$}g-i\backslashgeq0.64{\$}) and blue ({\$}g-i{\textless}0.64{\$}) colors and a wide range of morphologies. Since we focus on extended galaxies ({\$}r{\_}\backslashmathrm{\{}eff{\}}=2.5{\$}-{\$}14{\^{}}{\{}\backslashprime\backslashprime{\}}{\$}), our sample is likely dominated by low-redshift objects. We define LSBGs to have mean surface brightnesses {\$}\backslashbar{\{}\backslashmu{\}}{\_}\backslashmathrm{\{}eff{\}}(g){\textgreater}24.3{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, which allows nucleated galaxies into our sample. As a result, the central surface brightness distribution spans a wide range of {\$}\backslashmu{\_}0(g)=18{\$}-{\$}27.4{\$} mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, with 50{\%} and 95{\%} of galaxies fainter than 24.3 and 22 mag arcsec{\$}{\^{}}{\{}-2{\}}{\$}, respectively. Furthermore, the surface brightness distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well-characterized by single-component S$\backslash$'{\{}e{\}}rsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We crossmatch our sample with existing optical, HI, and ultraviolet catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, ranging from dwarf spheroidals and ultra-diffuse galaxies in nearby groups to gas-rich irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the LSBG population.}, -archivePrefix = {arXiv}, -arxivId = {1709.04474}, -author = {Greco, Johnny P and Greene, Jenny E and Strauss, Michael A and Macarthur, Lauren A and Flowers, Xzavier and Goulding, Andy D and Huang, Song and Kim, Ji Hoon and Komiyama, Yutaka and Leauthaud, Alexie and Leisman, Lukas and Lupton, Robert H and Sif{\'{o}}n, Crist{\'{o}}bal and Wang, Shiang-Yu}, -doi = {10.3847/1538-4357/aab842}, -eprint = {1709.04474}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {dwarf,galaxies,general,keywords}, -number = {2}, -pages = {104}, -title = {{Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey}}, -url = {http://arxiv.org/abs/1709.04474%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aab842}, -volume = {857}, -year = {2018} -} -@article{James2018, -abstract = {We present the first spatially resolved rest-frame ultraviolet (UV) study of the gravitationally lensed galaxy, the 'Cosmic Horseshoe' (J1148+1930) at z = 2.38. Our gravitational lens model shows that the system is made up of four star-forming regions, each {\$\sim${}}4-8 kpc2 in size, from which we extract four spatially exclusive regional spectra. We study the interstellar and wind absorption lines, along with C III] doublet emission lines, in each region to investigate any variation in emission/absorption line properties. Themapped C III] emission shows distinct kinematical structure, with velocity offsets of {\$\sim${}}±50 km s-1 between regions suggestive of a merging system, and a variation in equivalent width that indicates a change in ionization parameter and/or metallicity between the regions. Absorption line velocities reveal a range of outflow strengths, with gas outflowing in the range -200 ≲ v (km s-1) ≲ -50 relative to the systemic velocity of that region. Interestingly, the strongest gas outflow appears to emanate from the most diffuse star-forming region. The star formation rates remain relatively constant ({\$\sim${}}8-16M⊙ yr-1), mostly due to large uncertainties in reddening estimates. As such, the outflows appear to be 'global' rather than 'locally' sourced.We measure electron densities with a range of log (Ne)= 3.92-4.36 cm-3, and point out that such high densities may be common when measured using the CIII] doublet due to its large critical density. Overall, our observations demonstrate that while it is possible to trace variations in large-scale gas kinematics, detecting inhomogeneities in physical gas properties and their effects on the outflowing gas may be more difficult. This study provides important lessons for the spatially resolved rest-frame UV studies expected with future observatories, such as James Webb Space Telescope.}, -archivePrefix = {arXiv}, -arxivId = {1802.00455}, -author = {James, Bethan L and Auger, Matt and Pettini, Max and Stark, Daniel P and Belokurov, V and Carniani, Stefano}, -doi = {10.1093/mnras/sty315}, -eprint = {1802.00455}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/James et al. - 2018 - Mapping UV properties throughout the cosmic horseshoe Lessons from VLT-MUSE(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: star formation,Gravitational lensing: strong,Ultraviolet: galaxies}, -number = {2}, -pages = {1726--1740}, -title = {{Mapping UV properties throughout the cosmic horseshoe: Lessons from VLT-MUSE}}, -url = {http://arxiv.org/abs/1802.00455}, -volume = {476}, -year = {2018} -} -@article{Piontek2009, -abstract = {We present a systematic study of stellar feedback processes in simulations of disc galaxy formation. Using a dark matter halo with properties similar to the ones for the Milky Way's stellar halo, we perform a comparison of different methods of distributing energy related to feedback processes to the surrounding gas. A most promising standard model is applied to haloes spanning a range of masses in order to compare the results to disc galaxy scaling relations. With few exceptions we find little or no angular momentum deficiency for our galaxies and a good agreement with the angular momentum-size relation. Our galaxies are in good agreement with the baryonic Tully-Fisher relation and the slope of the photometric Tully-Fisher relation is reproduced. We find a zero-point offset of 0.7-1 mag, depending on the employed IMF. Applying the standard model to Milky Way-type haloes with different assembly histories, we show that a quiet assembly history does not guarantee the formation of a disc. We also study our standard feedback model in combination with additional physical processes like a UV background, kinetic feedback, a delayed energy deposition as expected for type Ia supernovae, mass return and metal-dependent cooling. Only a combination of effects yields a real improvement of the resulting galaxy by reducing the bulge, while including metal-dependent cooling increases the bulge again. We find that in general the stellar mass fraction of our galaxies is too high. In an ad hoc experiment we show that an removal of the bulge could reconcile this. However, the fit of the Tully-Fisher relation can only be improved by delaying the star formation, but not suppressing it completely. Our models do not seem to be efficient enough to achieve either effect. A mechanism to create bulge-less disc galaxies in simulations therefore remains elusive. We conclude that disc formation is a complex, highly interconnected problem that is difficult to handle in a controlled manner. We expect a solution to be coming from a combination of small effects rather than one large breakthrough. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0909.4167}, -author = {Piontek, Franziska and Steinmetz, Matthias}, -doi = {10.1111/j.1365-2966.2010.17637.x}, -eprint = {0909.4167}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: spiral,Galaxies: structure,Hydrodynamics,Methods: numerical}, -number = {4}, -pages = {2625--2642}, -title = {{The modelling of feedback processes in cosmological simulations of disc galaxy formation}}, -url = {http://arxiv.org/abs/0909.4156}, -volume = {410}, -year = {2011} -} -@article{Liao2024, -abstract = {In this study of the ‘Resolving supermAssive Black hole Binaries In galacTic hydrodynamical Simulations' (RABBITS) series, we investigate the orbital evolution of supermassive black holes (SMBHs) during galaxy mergers. We simulate both disc and elliptical galaxy mergers using the KETJU code, which can simultaneously follow galaxy (hydro-)dynamics and small-scale SMBH dynamics with post-Newtonian corrections. With our SMBH binary subgrid model, we show how active galactic nuclei (AGNs) feedback affects galaxy properties and SMBH coalescence. We find that simulations without AGN feedback exhibit excessive star formation, resulting in merger remnants that deviate from observed properties. Kinetic AGN feedback proves more effective than thermal AGN feedback in expelling gas from the centre and quenching star formation. The different central galaxy properties, which are a result of distinct AGN feedback models, lead to varying rates of SMBH orbital decay. In the dynamical friction phase, galaxies with higher star formation and higher SMBH masses possess denser centres, become more resistant to tidal stripping, experience greater dynamical friction, and consequently form SMBH binaries earlier. As AGN feedback reduces gas densities in the centres, dynamical friction by stars dominates over gas. In the SMBH hardening phase, compared to elliptical mergers, disc mergers exhibit higher central densities of newly formed stars, resulting in accelerated SMBH hardening and shorter merger time-scales (i.e. ≲ 500 Myr versus ≳ 1 Gyr). Our findings highlight the importance of AGN feedback and its numerical implementation in understanding the SMBH coalescing process, a key focus for low-frequency gravitational wave observatories.}, -archivePrefix = {arXiv}, -arxivId = {2311.01493}, -author = {Liao, Shihong and Irodotou, Dimitrios and Johansson, Peter H. and Naab, Thorsten and Rizzuto, Francesco Paolo and Hislop, Jessica M. and Wright, Ruby J. and Rawlings, Alexander}, -doi = {10.1093/mnras/stae1123}, -eprint = {2311.01493}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Liao2024RABBITS2.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cD,galaxies: disc,galaxies: elliptical and lenticular,galaxies: interactions,gravitational waves,methods: numerical,quasars: supermassive black holes}, -number = {4}, -pages = {4058--4081}, -title = {{RABBITS – II. The impact of AGN feedback on coalescing supermassive black holes in disc and elliptical galaxy mergers}}, -volume = {530}, -year = {2024} -} -@article{Aguero2016, -abstract = {We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75% of the hosts), with a bar (44% weak, 37% strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem not to be important for the appearance of CNRs, which appear to be more related to intrinsic properties of the host galaxies or to minor merger processes; 2) the proportion of weak bars in galaxies with a CNR is higher than expected; 3) the incidence of Seyfert (Sy) activity coeval with CNRs is significantly larger than the rate expected from the morphological distribution of the host galaxies; 4) the rate of Sy 2 to Sy 1 type galaxies with CNRs is about three times larger than the expected ratio for galaxies without CNRs and is opposite to that predicted by the geometric paradigm of the classical unified model for AGNs, although it does support the hypothesis that Sy 2 activity is linked to circumnuclear star formation. The possible selection effects of the sample are discussed, and we conclude that the detected trends are strong enough to justify high quality observations of as large as possible set of galaxies with circumnuclear rings and their matched control samples.}, -author = {Ag{\"{u}}ero, Mar{\'{i}}a P. and D{\'{i}}az, Rub{\'{e}}n J. and Dottori, Horacio}, -doi = {10.4236/ijaa.2016.63018}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ag{\"{u}}ero, D{\'{i}}az, Dottori - 2016 - Nuclear Activity in Circumnuclear Ring Galaxies(2).pdf:pdf}, -issn = {2161-4717}, -journal = {International Journal of Astronomy and Astrophysics}, -keywords = {active,dynamics,galaxies,nuclei,spiral,structure}, -number = {03}, -pages = {219--235}, -title = {{Nuclear Activity in Circumnuclear Ring Galaxies}}, -url = {http://www.scirp.org/journal/doi.aspx?DOI=10.4236/ijaa.2016.63018}, -volume = {06}, -year = {2016} -} -@article{Gavazzi2007, -abstract = {We present a weak gravitational lensing analysis of 22 early-type strong lens galaxies, based on deep HST images obtained as part of the Sloan Lens ACS Survey. Using the most advanced techniques to control systematic uncertainties related to the variable PSF and charge transfer efficiency of the ACS, we detect weak lensing signal out to 300 kpc/h. We analyze blank control fields from the COSMOS survey in the same manner, inferring that the residual systematic uncertainty in the tangential shear is <0.3%. A joint strong and weak lensing analysis shows that the average total mass density profile is consistent with isothermal over two decades in radius (3-300 kpc/h, approximately 1-100 Reff). This finding extends by over an order of magnitude in radius previous results, based on strong lensing and/or stellar dynamics, that luminous and dark component ``conspire'' to form an isothermal mass distribution. In order to disentangle the contributions of luminous and dark matter, we fit a two-component mass model (R^1/4 + NFW) to the weak and strong lensing constraints. It provides a good fit to the data with only two free parameters; i) the average stellar mass-to-light ratio M_*/L_V=4.48 +- 0.46 hMo/Lo, in agreement with that expected for an old stellar population; ii) the average virial mass-to-light ratio M_vir/L_V = 246+101-87 hMo/Lo. [abridged]}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701589}, -author = {Gavazzi, Raphael and Treu, Tommaso and Rhodes, Jason D. and Koopmans, Leon V. E. and Bolton, Adam S. and Burles, Scott and Massey, Richard J. and Moustakas, Leonidas A.}, -doi = {10.1086/519237}, -eprint = {0701589}, -isbn = {01944363}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Cosmology: Gravitational Lensing,Galaxies: Elliptical and Lenticular,Galaxies: Structure,cD}, -number = {1}, -pages = {176--190}, -pmid = {21924127}, -primaryClass = {astro-ph}, -title = {{The Sloan Lens ACS Survey. IV. The Mass Density Profile of Early‐Type Galaxies out to 100 Effective Radii}}, -url = {http://stacks.iop.org/0004-637X/667/i=1/a=176}, -volume = {667}, -year = {2007} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10{\^{}}11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r{\_}vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of {\$\sim${}}25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r{\_}vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of LCDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2004} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales (∼500 kpc) in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the virial radius of the haloes while describing the infalling matter via fluxes through a spherical shell; and we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP described for the first time in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one- and two-point statistics. The peripheral and advected momenta are correlated with the spin of the embedded halo at levels of 30 and 50 per cent. The infall takes place preferentially in the plane perpendicular to the direction defined by the spin of the halo. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be ∼15 per cent. The substructures have their spin orthogonal to their velocity vector in the rest frame of the halo at a level of about 5 per cent, suggestive of an image of a flow along filamentary structures, which provides an explanation for the measured anisotropy. Using a 'synthetic' stacked halo, it is shown that the positions and orientations of satellites relative to the direction of spin of the halo are not random even in projection. The average ellipticity of stacked haloes is 10 per cent, while the alignment excess in projection reaches 2 per cent. All measured correlations are fitted by a simple three-parameter model. We conclude that a halo does not see its environment as an Isotropic perturbation, we investigate how the anisotropy is propagated inwards using perturbation theory, and we discuss briefly the implications for weak lensing, warps and the thickness of galactic discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D. and Pichon, C. and Colombi, S.}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Aubert, Pichon, Colombi - 2004 - The origin and implications of dark matter anisotropic cosmic infall on ≈ L haloes.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Yang2019, -abstract = {Using the Atacama Large Millimeter/submillimeter Array (ALMA), we report high angular-resolution observations of the redshift z = 3.63 galaxy H-ATLAS J083051.0+013224 (G09v1.97), one of the most luminous strongly lensed galaxies discovered by the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). We present 0.″2-0.″4 resolution images of the rest-frame 188 and 419 $\mu$m dust continuum and the CO(6-5), H2O(211-202), and Jup = 2 H2O+ line emission. We also report the detection of H2O(211-202) in this source. The dust continuum and molecular gas emission are resolved into a nearly complete ∼1.″5 diameter Einstein ring plus a weaker image in the center, which is caused by a special dual deflector lensing configuration. The observed line profiles of the CO(6-5), H2O(211-202), and Jup = 2 H2O+ lines are strikingly similar. In the source plane, we reconstruct the dust continuum images and the spectral cubes of the CO, H2O, and H2O+ line emission at sub-kiloparsec scales. The reconstructed dust emission in the source plane is dominated by a compact disk with an effective radius of 0.7 ± 0.1 kpc plus an overlapping extended disk with a radius twice as large. While the average magnification for the dust continuum is $\mu$ ∼ 10-11, the magnification of the line emission varies from 5 to 22 across different velocity components. The line emission of CO(6-5), H2O(211-202), and H2O+ have similar spatial and kinematic distributions. The molecular gas and dust content reveal that G09v1.97 is a gas-rich major merger in its pre-coalescence phase, with a total molecular gas mass of ∼1011 M. Both of the merging companions are intrinsically ultra-luminous infrared galaxies (ULIRGs) with infrared luminosities LIR reaching 4 × 1012 L, and the total LIR of G09v1.97 is (1.4 ± 0.7)×1013 L. The approaching southern galaxy (dominating from V = -400 to -150 km s-1 relative to the systemic velocity) shows no obvious kinematic structure with a semi-major half-light radius of as = 0.4 kpc, while the receding galaxy (0 to 350 km s-1) resembles an as = 1.2 kpc rotating disk. The two galaxies are separated by a projected distance of 1.3 kpc, bridged by weak line emission (-150 to 0 km s-1) that is co-spatially located with the cold dust emission peak, suggesting a large amount of cold interstellar medium (ISM) in the interacting region. As one of the most luminous star-forming dusty high-redshift galaxies, G09v1.97 is an exceptional source for understanding the ISM in gas-rich starbursting major merging systems at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {1903.00273}, -author = {Yang, C. and Gavazzi, R. and Beelen, A. and Cox, P. and Omont, A. and Lehnert, M. D. and Gao, Y. and Ivison, R. J. and Swinbank, A. M. and Barcos-Mu{\~{n}}oz, L. and Neri, R. and Cooray, A. and Dye, S. and Eales, S. and Fu, H. and Gonz{\'{a}}lez-Alfonso, E. and Ibar, E. and Micha{\l}owski, M. J. and Nayyeri, H. and Negrello, M. and Nightingale, J. and P{\'{e}}rez-Fournon, I. and Riechers, D. A. and Smail, I. and {Van Der Werf}, P.}, -doi = {10.1051/0004-6361/201833876}, -eprint = {1903.00273}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Yang et al. - 2019 - CO, H2O, H2O line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales.pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: ISM,Galaxies: high-redshift,Gravitational lensing: strong,ISM: molecules,Radio lines: ISM,Submillimeter: galaxies}, -pages = {23--42}, -title = {{CO, H2O, H2O+ line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales}}, -url = {http://arxiv.org/abs/1903.00273}, -volume = {624}, -year = {2019} -} -@article{Pontzen2015a, -abstract = {Galaxies and the dark matter haloes that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealized calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter core-creation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are 'maximally stable', i.e. that do not evolve at first order when external potentials (which arise from baryons, large-scale tidal fields or infalling substructure) are applied. We show that a spherically symmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for near-isotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealized spherically symmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter haloes (formed in collisionless cosmological simulations) nearly attain our maximally stable limit, but their evolution freezes out before reaching it.}, -archivePrefix = {arXiv}, -arxivId = {1502.07356}, -author = {Pontzen, Andrew and Read, Justin I and Teyssier, Romain and Governato, Fabio and Gualandris, Alessia and Roth, Nina and Devriendt, Julien}, -doi = {10.1093/mnras/stv1032}, -eprint = {1502.07356}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {1366--1379}, -title = {{Milking the spherical cow - on aspherical dynamics in spherical coordinates}}, -volume = {451}, -year = {2015} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A and Birnboim, Y and Engel, G and Freundlich, J and Goerdt, T and Mumcuoglu, M and Neistein, E and Pichon, C and Teyssier, R and Zinger, E}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {https://ui.adsabs.harvard.edu/%7B%5C#%7Dabs/2009Natur.457..451D/abstract}, -volume = {457}, -year = {2009} -} -@article{Gonzalez2023, -abstract = {The new capabilities that JWST offers in the near- and mid-infrared (IR) are used to investigate in unprecedented detail the nature of optical/near-IR-faint, mid-IR-bright sources, with HST-dark galaxies among them. We gather JWST data from the CEERS survey in the Extended Groth Strip, jointly with HST data, and analyze spatially resolved optical-to-mid-IR spectral energy distributions to estimate photometric redshifts in two dimensions and stellar population properties on a pixel-by-pixel basis for red galaxies detected by NIRCam. We select 138 galaxies with F150W − F356W > 1.5 mag and F356W < 27.5 mag. The nature of these sources is threefold: (1) 71% are dusty star-forming galaxies (SFGs) at 2 < z < 6 with 9 < log M ⋆ / M ⊙ < 11 and a variety of specific SFRs (<1 to >100 Gyr −1 ); (2) 18% are quiescent/dormant (i.e., subject to reignition/rejuvenation) galaxies (QGs) at 3 < z < 5, with log M ⋆ / M ⊙ ∼ 10 and poststarburst mass-weighted ages (0.5–1.0 Gyr); and (3) 11% are strong young starbursts with indications of high equivalent width emission lines (typically, [O iii ]+H $\beta$ ) at 6 < z < 7 (XELG- z 6) and log M ⋆ / M ⊙ ∼ 9.5 . The sample is dominated by disk-like galaxies with remarkable compactness for XELG- z 6 (effective radii smaller than 0.4 kpc). Large attenuations in SFGs, 2 < A ( V ) < 5 mag, are found within 1.5 times the effective radius, approximately 2 kpc, while QGs present A ( V ) ∼ 0.2 mag. Our SED-fitting technique reproduces the expected dust emission luminosities of IR-bright and submillimeter galaxies. This study implies high levels of star formation activity between z ∼ 20 and z ∼ 10, where virtually 100% of our galaxies had already formed 10 8 M ⊙ , 60% had assembled 10 9 M ⊙ , and 10% up to 10 10 M ⊙ (in situ or ex situ).}, -archivePrefix = {arXiv}, -arxivId = {2211.00045}, -author = {P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G. and Barro, Guillermo and Annunziatella, Marianna and Costantin, Luca and Garc{\'{i}}a-Argum{\'{a}}nez, {\'{A}}ngela and McGrath, Elizabeth J. and M{\'{e}}rida, Rosa M. and Zavala, Jorge A and {Arrabal Haro}, Pablo and Bagley, Micaela B. and Backhaus, Bren E. and Behroozi, Peter and Bell, Eric F and Bisigello, Laura and Buat, V{\'{e}}ronique and Calabr{\`{o}}, Antonello and Casey, Caitlin M. and Cleri, Nikko J. and Coogan, Rosemary T. and Cooper, M. C. and Cooray, Asantha R. and Dekel, Avishai and Dickinson, Mark and Elbaz, David and Ferguson, Henry C. and Finkelstein, Steven L. and Fontana, Adriano and Franco, Maximilien and Gardner, Jonathan P. and Giavalisco, Mauro and G{\'{o}}mez-Guijarro, Carlos and Grazian, Andrea and Grogin, Norman A. and Guo, Yuchen and Huertas-Company, Marc and Jogee, Shardha and Kartaltepe, Jeyhan S. and Kewley, Lisa J. and Kirkpatrick, Allison and Kocevski, Dale D. and Koekemoer, Anton M. and Long, Arianna S. and Lotz, Jennifer M. and Lucas, Ray A. and Papovich, Casey and Pirzkal, Nor and Ravindranath, Swara and Somerville, Rachel S. and Tacchella, Sandro and Trump, Jonathan R. and Wang, Weichen and Wilkins, Stephen M. and Wuyts, Stijn and Yang, Guang and Yung, L. Y. Aaron}, -doi = {10.3847/2041-8213/acb3a5}, -eprint = {2211.00045}, -file = {:C\:/Users/Jammy/Documents/Papers/High_Redshift_galaxies/Gonzales2023HSTDarkCEERS.pdf:pdf}, -issn = {2041-8205}, -journal = {ApJL}, -number = {1}, -pages = {L16}, -title = {{CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies}}, -volume = {946}, -year = {2023} -} -@article{Hopkins2006, -abstract = {We present an evolutionary model for starbursts, quasars, and spheroidal galaxies in which mergers between gas-rich galaxies drive nuclear inflows of gas, producing starbursts and feeding the buried growth of supermassive black holes (BHs) until feedback expels gas and renders a briefly visible optical quasar. The quasar lifetime and obscuring column density depend on both the instantaneous and peak quasar luminosity, and we determine this dependence using a large set of galaxy merger simulations varying galaxy properties, orbital geometry, and gas physics. We use these fits to deconvolve observed quasar luminosity functions and obtain the evolution of the formation rate of quasars with peak luminosity, n dot(Lpeak,z). Quasars spend extended periods at luminosities well below peak, so n dot(Lpeak) has a maximum corresponding to the ``break'' in the observed luminosity function. From n dot(Lpeak) and our simulations, we obtain self-consistent hard and soft X-ray and optical luminosity functions and predict many observables at multiple redshifts, including column density distributions of optical and X-ray samples, the luminosity function of broad-line quasars in X-ray samples and broad-line fraction versus luminosity, active BH mass functions, the distribution of Eddington ratios, the mass function of relic BHs and total BH mass density, and the cosmic X-ray background. In every case, our predictions agree well with observed estimates, without invoking ad hoc assumptions about source properties or distributions. We provide a library of Monte Carlo realizations of our models for comparison with observations.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506398}, -author = {Hopkins, Philip F and Hernquist, Lars and Cox, Thomas J and {Di Matteo}, Tiziana and Robertson, Brant and Springel, Volker}, -doi = {10.1086/499298}, -eprint = {0506398}, -isbn = {doi:10.1086/499298}, -issn = {0067-0049}, -journal = {The Astrophysical Journal Supplement Series}, -number = {1}, -pages = {1--49}, -primaryClass = {astro-ph}, -title = {{A Unified, Merger‐driven Model of the Origin of Starbursts, Quasars, the Cosmic X‐Ray Background, Supermassive Black Holes, and Galaxy Spheroids}}, -url = {http://stacks.iop.org/0067-0049/163/i=1/a=1}, -volume = {163}, -year = {2006} -} -@article{Yan2016a, -abstract = {The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R{\$\sim${}}2000 from 3,622-10,354A. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is {\$\sim${}}73 per 1.4A pixel for spectra stacked between 1-1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals.}, -archivePrefix = {arXiv}, -arxivId = {1607.08613}, -author = {Yan, Renbin and Bundy, Kevin and Law, David R and Bershady, Matthew A and Andrews, Brett and Cherinka, Brian and Diamond-Stanic, Aleksandar M and Drory, Niv and MacDonald, Nicholas and S{\'{a}}nchez-Gallego, Jos{\'{e}} R and Thomas, Daniel and Wake, David A and Weijmans, Anne-Marie and Westfall, Kyle B and Zhang, Kai and Arag{\'{o}}n-Salamanca, Alfonso and Belfiore, Francesco and Bizyaev, Dmitry and Blanc, Guillermo A and Blanton, Michael R and Brownstein, Joel and Cappellari, Michele and D'Souza, Richard and Emsellem, Eric and Fu, Hai and Gaulme, Patrick and Graham, Mark T and Goddard, Daniel and Gunn, James E and Harding, Paul and Jones, Amy and Kinemuchi, Karen and Li, Cheng and Li, Hongyu and Maiolino, Roberto and Mao, Shude and Maraston, Claudia and Masters, Karen and Merrifield, Michael R and Oravetz, Daniel and Pan, Kaike and Parejko, John K and Sanchez, Sebastian F and Schlegel, David and Simmons, Audrey and Thanjavur, Karun and Tinker, Jeremy and Tremonti, Christy and van den Bosch, Remco and Zheng, Zheng}, -doi = {10.3847/0004-6256/152/6/197}, -eprint = {1607.08613}, -issn = {1538-3881}, -title = {{SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality}}, -url = {http://arxiv.org/abs/1607.08613%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-6256/152/6/197}, -volume = {197}, -year = {2016} -} -@article{Jiao2014, -abstract = {High-throughput sequencing allows the detection and quantification of frequencies of somatic single nucleotide variants (SNV) in heterogeneous tumor cell populations. In some cases, the evolutionary history and population frequency of the subclonal lineages of tumor cells present in the sample can be reconstructed from these SNV frequency measurements. However, automated methods to do this reconstruction are not available and the conditions under which reconstruction is possible have not been described. We describe the conditions under which the evolutionary history can be uniquely reconstructed from SNV frequencies from single or multiple samples from the tumor population and we introduce a new statistical model, PhyloSub, that infers the phylogeny and genotype of the major subclonal lineages represented in the population of cancer cells. It uses a Bayesian nonparametric prior over trees that groups SNVs into major subclonal lineages and automatically estimates the number of lineages and their ancestry. We sample from the joint posterior distribution over trees to identify evolutionary histories and cell population frequencies that have the highest probability of generating the observed SNV frequency data. When multiple phylogenies are consistent with a given set of SNV frequencies, PhyloSub represents the uncertainty in the tumor phylogeny using a partial order plot. Experiments on a simulated dataset and two real datasets comprising tumor samples from acute myeloid leukemia and chronic lymphocytic leukemia patients demonstrate that PhyloSub can infer both linear (or chain) and branching lineages and its inferences are in good agreement with ground truth, where it is available.}, -author = {Jiao, Wei and Vembu, Shankar and Deshwar, Amit G and Stein, Lincoln and Morris, Quaid}, -doi = {10.1186/1471-2105-15-35}, -issn = {14712105}, -journal = {BMC Bioinformatics}, -keywords = {PhyloSub}, -mendeley-tags = {PhyloSub}, -number = {1}, -title = {{Inferring clonal evolution of tumors from single nucleotide somatic mutations}}, -volume = {15}, -year = {2014} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://adsabs.harvard.edu/abs/2010ApJ...709.1138D}, -volume = {709}, -year = {2010} -} -@article{Herbert-Fort2007, -abstract = {We measure the distribution of velocities for prograde and retrograde satellite galaxies using a combination of published data and new observations for 78 satellites of 63 extremely isolated disc galaxies (169 satellites total). We find that the velocity distribution is non-Gaussian ({\textgreater}99.9{\%} confidence), but that it can be described as the sum of two Gaussians, one of which is broad (sigma = 176 pm 15 km/s), has a mean prograde velocity of 86 pm 30 km/s, and contains {\$\sim${}}55{\%} of the satellites, while the other is slightly retrograde with a mean velocity of -21 pm 22 km/s and sigma = 74 pm 18 km/s and contains {\$\sim${}}45{\%} of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher-level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Paykari2020, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1910.10521}, -author = {{Euclid Collaboration} and Paykari, P and Kitching, T and Hoekstra, H and Azzollini, R and Cardone, V.$\sim$F. and Cropper, M and Duncan, C.$\sim$A.$\sim$J. and Kannawadi, A and Miller, L and Aussel, H and Conti, I.$\sim$F. and Auricchio, N and Baldi, M and Bardelli, S and Biviano, A and Bonino, D and Borsato, E and Bozzo, E and Branchini, E and Brau-Nogue, S and Brescia, M and Brinchmann, J and Burigana, C and Camera, S and Capobianco, V and Carbone, C and Carretero, J and Castander, F.$\sim$J. and Castellano, M and Cavuoti, S and Charles, Y and Cledassou, R and Colodro-Conde, C and Congedo, G and Conselice, C and Conversi, L and Copin, Y and Coupon, J and Courtois, H.$\sim$M. and {Da Silva}, A and Dupac, X and Fabbian, G and Farrens, S and Ferreira, P.$\sim$G. and Fosalba, P and Fourmanoit, N and Frailis, M and Fumana, M and Galeotta, S and Garilli, B and Gillard, W and Gillis, B.$\sim$R. and Giocoli, C and Graci{\'{a}}-Carpio, J and Grupp, F and Hormuth, F and Ili{\'{c}}, S and Israel, H and Jahnke, K and Keihanen, E and Kermiche, S and Kilbinger, M and Kirkpatrick, C.$\sim$C. and Kubik, B and Kunz, M and Kurki-Suonio, H and Laureijs, R and {Le Mignant}, D and Ligori, S and Lilje, P.$\sim$B. and Lloro, I and Maciaszek, T and Maiorano, E and Marggraf, O and Markovic, K and Martinet, N and Marulli, F and Massey, R and Mauri, N and Medinaceli, E and Mei, S and Mellier, Y and Meneghetti, M and Metcalf, R.$\sim$B. and Moresco, M and Moscardini, L and Munari, E and Neissner, C and Nichol, R.$\sim$C. and Niemi, S and Nutma, T and Padilla, C and Paltani, S and Pasian, F and Pettorino, V and Pires, S and Polenta, G and Raison, F and Renzi, A and Rhodes, J and Romelli, E and Roncarelli, M and Rossetti, E and Saglia, R and Sakr, Z and S{\'{a}}nchez, A.$\sim$G. and Sapone, D and Scaramella, R and Schneider, P and Schrabback, T and Scottez, V and Secroun, A and Serrano, S and Sirignano, C and Sirri, G and Stanco, L and Starck, J -L. and Sureau, F and Tallada-Cresp\'\i, P and Taylor, A and Tenti, M and Tereno, I and Toledo-Moreo, R and Torradeflot, F and Valenziano, L and Vannier, M and Vassallo, T and Zoubian, J and Zucca, E}, -doi = {10.1051/0004-6361/201936980}, -eprint = {1910.10521}, -journal = {A\&A}, -keywords = {Astrophysics - Cosmology and Nongalactic Astrophys,gravitational lensing: weak}, -month = {mar}, -pages = {A139}, -primaryClass = {astro-ph.CO}, -title = {{Euclid preparation. VI. Verifying the performance of cosmic shear experiments}}, -volume = {635}, -year = {2020} -} -@article{Veale2016, -abstract = {We present spatially resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (ETGs; MK ≲ -25.7 mag, stellar mass M* ≳ 1011.8 M⊙) of the volumelimited (D < 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650-5850 {\AA} from the 246-fibre Mitchell integral-field spectrograph at McDonald Observatory, covering a 107 arcsec×107 arcsec field of view(often reaching 2 to 3 effective radii).We measure the 2D spatial distribution of each galaxy's angular momentum ($\lambda$ and fast or slow rotator status), velocity dispersion ($\sigma$), and higher order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ($\sim$80 per cent) of slow and non-rotators with $\lambda$ ≲ 0.2. When combined with the lower mass ETGs in the ATLAS3D survey, we find the fraction of slow rotators to increase dramatically with galaxy mass, reaching $\sim$50 per cent at MK $\sim$ -25.5 mag and $\sim$90 per cent at MK ≲ -26 mag. All of our fast rotators show a clear anticorrelation between h3 and V/$\sigma$, and the slope of the anticorrelation is steeper in more round galaxies. The radial profiles of s show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK ≲ -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat s profiles, whereas five of the seven 'isolated' galaxies are all fainter than MK = -25.8 mag and have falling $\sigma$. All of our galaxies have positive average h4; the most luminous galaxies have average h4 $\sim$ 0.05, while less luminous galaxies have a range of values between 0 and 0.05. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising s profiles. We discuss the implications for the relationship among dynamical mass, $\sigma$, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E. and McConnell, Nicholas J. and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P. and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Veale et al. - 2017 - The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Costantin2017, -abstract = {Context. The intrinsic shape of galactic bulges in nearby galaxies provides crucial information to separate bulge types. Aims. We aim to derive accurate constraints to the intrinsic shape of bulges to provide new clues on their formation mechanisms and set new limitations for future simulations. Methods. We retrieved the intrinsic shape of a sample of CALIFA bulges using a statistical approach. Taking advantage of GalMer numerical simulations of binary mergers we estimated the reliability of the procedure. Analyzing the i-band mock images of resulting lenticular remnants, we studied the intrinsic shape of their bulges at different galaxy inclinations. Finally, we introduced a new (B=A, C=A) diagram to analyze possible correlations between the intrinsic shape and the properties of bulges. Results. We tested the method on simulated lenticular remnants, finding that for galaxies with inclinations of 25° ≤ $\theta$ ≤ 65° we can safely derive the intrinsic shape of their bulges. We found that our CALIFA bulges tend to be nearly oblate systems (66%), with a smaller fraction of prolate spheroids (19%), and triaxial ellipsoids (15%). The majority of triaxial bulges are in barred galaxies (75%). Moreover, we found that bulges with low S{\'{e}}rsic indices or in galaxies with low bulge-to-total luminosity ratios form a heterogeneous class of objects; additionally, bulges in late-type galaxies or in less massive galaxies have no preference for being oblate, prolate, or triaxial. On the contrary, bulges with high S{\'{e}}rsic index, in early-type galaxies, or in more massive galaxies are mostly oblate systems. Conclusions. We concluded that various evolutionary pathways may coexist in galaxies, with merging events and dissipative collapse being the main mechanisms driving the formation of the most massive oblate bulges and bar evolution reshaping the less massive triaxial bulges.}, -archivePrefix = {arXiv}, -arxivId = {1710.05222}, -author = {Costantin, L. and M{\'{e}}ndez-Abreu, J. and Corsini, E. M. and Eliche-Moral, M. C. and Tapia, T. and Morelli, L. and Elena, Dalla Bont{\`{a}} and Pizzella, A.}, -doi = {10.1051/0004-6361/201731823}, -eprint = {1710.05222}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Costantin et al. - 2018 - The intrinsic shape of bulges in the CALIFA survey.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -pages = {1--17}, -title = {{The intrinsic shape of bulges in the CALIFA survey}}, -url = {http://arxiv.org/abs/1710.05222%0Ahttp://dx.doi.org/10.1051/0004-6361/201731823}, -volume = {609}, -year = {2018} -} -@article{Ikarashi2014, -author = {Ikarashi, Soh and Ivison, R. J. and Caputi, Karina I. and Aretxaga, Itziar and Dunlop, James S. and Hatsukade, Bunyo and Hughes, David H. and Iono, Daisuke and Izumi, Takuma and Kawabe, Ryohei and Kohno, Kotaro and Lagos, Claudia D. P. and Motohara, Kentaro and Nakanishi, Kouichiro and Ohta, Kouji and Tamura, Yoichi and Umehata, Hideki and Wilson, Grant W. and Yabe, Kiyoto and Yun, Min S.}, -doi = {10.1088/0004-637X/810/2/133}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {133}, -title = {{COMPACT STARBURSTS IN $z\sim 3$–6 SUBMILLIMETER GALAXIES REVEALED BY ALMA}}, -url = {http://stacks.iop.org/0004-637X/810/i=2/a=133?key=crossref.086f0a3643102b0606542cef2c0a73d3}, -volume = {810}, -year = {2015} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T < 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim & Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H. and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Massey2010d, -abstract = {Charge Transfer Inefficiency (CTI) due to radiation damage above the Earth's atmosphere creates spurious trailing in Hubble Space Telescope (HST) images. Radiation damage also creates unrelated warm pixels - but these happen to be perfect for measuring CTI. We model CTI in the Advanced Camera for Surveys (ACS)/Wide Field Channel and construct a physically motivated correction scheme. This operates on raw data, rather than secondary science products, by returning individual electrons to pixels from which they were unintentionally dragged during readout. We apply our correction to images from the HST Cosmic Evolution Survey (COSMOS), successfully reducing the CTI trails by a factor of ∼30 everywhere in the CCD and at all flux levels. We quantify changes in galaxy photometry, astrometry and shape. The remarkable 97 per cent level of correction is more than sufficient to enable a (forthcoming) reanalysis of downstream science products and the collection of larger surveys. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0909.0507}, -author = {Massey, Richard and Stoughton, Chris and Leauthaud, Alexie and Rhodes, Jason and Koekemoer, Anton and Ellis, Richard and Shaghoulian, Edgar}, -doi = {10.1111/j.1365-2966.2009.15638.x}, -eprint = {0909.0507}, -file = {:C\:/Users/Jammy/Documents/Papers/CTI/Massey2010PixelBased.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Instrumentation: detectors,Methods: data analysis,Space vehicles: instruments}, -number = {1}, -pages = {371--384}, -title = {{Pixel-based correction for charge transfer inefficiency in the hubble space telescope advanced camera for surveys}}, -volume = {401}, -year = {2010} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Dunlop2013, -abstract = {We use the new ultra-deep, near-infrared imaging of the Hubble Ultra-Deep Field (HUDF) provided by our UDF12 Hubble Space Telescope (HST)Wide Field Camera 3/IR campaign to explore the rest-frame ultraviolet (UV) properties of galaxies at redshifts z ≥ 6.5. We present the first unbiased measurement of the average UV power-law index, ($\beta$), (f$\lambda$ $\alpha$ $\lambda$$\beta$) for faint galaxies at z≃7, the first meaningful measurements of ($\beta$) at z≃8, and tentative estimates for a new sample of galaxies at z≃9. Utilizing galaxy selection in the new F140W (J140) imaging to minimize colour bias, and applying both colour and power-law estimators of $\beta$, we find ($\beta$)= -2.1 ± 0.2 at z ≃7 for galaxies with MUV ≃-18. This means that the faintest galaxies uncovered at this epoch have, on average, UV colours no more extreme than those displayed by the bluest star-forming galaxies at low redshift. At z ≃ 8 we find a similar value, ($\beta$)= -1.9± 0.3. At z ≃ 9, we find ($\beta$)= -1.8± 0.6, essentially unchanged from z ≃ 6 to 7 (albeit highly uncertain). Finally, we show that there is as yet no evidence for a significant intrinsic scatter in $\beta$ within our new, robust z ≃ 7 galaxy sample. Our results are most easily explained by a population of steadily star-forming galaxies with either ≃ solar metallicity and zero dust, or moderately sub-solar (≃10-20 per cent) metallicity with modest dust obscuration (AV ≃ 0.1-0.2). This latter interpretation is consistent with the predictions of a state-of-the-art galaxy-formation simulation, which also suggests that a significant population of very-low metallicity, dust-free galaxies with $\beta$ ≃ -2.5 may not emerge until MUV > -16, a regime likely to remain inaccessible until the James Webb Space Telescope. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1212.0860}, -author = {Dunlop, J. S. and Rogers, A. B. and McLure, R. J. and Ellis, R. S. and Robertson, B. E. and Koekemoer, A. and Dayal, P. and Curtis-Lake, E. and Wild, V. and Charlot, S. and Bowler, R. A.A. and Schenker, M. A. and Ouchi, M. and Ono, Y. and Cirasuolo, M. and Furlanetto, S. R. and Stark, D. P. and Targett, T. A. and Schneider, E.}, -doi = {10.1093/mnras/stt702}, -eprint = {1212.0860}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dunlop et al. - 2013 - The UV continua and inferred stellar populations of galaxies at z≃7-9 revealed by the Hubble Ultra-Deep Field 201.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Evolution-galaxies,First stars,Formation-galaxies,Galaxies,High-redshift-galaxies,Reionization,Stellar content-dark ages}, -number = {4}, -pages = {3520--3533}, -title = {{The UV continua and inferred stellar populations of galaxies at z≃7-9 revealed by the Hubble Ultra-Deep Field 2012 campaign}}, -volume = {432}, -year = {2013} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L. Gabriel and Arg{\"{u}}elles, C. R. and Perlick, Volker and Rueda, J. A. and Ruffini, R.}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/G{\'{o}}mez et al. - 2016 - Strong lensing by fermionic dark matter in galaxies(2).pdf:pdf}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Birrer2018, -abstract = {We present a blind time-delay strong lensing (TDSL) cosmographic analysis of the doubly imaged quasar SDSS 1206+4332. We combine the relative time delay between the quasar images, Hubble Space Telescope imaging, the Keck stellar velocity dispersion of the lensing galaxy, and wide-field photometric and spectroscopic data of the field to constrain two angular diameter distance relations. The combined analysis is performed by forward modelling the individual data sets through a Bayesian hierarchical framework, and it is kept blind until the very end to prevent experimenter bias. After unblinding, the inferred distances imply a Hubble constant H 0 = 68.8 +5.4-5.1 km s '1 Mpc '1, assuming a flat cold dark matter cosmology with uniform prior on m in [0.05, 0.5]. The precision of our cosmographic measurement with the doubly imaged quasar SDSS 1206+4332 is comparable with those of quadruply imaged quasars and opens the path to perform on selected doubles the same analysis as anticipated for quads. Our analysis is based on a completely independent lensing code than our previous three H0LiCOW systems and the new measurement is fully consistent with those. We provide the analysis scripts paired with the publicly available software to facilitate independent analysis (footnote with link to www.h0licow.org). The consistency between blind measurements with independent codes provides an important sanity check on lens modelling systematics. By combining the likelihoods of the four systems under the same prior, we obtain H 0 = 72.5 +2.1-2.3 km s '1 Mpc '1. This measurement is independent of the distance ladder and other cosmological probes.}, -archivePrefix = {arXiv}, -arxivId = {1809.01274}, -author = {Birrer, S and Treu, T and Rusu, C E and Bonvin, V and Fassnacht, C D and Chan, J H H and Agnello, A and Shajib, A J and Chen, G C F and Auger, M and Courbin, F and Hilbert, S and Sluse, D and Suyu, S H and Wong, K C and Marshall, P and Lemaux, B C and Meylan, G}, -doi = {10.1093/mnras/stz200}, -eprint = {1809.01274}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmological parameters,dark energy,ravitational lensing: strong}, -number = {4}, -pages = {4726--4753}, -title = {{H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant}}, -url = {http://arxiv.org/abs/1809.01274}, -volume = {484}, -year = {2019} -} -@article{Handley2015, -abstract = {PolyChord is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of PolyChord v1.3, and provides an extensive account of the algorithm. PolyChord utilises slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelised using openMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in CosmoMC and CAMB, and is now in use in the CosmoChord and ModeChord codes. PolyChord is available for download at: http://ccpforge.cse.rl.ac.uk/gf/project/polychord/}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Sirianni2004, -abstract = {The Advanced Camera for Surveys (ACS), installed in the Hubble Space Telescope (HST) in March 2002, comprises three cameras: the Wide Field Camera (WFC), designed for deep near-IR survey imaging programs; the High Resolution Camera (HRC), a high angular resolution imager which fully samples the HST full spread function (PSF) in the visible; and the Solar Blind Camera (SBC), a far-UV imager. The WFC and HRC employ CCD detectors. Their performances are affected by the on-going damage due to the space radiation environment where they operate. We present an overview of the performance of the ACS CCD detectors, based on the first two years of flight science operations. We analyze the evolution with time of the basic detector performance that are subjected to degradation due to the on-going radiation damage. Comparison is made with ground testing prediction and with the amount of performance degradation seen in other CCD detectors on board of HST.}, -author = {Sirianni, Marco and Mutchler, Max and Clampin, Mark and Ford, Holland and Illingworth, Garth and Hartig, George and van Orsow, Doug and Wheeler, Thomas}, -doi = {10.1117/12.552584}, -issn = {0277786X}, -journal = {Optical and Infrared Detectors for Astronomy}, -number = {January 2014}, -pages = {173}, -title = {{Performance of the Advanced Camera for Surveys CCDs after two years on orbit}}, -volume = {5499}, -year = {2004} -} -@article{Bower:2016aa, -author = {Bower, R and Schaye, J and Frenk, C.$\sim$S. and Theuns, T and Schaller, M and Crain, R.$\sim$A. and McAlpine, S}, -journal = {ArXiv e-prints}, -month = {jul}, -title = {{The dark nemesis of galaxy formation: why hot haloes trigger black hole growth and bring star formation to an end}}, -year = {2016} -} -@article{Oguri2010, -abstract = {Cadenced optical imaging surveys in the next decade will be capable of detecting time-varying galaxy-scale strong gravitational lenses in large numbers, increasing the size of the statistically well-defined samples of multiply imaged quasars by two orders of magnitude, and discovering the first strongly lensed supernovae. We carry out a detailed calculation of the likely yields of several planned surveys, using realistic distributions for the lens and source properties and taking magnification bias and image configuration detectability into account. We find that upcoming wide-field synoptic surveys should detect several thousand lensed quasars. In particular, the Large Synoptic Survey Telescope (LSST) should find more than some 8000 lensed quasars, some 3000 of which will have well-measured time delays. The LSST should also find some 130 lensed supernovae during the 10-yr survey duration, which is compared with ∼15 lensed supernovae predicted to be found by a deep, space-based supernova survey done by the Joint Dark Energy Mission. We compute the quad fraction in each survey, predicting it to be ∼15 per cent for the lensed quasars and ∼30 per cent for the lensed supernovae. Generating a mock catalogue of around 1500 well-observed double-image lenses, as could be derived from the LSST survey, we compute the available precision on the Hubble constant and the dark energy equation parameters for the time-delay distance experiment (assuming priors from Planck): the predicted marginalized 68 per cent confidence intervals are $\sigma$(w0) = 0.15, $\sigma$(wa) = 0.41 and $\sigma$(h) = 0.017. While this is encouraging in the sense that these uncertainties are only 50 per cent larger than those predicted for a space-based Type Ia supernova sample, we show how the dark energy figure of merit degrades with decreasing knowledge of the lens mass distribution. {\textcopyright} 2010 The Authors. Journal compilation {\textcopyright} 2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1001.2037}, -author = {Oguri, Masamune and Marshall, Philip J.}, -doi = {10.1111/j.1365-2966.2010.16639.x}, -eprint = {1001.2037}, -isbn = {0769538010}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Cosmology: theory,Gravitational lensing: strong}, -number = {4}, -pages = {2579--2593}, -title = {{Gravitationally lensed quasars and supernovae in future wide-field optical imaging surveys}}, -volume = {405}, -year = {2010} -} -@article{Kotilainen2018, -abstract = {Recently, the relation between the masses of the black hole (MBH) and the host galaxy (Mhost) in quasars has been probed down to the parameter space ofMBH {\$\sim${}} 108M⊙ and Mhost {\$\sim${}} 1011M⊙ at z {\textless} 0.5. In this study, we have investigated the MBH-Mhost log-linear relation for a sample of 37 quasars with low black hole masses (107M⊙ {\textless} MBH {\textless} 108.3M⊙) at 0.5 {\textless} z {\textless} 1.0. The black hole masses were derived using virial mass estimates from Sloan Digital Sky Survey (SDSS) optical spectra. For 25 quasars, we detected the presence of the host galaxy from deep near-infraredH-band imaging, whereas upper limits for the host galaxy luminosity (mass) were estimated for the 12 unresolved quasars. We combined our previous studies with the results from this work to create a sample of 89 quasars at z {\textless} 1.0 having a large range of black hole masses (107M⊙ {\textless} MBH {\textless} 1010M⊙) and host galaxy masses (1010M⊙ {\textless} Mhost {\textless} 1013M⊙). Most of the quasars at the low-mass end lie below the extrapolation of the local relation. This apparent break in the linearity of the entire sample is due to increasing fraction of discdominated host galaxies in the low-mass quasars. After correcting for the disc component, and considering only the bulge component, the bilinear regression for the entire quasar sample holds over 3.5 dex in both the black hole mass and the bulge mass, and is in very good agreement with the local relation. We advocate secular evolution of discs of galaxies being responsible for the relatively strong disc domination.}, -archivePrefix = {arXiv}, -arxivId = {1409.1948}, -author = {Sanghvi, J and Kotilainen, J K and Falomo, R and Decarli, R and Karhunen, K and Uslenghi, M}, -doi = {10.1093/mnras/stu1822}, -eprint = {1409.1948}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: high-redshift,Galaxies: nuclei,Quasars: general}, -number = {2}, -pages = {1261--1268}, -title = {{The black hole-host galaxy relation for very low mass quasars}}, -volume = {445}, -year = {2014} -} -@article{Hoekstra2004, -abstract = {We present the results of a study of weak lensing by galaxies based on 45.5 deg{\$}{\^{}}2{\$} of {\$}R{\_}C{\$} band imaging data from the Red-Sequence Cluster Survey (RCS). We present the first weak lensing detection of the flattening of galaxy dark matter halos. We use a simple model in which the ellipticity of the halo is {\$}f{\$} times the observed ellipticity of the lens. We find a best fit value of {\$}f=0.77{\^{}}{\{}+0.18{\}}{\_}{\{}-0.21{\}}{\$}, suggesting that the dark matter halos are somewhat rounder than the light distribution. The fact that we detect a significant flattening implies that the halos are well aligned with the light distribution. Given the average ellipticity of the lenses, this implies a halo ellipticity of {\$}{\textless}e{\_}{\{}\backslashrm halo{\}} {\textgreater}=0.33{\^{}}{\{}+0.07{\}}{\_}{\{}-0.09{\}}{\$}, in fair agreement with results from numerical simulations of CDM. This result provides strong support for the existence of dark matter, as an isotropic lensing signal is excluded with 99.5{\%} confidence. We also study the average mass profile around the lenses, using a maximum likelihood analysis. We consider two models for the halo mass profile: a truncated isothermal sphere (TIS) and an NFW profile. We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo. The best fit NFW model yields a mass {\$}M{\_}{\{}200{\}}=(8.4\backslashpm0.7\backslashpm0.4)\backslashtimes 10{\^{}}{\{}11{\}} h{\^{}}{\{}-1{\}} M{\_}\backslashodot{\$} and a scale radius {\$}r{\_}s=16.2{\^{}}{\{}+3.6{\}}{\_}{\{}-2.9{\}} h{\^{}}{\{}-1{\}}{\$} kpc. This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, H K C and Gladders, Michael D}, -doi = {10.1086/382726}, -eprint = {0306515}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of Galaxy Dark Matter Halos from Weak Lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2004} -} -@article{Xie2014, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stu2487}, -volume = {447}, -year = {2015} -} -@article{Maresca2021, -abstract = {With the advent of next-generation surveys and the expectation of discovering huge numbers of strong gravitational lens systems, much effort is being invested into developing automated procedures for handling the data. The several orders of magnitude increase in the number of strong galaxy–galaxy lens systems is an insurmountable challenge for traditional modelling techniques. Whilst machine learning techniques have dramatically improved the efficiency of lens modelling, parametric modelling of the lens mass profile remains an important tool for dealing with complex lensing systems. In particular, source reconstruction methods are necessary to cope with the irregular structure of high-redshift sources. In this paper, we consider a convolutional neural network (CNN) that analyses the outputs of semi-analytic methods that parametrically model the lens mass and linearly reconstruct the source surface brightness distribution. We show the unphysical source reconstructions that arise as a result of incorrectly initialized lens models can be effectively caught by our CNN. Furthermore, the CNN predictions can be used to automatically reinitialize the parametric lens model, avoiding unphysical source reconstructions. The CNN, trained on reconstructions of lensed S{\'{e}}rsic sources, accurately classifies source reconstructions of the same type with a precision P > 0.99 and recall R > 0.99. The same CNN, without retraining, achieves P = 0.89 and R = 0.89 when classifying source reconstructions of more complex lensed Hubble Ultra-Deep Field (HUDF) sources. Using the CNN predictions to reinitialize the lens modelling procedure, we achieve a 69 per cent decrease in the occurrence of unphysical source reconstructions. This combined CNN and parametric modelling approach can greatly improve the automation of lens modelling.}, -archivePrefix = {arXiv}, -arxivId = {2012.04665}, -author = {Maresca, Jacob and Dye, Simon and Li, Nan}, -doi = {10.1093/mnras/stab387}, -eprint = {2012.04665}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Maresca2021Unphysical.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {galaxies,gravitational lensing,strong,structure}, -number = {2}, -pages = {2229--2241}, -title = {{Auto-identification of unphysical source reconstructions in strong gravitational lens modelling}}, -volume = {503}, -year = {2021} -} -@article{Goerdt2010, -abstract = {We perform a detailed investigation into the disruption of central cusps via the transfer of energy from sinking massive objects. Constant density inner regions form at the radius where the enclosed mass approximately matches the mass of the infalling body. We explore parameter space using numerical simulations and give an empirical relation for the size of the resulting core within structures that have different initial cusp slopes. We find that infalling bodies always stall at the edge of these newly formed cores, experiencing no dynamical friction over many dynamical times. As applications, we consider the resulting decrease in the dark matter annihilation flux due to centrally destroyed cusps, and we present a new theory for the formation of close binary nuclei-the "stalled binary" model.We focus on one particularly interesting binary nucleus system, the dwarf spheroidal galaxy VCC 128 which is darkmatter dominated at all radii.We showthat its nucleiwould rapidly coalesce within a fewmillion years if it has a central dark matter cusp slope steeper than r-1. However, if its initial dark matter cusp is slightly shallower than a logslope of-0.75 at∼0.1% of the virial radius, then the sinking nuclei naturally create a core equal to their observed separation and stall. This is close to the logslope measured in a recent billion particle cold darkmatter halo simulation. {\textcopyright} 2010. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0806.1951}, -author = {Goerdt, Tobias and Moore, Ben and Read, J. I. and Stadel, Joachim}, -doi = {10.1088/0004-637X/725/2/1707}, -eprint = {0806.1951}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Cosmology: theory,Dark matter,Galaxies: dwarf,Galaxies: individual (VCC 128),Methods: numerical}, -month = {dec}, -number = {2}, -pages = {1707--1716}, -title = {{Core creation in galaxies and halos via sinking massive objects}}, -url = {http://stacks.iop.org/0004-637X/725/i=2/a=1707?key=crossref.f1a39f421687694dc69519d38297f745}, -volume = {725}, -year = {2010} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T < 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim & Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H. and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Baugh:1996aa, -author = {Baugh, C.$\sim$M. and Cole, S and Frenk, C.$\sim$S.}, -journal = {\mnras}, -month = {dec}, -pages = {1361--1378}, -title = {{Evolution of the Hubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{Einstein1916, -abstract = {Not Available}, -author = {Lorentz, H. A. and Einstein, A. and Minkowski, H. and Einstein, A.}, -doi = {10.1007/978-3-663-19510-8_7}, -isbn = {1521-3889}, -issn = {15213889}, -journal = {Das Relativit{\"{a}}tsprinzip}, -number = {7}, -pages = {81--124}, -pmid = {168842}, -title = {{Die Grundlage der allgemeinen Relativit{\"{a}}tstheorie}}, -volume = {354}, -year = {1923} -} -@article{Greene2017b, -abstract = {The "kinematic" morphology-density relation for early-type galaxies posits that those galaxies with low angular momentum are preferentially found in the highest-density regions of the universe. We use a large sample of galaxy groups with halo masses 10^12.5 < M_halo < 10^14.5 M_sun/h observed with the Mapping Nearby Galaxies at APO (MaNGA) survey to examine whether there is a correlation between local environment and rotational support that is independent of stellar mass. We find no compelling evidence for a relationship between the angular momentum content of early-type galaxies and either local overdensity or radial position within the group at fixed stellar mass.}, -archivePrefix = {arXiv}, -arxivId = {1708.07843}, -author = {Greene, J. E. and Leauthaud, A. and Emsellem, E. and Goddard, D. and Ge, J. and Andrews, B. H. and Brinkman, J. and Brownstein, J. R. and Greco, J. and Law, D. and Lin, Y.-T. and Masters, K. L. and Merrifield, M. and More, S. and Okabe, N. and Schneider, D. P. and Thomas, D. and Wake, D. A. and Yan, R. and Drory, N.}, -doi = {10.3847/2041-8213/aa8ace}, -eprint = {1708.07843}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2017 - SDSS-IV MaNGA Probing the Kinematic Morphology–Density Relation of Early-type Galaxies with MaNGA.pdf:pdf}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L33}, -title = {{SDSS-IV MaNGA: Probing the Kinematic Morphology–Density Relation of Early-type Galaxies with MaNGA}}, -url = {http://arxiv.org/abs/1708.07843%0Ahttp://dx.doi.org/10.3847/2041-8213/aa8ace}, -volume = {851}, -year = {2017} -} -@article{Bruce2014b, -abstract = {We have constructed a mass-selected sample of M{\textless}inf{\textgreater}*{\textless}/inf{\textgreater} {\textgreater} 10{\textless}sup{\textgreater}11{\textless}/sup{\textgreater}M{\textless}inf{\textgreater}⊙{\textless}/inf{\textgreater} galaxies at 1 {\textless} z {\textless} 3 in the CANDELS UKIDSS UDS and COSMOS fields and have decomposed these systems into their separate bulge and disc components according to their H160-band morphologies. By extending this analysis to multiple bands, we have been able to conduct individual bulge and disc component SED fitting which has provided us with stellar-mass and star formation rate estimates for the separate bulge and disc components. Having utilized the new decomposed stellar-mass estimates, we confirm that the bulge components display a stronger size evolution than the discs. The median sizes of the bulge components is 3.09 ± 0.20 times smaller than similarly massive local galaxies over the full 1 {\textless} z {\textless} 3 redshift range; for the discs, the corresponding factor is 1.77 ± 0.10. Moreover, by splitting our sample into the passive and star-forming bulge and disc sub-populations and examining their sizes as a fraction of their present-day counter-parts, we find that the star-forming and passive bulges are equally compact, star-forming discs are larger, while the passive discs have intermediate sizes. This trend is not evident when classifying galaxy morphology on the basis of single-S{\'{e}}rsic fits and adopting the overall star formation rates. Finally, by evolving the star formation histories of the passive discs back to the redshifts when the passive discs were last active, we show that the passive and star-forming discs have consistent sizes at the relevant epoch. These trends need to be reproduced by any mechanisms which attempt to explain the morphological evolution of galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1405.5221}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1537}, -eprint = {1405.5221}, -isbn = {0035-8711}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -number = {2}, -pages = {1660--1673}, -title = {{The decomposed bulge and disc size-mass relations of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -url = {http://arxiv.org/abs/1405.5221}, -volume = {444}, -year = {2014} -} -@article{Birrer2018a, -abstract = {We present lenstronomy, a multi-purpose open-source gravitational lens modelling pythonpackage. lenstronomy is able to reconstruct the lens mass and surface brightness distributions of strong lensing systems using forward modelling. lenstronomy supports a wide range of analytic lens and light models in arbitrary combination. The software is also able to reconstruct complex extended sources (Birrer et. al 2015) as well as being able to model point sources. We designed lenstronomy to be stable, flexible and numerically accurate, with a clear user interface that could be deployed across different platforms. Throughout its development, we have actively used lenstronomy to make several measurements including deriving constraints on dark matter properties in strong lenses, measuring the expansion history of the universe with time-delay cosmography, measuring cosmic shear with Einstein rings and decomposing quasar and host galaxy light. The software is distributed under the MIT license. The documentation, starter guide, example notebooks, source code and installation guidelines can be found at https://lenstronomy.readthedocs.io.}, -archivePrefix = {arXiv}, -arxivId = {1803.09746}, -author = {Birrer, Simon and Amara, Adam}, -doi = {10.1016/j.dark.2018.11.002}, -eprint = {1803.09746}, -issn = {22126864}, -journal = {Physics of the Dark Universe}, -keywords = {Gravitational lensing,Image simulations,Software}, -pages = {189--201}, -title = {{lenstronomy: Multi-purpose gravitational lens modelling software package}}, -volume = {22}, -year = {2018} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Greene2012, -abstract = {We use the Mitchell Spectrograph (formerly VIRUS-P) on the McDonald Observatory 2.7m Harlan J. Smith Telescope to search for the chemical signatures of massive elliptical galaxy assembly. The Mitchell Spectrograph is an integral-field spectrograph with a uniquely wide field of view (107x107 sq arcsec), allowing us to achieve remarkably high signal-to-noise ratios of {\$\sim${}}20-70 per pixel in radial bins of 2-2.5 times the effective radii of the eight galaxies in our sample. Focusing on a sample of massive elliptical galaxies with stellar velocity dispersions sigma* {\textgreater}150 km/s, we study the radial dependence in the equivalent widths (EWs) of key metal absorption lines. By twice the effective radius, the Mgb EWs have dropped by {\$\sim${}}50{\%}, and only a weak correlation between sigma* and Mgb EW remains. The Mgb EWs at large radii are comparable to those seen in the centers of elliptical galaxies that are approximately an order of magnitude less massive. We find that the well-known metallicity gradients often observed within an effective radius continue smoothly to 2.5R{\_}e, while the abundance ratio gradients remain flat. Much like the halo of the Milky Way, the stellar halos of our galaxies have low metallicities and high alpha-abundance ratios, as expected for very old stars formed in small stellar systems. Our observations support a picture in which the outer parts of massive elliptical galaxies are built by the accretion of much smaller systems whose star formation history was truncated at early times.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -pages = {32}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -url = {http://stacks.iop.org/0004-637X/750/i=1/a=32}, -volume = {786}, -year = {2014} -} -@article{Sales2012, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V. and Navarro, Julio F. and Theuns, Tom and Schaye, Joop and White, Simon D.M. and Frenk, Carlos S. and Crain, Robert A. and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sales et al. - 2012 - The origin of discs and spheroids in simulated galaxies(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -month = {jun}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Pontzen2017, -abstract = {We show how the interplay between active galactic nuclei (AGN) and merger history determines whether a galaxy quenches star formation at high redshift. We first simulate, in a full cosmological context, a galaxy of total dynamical mass {\$}10{\^{}}{\{}12{\}}\backslash,M{\_}{\{}\backslashodot{\}}{\$} at {\$}z=2{\$}. Then we systematically alter the accretion history of the galaxy by minimally changing the linear overdensity in the initial conditions. This "genetic modification" approach allows the generation of three sets of {\$}\backslashLambda{\$}CDM initial conditions leading to maximum merger ratios of 1:10, 1:5 and 2:3 respectively. The changes leave the final halo mass, large scale structure and local environment unchanged, providing a controlled numerical experiment. Interaction between the AGN physics and mergers in the three cases lead respectively to a star-forming, temporarily-quenched and permanently-quenched galaxy. However the differences do not primarily lie in the black hole accretion rates, but in the kinetic effects of the merger: the galaxy is resilient against AGN feedback unless its gaseous disk is first disrupted. Typical accretion rates are comparable in the three cases, falling below {\$}0.1\backslash,M{\_}{\{}\backslashodot{\}}{\$} yr{\$}{\^{}}{\{}-1{\}}{\$}, equivalent to around {\$}2\backslash{\%}{\$} of the Eddington rate or {\$}10{\^{}}{\{}-3{\}}{\$} times the pre-quenching star formation rate, in agreement with observations. This low level of black hole accretion can be sustained even when there is insufficient dense cold gas for star formation. Conversely, supernova feedback is too distributed to generate outflows in high-mass systems, and cannot maintain quenching over periods longer than the halo gas cooling time.}, -archivePrefix = {arXiv}, -arxivId = {1607.02507}, -author = {Pontzen, Andrew and Tremmel, Michael and Roth, Nina and Peiris, Hiranya V and Saintonge, Am{\'{e}}lie and Volonteri, Marta and Quinn, Tom and Governato, Fabio}, -doi = {10.1093/mnras/stw2627}, -eprint = {1607.02507}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: star formation,Galaxies: stellar content}, -number = {1}, -pages = {547--558}, -title = {{How to quench a galaxy}}, -volume = {465}, -year = {2017} -} -@article{Shao2016, -abstract = {The spatial distribution of the satellite populations of the Milky Way and Andromeda are puzzling in that they are nearly perpendicular to the discs of their central galaxies. To understand the origin of such configurations we study the alignment of the central galaxy, satellite system and dark matter halo in the largest of the 'Evolution and Assembly of GaLaxies and their Environments' (eagle) simulation. We find that centrals and their satellite systems tend to be well aligned with their haloes, with a median misalignment angle of 33° in both cases. While the centrals are better aligned with the inner 10 kpc halo, the satellite systems are better aligned with the entire halo indicating that satellites preferentially trace the outer halo. The central-satellite alignment is weak (median misalignment angle of 52°) and we find that around 20 per cent of systems have a misalignment angle larger than 78°, which is the value for the Milky Way. The central-satellite alignment is a consequence of the tendency of both components to align with the dark matter halo. As a consequence, when the central is parallel to the satellite system, it also tends to be parallel to the halo. In contrast, if the central is perpendicular to the satellite system, as in the case of the Milky Way and Andromeda, then the central-halo alignment is much weaker. Dispersion-dominated (spheroidal) centrals have a stronger alignment with both their halo and their satellites than rotation-dominated (disc) centrals. We also found that the halo, the central galaxy and the satellite system tend to be aligned with the surrounding large-scale distribution of matter, with the halo being the better aligned of the three.}, -archivePrefix = {arXiv}, -arxivId = {1605.01728}, -author = {Shao, Shi and Cautun, Marius and Frenk, Carlos S and Gao, Liang and Crain, Robert A and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw1247}, -eprint = {1605.01728}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3772--3783}, -title = {{Alignments between galaxies, satellite systems and haloes}}, -volume = {460}, -year = {2016} -} -@article{Swinbank2015a, -abstract = {We exploit long baseline ALMA submillimeter observations of the lensed star-forming galaxy SDP 81 at z = 3.042 to investigate the properties of the interstellar medium (ISM) on scales of 50-100 pc. The kinematics of the 12CO gas within this system are well described by a rotationally supported disk with an inclination-corrected rotation speed, vrot = 320 ± 20 km s-1, and a dynamical mass of Mdyn= (3.5 ± 1.0)× 1010 within a radius of 1.5 kpc. The disk is gas-rich and unstable, with a Toomre parameter, Q = 0.30 ± 0.10, and so into star-forming regions with Jeans length LJ∼130 pc. We identify five star-forming regions within the ISM on these scales and show that their scaling relations between luminosity, line widths, and sizes are significantly offset from those typical of molecular clouds in local galaxies (Larson's relations). These offsets are likely to be caused by the high external hydrostatic pressure for the ISM, Ptot/KB∼ 40-20+30 × 107 K cm-3, which is ∼104× higher than the typical ISM pressure in the Milky Way. The physical conditions of the star-forming ISM and giant molecular clouds appear to be similar to those found in the densest environments in the local universe, such as those in the Galactic center.}, -archivePrefix = {arXiv}, -arxivId = {1505.05148}, -author = {Swinbank, A. M. and Dye, S. and Nightingale, J. W. and Furlanetto, C. and Smail, Ian and Cooray, A. and Dannerbauer, H. and Dunne, L. and Eales, S. and Gavazzi, R. and Hunter, T. and Ivison, R. J. and Negrello, M. and Oteo-Gomez, I. and Smit, R. and Werf, P. Van Der and Vlahakis, C.}, -doi = {10.1088/2041-8205/806/1/L17}, -eprint = {1505.05148}, -issn = {20418213}, -journal = {Astrophysical Journal Letters}, -keywords = {evolution,galaxies: high-redshift,galaxies: starburst}, -number = {1}, -title = {{ALMA resolves the properties of star-forming regions in a dense gas disk at z ∼ 3}}, -volume = {806}, -year = {2015} -} -@article{Veale2016, -abstract = {We present spatially resolved two-dimensional stellar kinematics for the 41 most massive early-type galaxies (ETGs; MK ≲ -25.7 mag, stellar mass M* ≳ 1011.8 M⊙) of the volumelimited (D {\textless} 108 Mpc) MASSIVE survey. For each galaxy, we obtain high-quality spectra in the wavelength range of 3650-5850 {\AA}from the 246-fibre Mitchell integral-field spectrograph at McDonald Observatory, covering a 107 arcsec×107 arcsec field of view(often reaching 2 to 3 effective radii).We measure the 2D spatial distribution of each galaxy's angular momentum ($\lambda$ and fast or slow rotator status), velocity dispersion ($\sigma$), and higher order non-Gaussian velocity features (Gauss-Hermite moments h3 to h6). Our sample contains a high fraction ({\$\sim${}}80 per cent) of slow and non-rotators with $\lambda$ ≲ 0.2. When combined with the lower mass ETGs in the ATLAS3D survey, we find the fraction of slow rotators to increase dramatically with galaxy mass, reaching {\$\sim${}}50 per cent at MK {\$\sim${}} -25.5 mag and {\$\sim${}}90 per cent at MK ≲ -26 mag. All of our fast rotators show a clear anticorrelation between h3 and V/$\sigma$, and the slope of the anticorrelation is steeper in more round galaxies. The radial profiles of s show a clear luminosity and environmental dependence: the 12 most luminous galaxies in our sample (MK ≲ -26 mag) are all brightest cluster/group galaxies (except NGC 4874) and all have rising or nearly flat s profiles, whereas five of the seven 'isolated' galaxies are all fainter than MK = -25.8 mag and have falling $\sigma$. All of our galaxies have positive average h4; the most luminous galaxies have average h4 {\$\sim${}} 0.05, while less luminous galaxies have a range of values between 0 and 0.05. Most of our galaxies show positive radial gradients in h4, and those galaxies also tend to have rising s profiles. We discuss the implications for the relationship among dynamical mass, $\sigma$, h4, and velocity anisotropy for these massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1609.00391}, -author = {Veale, Melanie and Ma, Chung Pei and Thomas, Jens and Greene, Jenny E and McConnell, Nicholas J and Walsh, Jonelle and Ito, Jennifer and Blakeslee, John P and Janish, Ryan}, -doi = {10.1093/mnras/stw2330}, -eprint = {1609.00391}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {1}, -pages = {356--384}, -title = {{The MASSIVE Survey - V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies}}, -volume = {464}, -year = {2017} -} -@article{Sonnenfeld2013a, -abstract = {This white paper describes the LSST Dark Energy Science Collaboration (DESC), whose goal is the study of dark energy and related topics in fundamental physics with data from the Large Synoptic Survey Telescope (LSST). It provides an overview of dark energy science and describes the current and anticipated state of the field. It makes the case for the DESC by laying out a robust analytical framework for dark energy science that has been defined by its members and the comprehensive three-year work plan they have developed for implementing that framework. The analysis working groups cover five key probes of dark energy: weak lensing, large scale structure, galaxy clusters, Type Ia supernovae, and strong lensing. The computing working groups span cosmological simulations, galaxy catalogs, photon simulations and a systematic software and computational framework for LSST dark energy data analysis. The technical working groups make the connection between dark energy science and the LSST system. The working groups have close linkages, especially through the use of the photon simulations to study the impact of instrument design and survey strategy on analysis methodology and cosmological parameter estimation. The white paper describes several high priority tasks identified by each of the 16 working groups. Over the next three years these tasks will help prepare for LSST analysis, make synergistic connections with ongoing cosmological surveys and provide the dark energy community with state of the art analysis tools. Members of the community are invited to join the LSST DESC, according to the membership policies described in the white paper. Applications to sign up for associate membership may be made by submitting the Web form at http://www.slac.stanford.edu/exp/lsst/desc/signup.html with a short statement of the work they wish to pursue that is relevant to the LSST DESC.}, -annote = {From Duplicate 14 (Supermassive black holes and their host spheroids I. Galaxy vivisection - Savorgnan, Giulia A. D.; Graham, Alister W.) - -NULL}, -archivePrefix = {arXiv}, -arxivId = {1211.0310}, -author = {{LSST Dark Energy Science Collaboration}}, -doi = {10.1023/A:1002120921330}, -eprint = {1211.0310}, -isbn = {doi:10.1088/0004-637X/786/2/89}, -issn = {0004640X}, -journal = {Astrophysics and Space Science}, -keywords = {Astrophysics - Cosmology and Extragalactic Astroph,Black hole physics,Data analysis,Galaxies: active,Galaxies: evolution,Galaxies: high-redshift,Galaxies: structure,Gravitational lensing: strong-methods,High Energy Physics - Experiment,Methods: numerical,Methods: statistical,Techniques: image processing,active,cD,catalogs,ccd,cte,cti,dwarf,evolution,formation,fundamental parameters,galaxies,galaxies: elliptical and lenticular,galaxies: formation,galaxies: high-redshift,galaxies: photometry,galaxies: statistics,galaxies: structure,galaxies: structure surveys,general,gravitational lensing,hxmt,interactions,irregular,ism,keyword1,keyword2,keyword3,le,proton-irradiated,quasars,scd,star formation,strong - galaxies,struc-,structure}, -month = {jun}, -number = {2}, -pages = {51--54}, -title = {{Large Synoptic Survey Telescope: Dark Energy Science Collaboration}}, -url = {http://arxiv.org/abs/1211.0310}, -volume = {263}, -year = {2012} -} -@article{Lipnicky2018, -abstract = {We report HI observations of eight spiral galaxies that are strongly lensing background sources. Our targets were selected from the Sloan WFC (Wide Field Camera) Edge-on Late-type Lens Survey (SWELLS) using the Arecibo, Karl G. Jansky Very Large Array, and Green Bank telescopes. We securely detect J1703+2451 at z=0.063 with a signal-to-noise of 6.7 and W50=79+/-13 km/s, obtaining the first detection of HI emission in a strong spiral lens. We measure a mass of M(HI)= 1.77+/-0.06(+0.35/-0.75) x 10{\^{}}9 M{\_}(sol) for this source. We find that this lens is a normal spiral, with observable properties that are fairly typical of spiral galaxies. For three other sources we did not secure a detection; however, we are able to place strong constraints on the HI masses of those galaxies. The observations for four of our sources were rendered unusable due to strong radio frequency interference.}, -archivePrefix = {arXiv}, -arxivId = {1802.01588}, -author = {Lipnicky, Andrew and Chakrabarti, Sukanya and Wright, Melvyn C H and Blitz, Leo and Heiles, Carl and Cotton, William and Frayer, David and Blandford, Roger and Shu, Yiping and Bolton, Adam S}, -doi = {10.1093/mnras/sty326}, -eprint = {1802.01588}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Radio lines: galaxies}, -number = {3}, -pages = {3097--3105}, -title = {{The first detection of neutral hydrogen in emission in a strong spiral lens}}, -url = {http://arxiv.org/abs/1802.01588%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty326}, -volume = {476}, -year = {2018} -} -@article{Mendez-Abreu2010, -abstract = {Context. Knowledge of the intrinsic shapes of galaxy components provides crucial information when constraining phenomena driving their formation and evolution. Aims. We analize the structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies to derive the intrinsic shape of their bulges. Methods. We developed a new method to derive the intrinsic shapes of bulges based on geometrical relationships between the apparent and intrinsic shapes of bulges and disks. Bulges were assumed to be triaxial ellipsoids sharing the same center and polar axis of their surrounding disks. Disks were assumed to be circular, infinitesimally thin, and to lie on the equatorial plane of bulges. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, the twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and the galaxy inclination. Results. We find that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them are characterized by an elliptical section (B/A {\textless} 0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C {\textless} (A + B)/2). Only 18{\%} of the observed bulges have a probability {\textgreater}50{\%} and none has a probability {\textgreater}90{\%} of being elongated along the polar axis. The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with S{\'{e}}rsic index n {\textgreater} 2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T {\textgreater} 0.3. Bulges with n ≤ 2 and with B/T ≤ 0.3 follow a similar distribution, which differs from that of bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. In particular, bulges with n ≤ 2 and B/T ≤ 0.3 exhibit a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n {\textgreater} 2 and with B/T {\textgreater} 0.3, respectively. No correlation is found between the intrinsic shape and either the luminosity or velocity dispersion of bulges. Conclusions. According to predictions of the numerical simulations of bulge formation, bulges with n ≤ 2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T ≤ 0.3, may be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n {\textgreater} 2 and B/T {\textgreater} 0.3. {\textcopyright}2010 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {M{\'{e}}ndez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -number = {7}, -pages = {A71}, -title = {{Structural properties of disk galaxies: II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Gilman2016, -abstract = {The arrival times, positions and fluxes of multiple images in strong lens systems can be used to infer the presence of dark subhaloes in the deflector, and thus test predictions of cold dark matter models. However, gravitational lensing does not distinguish between perturbations to a smooth gravitational potential arising from baryonic and non-baryonic mass. In this work, we quantify the extent to which the stellar mass distribution of a deflector can reproduce flux ratio and astrometric anomalies typically associated with the presence of a dark matter subhalo. Using Hubble Space Telescope images of nearby galaxies, we simulate strong lens systems with real distributions of stellar mass as they would be observed at redshift zd = 0.5. We add a dark matter halo and external shear to account for the smooth dark matter field, omitting dark substructure, and use a Monte Carlo procedure to characterize the distributions of image positions, time delays and flux ratios for a compact background source of diameter 5 pc. By convolving high-resolution images of real galaxies with a Gaussian point spread function, we simulate the most detailed smooth potential one could construct given high-quality data, and find scatter in flux ratios of ≈10 per cent, which we interpret as a typical deviation from a smooth potential caused by large- and small-scale structure in the lensing galaxy. We demonstrate that the flux ratio anomalies arising from galaxy-scale baryonic structure can be minimized by selecting the most massive and round deflectors and by simultaneously modelling flux ratio and astrometric data.}, -archivePrefix = {arXiv}, -arxivId = {1610.08525}, -author = {Gilman, Daniel and Agnello, Adriano and Treu, Tommaso and Keeton, Charles R. and Nierenberg, Anna M.}, -doi = {10.1093/mnras/stx158}, -eprint = {1610.08525}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gilman et al. - 2017 - Strong lensing signatures of luminous structure and substructure in early-type galaxies.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: structure,Gravitational lensing: strong}, -number = {4}, -pages = {3970--3992}, -title = {{Strong lensing signatures of luminous structure and substructure in early-type galaxies}}, -url = {http://arxiv.org/abs/1610.08525}, -volume = {467}, -year = {2017} -} -@article{Xu2016, -abstract = {Early-type galaxies provide unique tests for the predictions of the cold dark matter cosmology and the baryonic physics assumptions entering models for galaxy formation. In this work, we use the Illustris simulation to study correlations of three main properties of early-type galaxies, namely, the stellar orbital anisotropies, the central dark matter fractions and the central radial density slopes, as well as their redshift evolution since {\$}z=1.0{\$}. We find that lower-mass galaxies or galaxies at higher redshift tend to be bluer in rest-frame colour, have higher central gas fractions, and feature more tangentially anisotropic orbits and steeper central density slopes than their higher-mass or lower-redshift counterparts, respectively. The projected central dark matter fraction within the effective radius shows a very mild mass dependence but positively correlates with galaxy effective radii due to the aperture effect. The central density slopes obtained by combining strong lensing measurements with single aperture kinematics are found to differ from the true density slopes. We identify systematic biases in this measurement to be due to two common modelling assumptions, isotropic stellar orbital distributions and power-law density profiles. We also compare the properties of early-type galaxies in Illustris to those from existing galaxy and strong lensing surveys, we find in general broad agreement but also some tension, which poses a potential challenge to the stellar formation and feedback models adopted by the simulation.}, -archivePrefix = {arXiv}, -arxivId = {1610.07605}, -author = {Xu, Dandan and Springel, Volker and Sluse, Dominique and Schneider, Peter and Sonnenfeld, Alessandro and Nelson, Dylan and Vogelsberger, Mark and Hernquist, Lars}, -doi = {10.1093/mnras/stx899}, -eprint = {1610.07605}, -keywords = {cosmology,gravitational lensing,haloes - galaxies,strong - galaxies,structure -,theory - dark matter}, -number = {October}, -pages = {27}, -title = {{The inner structure of early-type galaxies in the Illustris simulation}}, -url = {http://arxiv.org/abs/1610.07605%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx899}, -volume = {27}, -year = {2016} -} -@article{LaBarbera2009, -abstract = {In this Letter, we present mean optical+NIR color gradient estimates for 5080 early-type galaxies (ETGs) in the grizY JHK wavebands of the Sloan Digital Sky Survey plus the UKIRT Infrared Deep Sky Survey. The color gradient is estimated as the logarithmic slope of the radial color profile in ETGs. With such a large sample size, we study the variation of the mean color gradient as a function of waveband with unprecedented accuracy. We find that (1) color gradients are mainly due, on average, to a metallicity variation of about -0.4 dex per decade in galaxy radius; and (2) a small, but significant, positive age gradient is present, on average, in ETGs, with the inner stellar population being slightly younger, by 0.1 dex per radial decade, than the outer one. Also, we show that the presence of a positive mean age gradient in ETGs, as found in the present study, implies their effective radius to be smaller at high-z, consistent with observations. {\textcopyright} 2009. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0905.0791}, -author = {{La Barbera}, F. and {De Carvalho}, R. R.}, -doi = {10.1088/0004-637X/699/2/L76}, -eprint = {0905.0791}, -isbn = {9780470057964}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters}, -number = {2 PART 2}, -pages = {L76--L79}, -pmid = {17897953}, -title = {{The origin of color gradients in early-type systems and their compactness at high-z}}, -url = {http://stacks.iop.org/1538-4357/699/i=2/a=L76?key=crossref.9031f64d59248ac62748a287a8a42f17}, -volume = {699}, -year = {2009} -} -@article{Shao2016, -abstract = {The spatial distribution of the satellite populations of the Milky Way and Andromeda are puzzling in that they are nearly perpendicular to the discs of their central galaxies. To understand the origin of such configurations we study the alignment of the central galaxy, satellite system and dark matter halo in the largest of the 'Evolution and Assembly of GaLaxies and their Environments' (eagle) simulation. We find that centrals and their satellite systems tend to be well aligned with their haloes, with a median misalignment angle of 33° in both cases. While the centrals are better aligned with the inner 10 kpc halo, the satellite systems are better aligned with the entire halo indicating that satellites preferentially trace the outer halo. The central-satellite alignment is weak (median misalignment angle of 52°) and we find that around 20 per cent of systems have a misalignment angle larger than 78°, which is the value for the Milky Way. The central-satellite alignment is a consequence of the tendency of both components to align with the dark matter halo. As a consequence, when the central is parallel to the satellite system, it also tends to be parallel to the halo. In contrast, if the central is perpendicular to the satellite system, as in the case of the Milky Way and Andromeda, then the central-halo alignment is much weaker. Dispersion-dominated (spheroidal) centrals have a stronger alignment with both their halo and their satellites than rotation-dominated (disc) centrals. We also found that the halo, the central galaxy and the satellite system tend to be aligned with the surrounding large-scale distribution of matter, with the halo being the better aligned of the three.}, -archivePrefix = {arXiv}, -arxivId = {1605.01728}, -author = {Shao, Shi and Cautun, Marius and Frenk, Carlos S and Gao, Liang and Crain, Robert A and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw1247}, -eprint = {1605.01728}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3772--3783}, -title = {{Alignments between galaxies, satellite systems and haloes}}, -volume = {460}, -year = {2016} -} -@article{Greene2017b, -abstract = {The "kinematic" morphology-density relation for early-type galaxies posits that those galaxies with low angular momentum are preferentially found in the highest-density regions of the universe. We use a large sample of galaxy groups with halo masses 10{\^{}}12.5 {\textless} M{\_}halo {\textless} 10{\^{}}14.5 M{\_}sun/h observed with the Mapping Nearby Galaxies at APO (MaNGA) survey to examine whether there is a correlation between local environment and rotational support that is independent of stellar mass. We find no compelling evidence for a relationship between the angular momentum content of early-type galaxies and either local overdensity or radial position within the group at fixed stellar mass.}, -archivePrefix = {arXiv}, -arxivId = {1708.07843}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Goddard, D and Ge, J and Andrews, B H and Brinkman, J and Brownstein, J R and Greco, J and Law, D and Lin, Y.-T. and Masters, K L and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Yan, R and Drory, N}, -doi = {10.3847/2041-8213/aa8ace}, -eprint = {1708.07843}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L33}, -title = {{SDSS-IV MaNGA: Probing the Kinematic Morphology–Density Relation of Early-type Galaxies with MaNGA}}, -url = {http://arxiv.org/abs/1708.07843%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa8ace}, -volume = {851}, -year = {2017} -} -@article{Cappellari2008, -abstract = {We present a simple and efficient anisotropic generalization of the semi-isotropic (two-integral) axisymmetric Jeans formalism, which is used to model the stellar kinematics of galaxies. The following is assumed: (i) a constant mass-to-light ratio (M/L) and (ii) a velocity ellipsoid that is aligned with cylindrical coordinates (R, z) and characterized by the classic anisotropy parameter. Our simple models are fit to SAURON integral-field observations of the stellar kinematics for a set of fast-rotator early-type galaxies. With only two free parameters ($\beta$z and the inclination), the models generally provide remarkably good descriptions of the shape of the first (V) and second () velocity moments, once a detailed description of the surface brightness is given. This is consistent with previous findings on the dynamical structure of these objects. With the observationally motivated assumption that $\beta$z ≳ 0, the method is able to recover the inclination. The technique can be used to determine the dynamical M/L and angular momenta of early-type fast-rotators and spiral galaxies, especially when the quality of the data does not justify more sophisticated modelling approaches. This formalism allows for the inclusion of dark matter, supermassive black holes, spatially varying anisotropy and multiple kinematic components. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0806.0042}, -author = {Cappellari, Michele}, -doi = {10.1111/j.1365-2966.2008.13754.x}, -eprint = {0806.0042}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure,cD}, -number = {1}, -pages = {71--86}, -title = {{Measuring the inclination and mass-to-light ratio of axisymmetric galaxies via anisotropic Jeans models of stellar kinematics}}, -volume = {390}, -year = {2008} -} -@article{Morningstar2019, -abstract = {We present a machine learning method for the reconstruction of the undistorted images of background sources in strongly lensed systems. This method treats the source as a pixelated image and utilizes the Recurrent Inference Machine (RIM) to iteratively reconstruct the background source given a lens model. Our architecture learns to minimize the likelihood of the model parameters (source pixels) given the data using the physical forward model (ray tracing simulations) while implicitly learning the prior of the source structure from the training data. This results in better performance compared to linear inversion methods, where the prior information is limited to the 2-point covariance of the source pixels approximated with a Gaussian form, and often specified in a relatively arbitrary manner. We combine our source reconstruction network with a convolutional neural network that predicts the parameters of the mass distribution in the lensing galaxies directly from telescope images, allowing a fully automated reconstruction of the background source images and the foreground mass distribution.}, -archivePrefix = {arXiv}, -arxivId = {1901.01359}, -author = {Morningstar, Warren R. and Levasseur, Laurence Perreault and Hezaveh, Yashar D. and Blandford, Roger and Marshall, Phil and Putzky, Patrick and Rueter, Thomas D. and Wechsler, Risa and Welling, Max}, -doi = {10.3847/1538-4357/ab35d7}, -eprint = {1901.01359}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Morningstar et al. - 2019 - Data-driven Reconstruction of Gravitationally Lensed Galaxies Using Recurrent Inference Machines(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {14}, -title = {{Data-driven Reconstruction of Gravitationally Lensed Galaxies Using Recurrent Inference Machines}}, -url = {http://arxiv.org/abs/1901.01359}, -volume = {883}, -year = {2019} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful number of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag limit of ∼24. However, gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z ∼ 5-7 for LSST. We find that the LSST Wide Fast Deep survey could detect up to 120 lensed Population (Pop) I and II SNe but no lensed Pop III SNe. Deep-drilling programs in 10 deg2 fields could detect Pop I and II core-collapse SNe at AB magnitudes of 27-28 and 26, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes Erik and Whalen, Daniel J and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S}, -doi = {10.1093/mnras/stz3203}, -eprint = {1805.02662}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: dark ages,Cosmology: observations,First stars: early universe,Galaxies: high,Gravitational lensing: strong,Redshift,Reionization,Stars: Population III,Supernovae: general}, -number = {2}, -pages = {2447--2459}, -title = {{Detecting strongly lensed supernovae at z ∼ 5-7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {491}, -year = {2020} -} -@article{Greene2012, -abstract = {We present a two-dimensional kinematic analysis out to ∼2-5 effective radii (Re) of 33 massive elliptical galaxies with stellar velocity dispersions $\sigma$ > 150 km s-1. Our observations were taken using the Mitchell Spectrograph (formerly VIRUS-P), a spectrograph with a large 107 × 107 arcsec2 field of view that allows us to construct robust, spatially resolved kinematic maps of V and $\sigma$ for each galaxy extending to at least 2 Re . Using these maps, we study the radial dependence of the stellar angular momentum and other kinematic properties. We see the familiar division between slow and fast rotators persisting out to a large radius in our sample. Centrally slow rotating galaxies, which are almost universally characterized by some form of kinematic decoupling or misalignment, remain slowly rotating in their halos. The majority of fast-rotating galaxies show either increases in specific angular momentum outward or no change beyond Re . The generally triaxial nature of the slow rotators suggests that they formed through mergers, consistent with a "two-phase" picture of elliptical galaxy formation. However, we do not observe the sharp transitions in kinematics proposed in the literature as a signpost of moving from central dissipationally formed components to outer accretion-dominated halos. {\textcopyright} 2014. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1202.4464}, -author = {Raskutti, Sudhir and Greene, Jenny E. and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/786/1/23}, -eprint = {1202.4464}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Raskutti, Greene, Murphy - 2014 - The stellar halos of massive elliptical galaxies. III. Kinematics at large radius(3).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure}, -number = {1}, -title = {{The stellar halos of massive elliptical galaxies. III. Kinematics at large radius}}, -volume = {786}, -year = {2014} -} -@article{Koopmans2005, -abstract = {We propose the novel method of 'gravitational imaging' to detect and quantify luminous and dark matter substructures in gravitational lens galaxies. The method utilizes highly magnified Einstein rings and arcs as sensitive probes of small perturbations in the lens potential (due to the presence of the mass substructure), reconstructing the gravitational lens potential non-parametrically. Numerical simulations show that the implemented algorithm can reconstruct the smooth mass distribution of a typical lens galaxy - exhibiting reasonable signal-to-noise Einstein rings - as well as compact substructure with masses as low as Msub ∼ 10-3 M lens, if present. 'Gravitational imaging' of pure dark matter substructures around massive galaxies can provide new insight into the standard cold dark matter paradigm, using very different physics than ground-based direct-detection experiments, and probe the hierarchical structure-formation model which predicts that this substructure exists in great abundance. {\textcopyright} 2005 RAS.}, -author = {Koopmans, L. V.E.}, -doi = {10.1111/j.1365-2966.2005.09523.x}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Koopmans2005GravImaging.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Gravitational lensing}, -number = {4}, -pages = {1136--1144}, -title = {{Gravitational imaging of cold dark matter substructures}}, -volume = {363}, -year = {2005} -} -@article{White1991, -abstract = {Analytic methods for studying the formation of galaxies by gas condensation within massive dark halos are presented. The present scheme applies to cosmogonies where structure grows through hierarchical clustering of a mixture of gas and dissipationless dark matter. The simplest models consistent with the current understanding of N-body work on dissipationless clustering, and that of numerical and analytic work on gas evolution and cooling are adopted. Standard models for the evolution of the stellar population are also employed, and new models for the way star formation heats and enriches the surrounding gas are constructed. Detailed results are presented for a cold dark matter universe with Omega = 1 and H(0) = 50 km/s/Mpc, but the present methods are applicable to other models. The present luminosity functions contain significantly more faint galaxies than are observed.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9602054}, -author = {White, Simon D. M. and Frenk, Carlos S.}, -doi = {10.1086/170483}, -eprint = {9602054}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Analytic Functions,Brightness Distribution,Cosmology,Dark Matter,Galactic Clusters,Galactic Evolution,Galactic Structure,Halos,Numerical Analysis,Star Distribution,Star Formation}, -month = {sep}, -pages = {52}, -primaryClass = {astro-ph}, -title = {{Galaxy formation through hierarchical clustering}}, -url = {http://arxiv.org/abs/astro-ph/9602054}, -volume = {379}, -year = {1991} -} -@article{Lipnicky2018, -abstract = {We reportHI observations of eight spiral galaxies that are strongly lensing background sources. Our targets were selected from the Sloan WFC (Wide Field Camera) Edge-on Late-type Lens Survey (SWELLS) using the Arecibo, Karl G. Jansky Very Large Array, and Green Bank telescopes. We securely detect J1703+2451 at z = 0.063 with a signal-to-noise ratio of 6.7 and W50 = 79 ± 13 km s-1, obtaining the first detection of HI emission in a strong spiral lens. We measure a mass of MHI = (1.77 ± 0.06 -0.75+0.35) × 109M⊙ for this source. We find that this lens is a normal spiral, with observable properties that are fairly typical of spiral galaxies. For three other sources, we did not secure a detection; however, we are able to place strong constraints on the HI masses of those galaxies. The observations for four of our sources were rendered unusable due to strong radio frequency interference.}, -archivePrefix = {arXiv}, -arxivId = {1802.01588}, -author = {Lipnicky, Andrew and Chakrabarti, Sukanya and Wright, Melvyn C H and Blitz, Leo and Heiles, Carl and Cotton, William and Frayer, David and Blandford, Roger and Shu, Yiping and Bolton, Adam S}, -doi = {10.1093/mnras/sty326}, -eprint = {1802.01588}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: spiral,Gravitational lensing: strong,Radio lines: galaxies}, -number = {3}, -pages = {3097--3105}, -title = {{The first detection of neutral hydrogen in emission in a strong spiral lens}}, -url = {http://arxiv.org/abs/1802.01588%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/sty326}, -volume = {476}, -year = {2018} -} -@article{Herbert-Fort2007, -abstract = {We measure the distribution of velocities for prograde and retrograde satellite galaxies using a combination of published data and new observations for 78 satellites of 63 extremely isolated disc galaxies (169 satellites total). We find that the velocity distribution is non-Gaussian (>99.9 per cent confidence), but that it can be described as the sum of two Gaussians, one of which is broad ($\sigma$ = 176 ± 15 km s-1), has a mean prograde velocity of 86 ± 30 km s-1, and contains ∼55 per cent of the satellites, while the other is slightly retrograde with a mean velocity of -21 ± 22 km s-1 and $\sigma$ = 74 ± 18 km s-1 and contains ∼45 per cent of the satellites. Both of these components are present over all projected radii and found in the sample regardless of cuts on primary inclination or satellite disc angle. The double-Gaussian shape, however, becomes more pronounced among satellites of more luminous primaries. We remove the potential dependence of satellite velocity on primary luminosity using the Tully-Fisher relation and still find the velocity distribution to be asymmetric and even more significantly non-Gaussian. The asymmetric velocity distribution demonstrates a connection between the inner, visible disc galaxy, and the kinematics of the outer, dark halo. The reach of this connection, extending even beyond the virial radii, suggests that it is imprinted by the satellite infall pattern and large-scale effects, rather than by higher level dynamical processes in the formation of the central galaxy or late-term evolution of the satellites. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0711.4123}, -author = {Herbert-Fort, St{\'{e}}phane and Zaritsky, Dennis and {Jin Kim}, Yeun and Bailin, Jeremy and Taylor, James E.}, -doi = {10.1111/j.1365-2966.2007.12756.x}, -eprint = {0711.4123}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Herbert-Fort et al. - 2008 - The orbital distribution of satellite galaxies.pdf:pdf}, -isbn = {9783863040475}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: evolution,Galaxies: haloes,Galaxies: structure}, -number = {2}, -pages = {803--813}, -title = {{The orbital distribution of satellite galaxies}}, -url = {http://arxiv.org/abs/0711.4123}, -volume = {384}, -year = {2008} -} -@article{Regier2015, -abstract = {We present a new, fully generative model of optical telescope image sets, along with a variational procedure for inference. Each pixel intensity is treated as a Poisson random variable, with a rate parameter dependent on latent properties of stars and galaxies. Key latent properties are themselves random, with scientific prior distributions constructed from large ancillary data sets. We check our approach on synthetic images. We also run it on images from a major sky survey, where it exceeds the performance of the current state-of-the-art method for locating celestial bodies and measuring their colors.}, -archivePrefix = {arXiv}, -arxivId = {1506.01351}, -author = {Regier, Jeffrey and Miller, Andrew and McAuliffe, Jon and Adams, Ryan and Hoffman, Matt and Lang, Dustin and Schlegel, David and Prabhat}, -eprint = {1506.01351}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Regier et al. - 2015 - Celeste Variational inference for a generative model of astronomical images.pdf:pdf}, -isbn = {9781510810587}, -journal = {32nd International Conference on Machine Learning, ICML 2015}, -pages = {2095--2103}, -title = {{Celeste: Variational inference for a generative model of astronomical images}}, -volume = {3}, -year = {2015} -} -@article{MacArthur2009a, -abstract = {We present a detailed study of the stellar populations (SPs) and kinematics of the bulge and inner disc regions of eight nearby spiral galaxies (Sa-Sd) based on deep Gemini/GMOS data. The long-slit spectra extend to 1-2 disc scalelengths with S/N/{\AA} ≥ 50. Several different model fitting techniques involving absorption-line indices and full spectrum fitting are explored, and found to weigh age, metallicity and abundance ratios differently. We find that the SPs of spiral galaxies are not well matched by single episodes of star formation; more representative SPs must involve average SP values integrated over the star formation history (SFH) of the galaxy. Our 'full population synthesis' method is an optimized linear combination of model templates to the full spectrum with masking of regions poorly represented by the models. Realistic determinations of the SP parameters and kinematics (rotation and velocity dispersion) also rely on careful attention to data/model matching (resolution and flux calibration). The population fits reveal a wide range of age and metallicity gradients (from negative to positive) in the bulge, allowing for diverse formation mechanisms. The observed positive age gradients within the effective radius of some late-type bulges helps reconcile the long-standing conundrum of the coexistence of secular-like kinematics, light profile shape and stellar bar with the 'classical'-like old and $\alpha$-enhanced SPs in the Milky Way bulge. The discs, on the other hand, almost always show mildly decreasing to flat profiles in both age and metallicity, consistent with inside-out formation. Our spiral bulges follow the same correlations of increasing light-weighted age and metallicity with central velocity dispersion as those of elliptical galaxies and early-type bulges found in other studies, but when SFHs more complex and realistic than a single burst are invoked, the trend with age is shallower and the scatter much reduced. In a mass-weighted context, however, all bulges are predominantly composed of old and metal-rich SPs. While secular contributions to the evolution of many of our bulges are clearly evident, with young (0.001-1 Gyr) SPs contributing as much as 90 per cent of the optical (V-band) light, the bulge mass fraction from young stars is small (≲25 per cent). The implies a bulge formation dominated by early processes that are common to all spheroids, whether they currently reside in discs or not. While monolithic collapse cannot be ruled out in some cases, merging must be invoked to explain the SP gradients in most bulges. Further bulge growth via secular processes or 'rejuvenated' star formation generally contributes minimally to the stellar mass budget, with the relative secular weight increasing with decreasing central velocity dispersion. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4135}, -author = {MacArthur, Lauren A. and Gonz{\'{a}}lez, J. Jes{\'{u}}s and Courteau, St{\'{e}}phane}, -doi = {10.1111/j.1365-2966.2009.14519.x}, -eprint = {0901.4135}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/MacArthur, Gonz{\'{a}}lez, Courteau - 2009 - Stellar population and kinematic profiles in spiral bulges and discs Population synthesis of inte.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: spiral,Galaxies: stellar content}, -number = {1}, -pages = {28--63}, -title = {{Stellar population and kinematic profiles in spiral bulges and discs: Population synthesis of integrated spectra}}, -volume = {395}, -year = {2009} -} -@article{Mendez-Abreu2016, -abstract = {We present a two-dimensional multi-component photometric decomposition of 404 galaxies from the Calar Alto Legacy Integral Field Area data release 3 (CALIFA-DR3). They represent all possible galaxies with no clear signs of interaction and not strongly inclined in the final CALIFA data release. Galaxies are modelled in the g, r, and i Sloan Digital Sky Survey (SDSS) images including, when appropriate, a nuclear point source, bulge, bar, and an exponential or broken disc component. We use a human-supervised approach to determine the optimal number of structures to be included in the fit. The dataset, including the photometric parameters of the CALIFA sample, is released together with statistical errors and a visual analysis of the quality of each fit. The analysis of the photometric components reveals a clear segregation of the structural composition of galaxies with stellar mass. At high masses (log (M∗/MȮ) > 11), the galaxy population is dominated by galaxies modelled with a single S{\'{e}}rsic or a bulge+disc with a bulge-to-total (B/T) luminosity ratio B/T > 0.2. At intermediate masses (9.5 < log (M∗/MȮ) < 11), galaxies described with bulge+disc but B/T < 0.2 are preponderant, whereas, at the low mass end (log (M∗/MȮ) < 9.5), the prevailing population is constituted by galaxies modelled with either purediscs or nuclear point sources+discs (i.e., no discernible bulge). We obtain that 57% of the volume corrected sample of disc galaxies in the CALIFA sample host a bar. This bar fraction shows a significant drop with increasing galaxy mass in the range 9.5 < log (M∗/MȮ) < 11.5. The analyses of the extended multi-component radial profile result in a volume-corrected distribution of 62%, 28%, and 10% for the so-called Type I (pure exponential), Type II (down-bending), and Type III (up-bending) disc profiles, respectively. These fractions are in discordance with previous findings. We argue that the different methodologies used to detect the breaks are the main cause for these differences.}, -archivePrefix = {arXiv}, -arxivId = {1610.05324}, -author = {M{\'{e}}ndez-Abreu, J. and Ruiz-Lara, T. and S{\'{a}}nchez-Menguiano, L. and {De Lorenzo-C{\'{a}}ceres}, A. and Costantin, L. and Catal{\'{a}}n-Torrecilla, C. and Florido, E. and Aguerri, J. A.L. and Bland-Hawthorn, J. and Corsini, E. M. and Dettmar, R. J. and Galbany, L. and Garc{\'{i}}a-Benito, R. and Marino, R. A. and M{\'{a}}rquez, I. and Ortega-Minakata, R. A. and Papaderos, P. and S{\'{a}}nchez, S. F. and S{\'{a}}nchez-Blazquez, P. and Spekkens, K. and {Van De Ven}, G. and Wild, V. and Ziegler, B.}, -doi = {10.1051/0004-6361/201629525}, -eprint = {1610.05324}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/M{\'{e}}ndez-Abreu et al. - 2017 - Two-dimensional multi-component photometric decomposition of CALIFA galaxies(2).pdf:pdf}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: photometry,Galaxies: stellar content,Galaxies: structure}, -title = {{Two-dimensional multi-component photometric decomposition of CALIFA galaxies}}, -url = {http://arxiv.org/abs/1610.05324%0Ahttp://dx.doi.org/10.1051/0004-6361/201629525}, -volume = {598}, -year = {2017} -} -@article{Unruh2016, -abstract = {Strong gravitational lensing is regarded as the most precise technique to measure the mass in the inner region of galaxies or galaxy clusters. In particular, the mass within one Einstein radius can be determined with an accuracy of the order of a few percent or better, depending on the image configuration. For other radii, however, degeneracies exist between galaxy density profiles, precluding an accurate determination of the enclosed mass. The source position transformation (SPT), which includes the well-known mass-sheet transformation (MST) as a special case, describes this degeneracy of the lensing observables in a more general way. In this paper we explore properties of an SPT, removing the MST to leading order, that is we consider degeneracies which have not been described before. The deflection field $\alpha$ ($\theta$) resulting from an SPT is not curl-free in general, and thus not a deflection that can be obtained from a lensing mass distribution. Starting from a variational principle, we construct lensing potentials that give rise to a deflection field $\alpha$, which differs from $\alpha$ by less than an observationally motivated upper limit. The corresponding mass distributions from these "valid" SPTs are studied: their radial profiles are modified relative to the original mass distribution in a significant and non-trivial way, and originally axi-symmetric mass distributions can obtain a finite ellipticity. These results indicate a significant effect of the SPT on quantitative analyses of lens systems. We show that the mass inside the Einstein radius of the original mass distribution is conserved by the SPT; hence, as is the case for the MST, the SPT does not affect the mass determination at the Einstein radius. Furthermore, we analyse a degeneracy between two lens models, empirically found previously, and show that this degeneracy can be interpreted as being due to an SPT. Thus, degeneracies between lensing mass distributions are not just a theoretical possibility, but do arise in actual lens modeling.}, -archivePrefix = {arXiv}, -arxivId = {1606.04321}, -author = {Unruh, Sandra and Schneider, Peter and Sluse, Dominique}, -doi = {10.1051/0004-6361/201629048}, -eprint = {1606.04321}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {cosmological parameters,gravitational lensing: strong}, -month = {jun}, -number = {1}, -pages = {1--13}, -title = {{Ambiguities in gravitational lens models: The density field from the source position transformation}}, -url = {http://arxiv.org/abs/1606.04321%0Ahttp://dx.doi.org/10.1051/0004-6361/201629048}, -volume = {601}, -year = {2017} -} -@article{Belokurov2014, -abstract = {We announce the discovery of a new Galactic companion found in data from the ESO VST ATLAS survey, and followed up with deep imaging on the 4-m William Herschel Telescope. The satellite is located in the constellation of Crater (the Cup) at a distance of andtld;170 kpc. Its half-light radius is rh = 30 pc and its luminosity is MV = -5.5. The bulk of its stellar population is old and metal poor. We would probably have classified the newly discovered satellite as an extended globular cluster were it not for the presence of a handful of blue loop stars and a sparsely populated red clump. The existence of the core helium burning population implies that star formation occurred in Crater perhaps as recently as 400 Myr ago. No globular cluster has ever accomplished the feat of prolonging its star formation by several Gyr. Therefore, if our hypothesis that the blue bright stars in Crater are blue loop giants is correct, the new satellite should be classified as a dwarf galaxy with unusual properties. Note that only 10°to the north of Crater, two ultrafaint galaxies Leo IV and Leo V orbit the Galaxy at approximately the same distance. This hints that all three satellites may once have been closely associated before falling together into the Milky Way halo. {\textcopyright} 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.3406}, -author = {Belokurov, V. and Irwin, M. J. and Koposov, S. E. and Evans, N. W. and Gonzalez-Solares, E. and Metcalfe, N. and Shanks, T.}, -doi = {10.1093/mnras/stu626}, -eprint = {1403.3406}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: Dwarf,Galaxy: Fundamental parameters,Galaxy: Globular clusters: General,Galaxy: Halo,Magnitude diagrams,Russell and colour,Stars: Hertzsprung}, -month = {jul}, -number = {3}, -pages = {2124--2133}, -title = {{Atlas lifts the cup: Discovery of a new milky way satellite in crater}}, -volume = {441}, -year = {2014} -} -@article{Kitching2008, -abstract = {In this paper, we extend the Bayesian model fitting shape measurement method presented in Miller et al., and use the method to estimate the shear from the Shear TEsting Programme simulations (STEP). The method uses a fast model fitting algorithm that uses realistic galaxy profiles and analytically marginalizes over the position and amplitude of the model by doing the model fitting in Fourier space. This is used to find the full posterior probability in ellipticity. The shear is then estimated in a Bayesian way from this posterior probability surface. The Bayesian estimation allows measurement bias arising from the presence of random noise to be removed. In this paper, we introduce an iterative algorithm that can be used to estimate the intrinsic ellipticity prior and show that this is accurate and stable. We present results using the STEP parametrization that relates the input shear $\gamma$T to the estimated shear $\gamma$M by introducing a bias m and an offset c: $\gamma$M - $\gamma$T = m$\gamma$T + c. The average number density of galaxies used in the STEP1 analysis was 9 per square arcminute, for STEP2 the number density was 30 per square arcminute. By using the method to estimate the shear from the STEP1 simulations we find the method to have a shear bias of m = 0.006 ± 0.005 and a variation in shear offset with point spread function type of $\sigma$c = 0.0002. Using the method to estimate the shear from the STEP2 simulations we find that the shear bias and offset are m = 0.002 ± 0.016 and c = -0.0007 ± 0.0006, respectively. In addition, we find that the bias and offset are stable to changes in the magnitude and size of the galaxies. Such biases should yield any cosmological constraints from future weak lensing surveys robust to systematic effects in shape measurement. Finally, we present an alternative to the STEP parametrization by using a quality factor that relates the intrinsic shear variance in a simulation to the variance in shear that is measured and show that the method presented has an average of Q ≳ 100 which is at least a factor of 10 times better than other shape measurement methods. {\textcopyright}2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0802.1528}, -author = {Kitching, T D and Miller, L and Heymans, C E and {Van Waerbeke}, L and Heavens, A F}, -doi = {10.1111/j.1365-2966.2008.13628.x}, -eprint = {0802.1528}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observation,Gravitational lensing,Methods: data analysis,Methods: numerical,Methods: statistical}, -number = {1}, -pages = {149--167}, -title = {{Bayesian galaxy shape measurement for weak lensing surveys - II. Application to simulations}}, -volume = {390}, -year = {2008} -} -@article{Geometryeh, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{De-Lucia:2007aa, -author = {{De Lucia}, G and Blaizot, J}, -journal = {\mnras}, -month = {feb}, -pages = {2--14}, -title = {{The hierarchical formation of the brightest cluster galaxies}}, -volume = {375}, -year = {2007} -} -@article{Handley2015a, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and $\backslash$nspectroscopic ESA cornerstone mission, currently scheduled for launch in$\backslash$nlate 2011. Its primary science drivers are the composition, formation$\backslash$nand evolution of the Galaxy. Gaia will not achieve its scientific$\backslash$nrequirements without detailed calibration and correction for radiation$\backslash$ndamage. Microscopic models of Gaia's CCDs are being developed to$\backslash$nsimulate the effect of radiation damage, charge trapping, which causes$\backslash$ncharge transfer inefficiency. The key to calculating the probability of$\backslash$na photoelectron being captured by a trap is the 3D electron density$\backslash$nwithin each CCD pixel. However, this has not been physically modelled$\backslash$nfor Gaia CCD pixels. In this paper, the first of a series, we motivate$\backslash$nthe need for such specialised 3D device modelling and outline how its$\backslash$nfuture results will fit into Gaia's overall radiation calibration$\backslash$nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -isbn = {9780819472311}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy III}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Libeskind2014, -abstract = {We examine the angular infall pattern of subhaloes on to host haloes in the context of the large-scale structure. We find that this infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are found to be preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that it is always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range (∼10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large-scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group. {\textcopyright}2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1407.0394}, -author = {Libeskind, Noam I and Knebe, Alexander and Hoffman, Yehuda and Gottl{\"{o}}ber, Stefan}, -doi = {10.1093/mnras/stu1216}, -eprint = {1407.0394}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Large-scale structure of universe}, -number = {2}, -pages = {1274--1280}, -title = {{The universal nature of subhalo accretion}}, -volume = {443}, -year = {2014} -} -@article{Weijmans2014, -abstract = {We use the Atlas3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q=0.25 and standard deviation sigma{\_}q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and sigma{\_}q =0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrisations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P T and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F and Davies, Roger L and Davis, Timothy A and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular,Galaxies,Structure,cD- galaxies}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS{\textless}sup{\textgreater}3D{\textless}/sup{\textgreater} project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 {\textless} z {\textless} 0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 percent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.0763}, -author = {Lackner, C N and Gunn, J E}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data%7B%5C_%7Dquery?bibcode=2012arXiv1201.0763L%7B%5C&%7Dlink%7B%5C_%7Dtype=ABSTRACT%7B%5C%25%7D5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Genel2017, -abstract = {We analyze scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, star-formation rate and redshift are reproduced, and a quantitative comparison of projected r-band sizes at 0{\$\sim${}}{\textless}z{\textless}{\$\sim${}}2 shows agreement to much better than 0.25dex. We follow populations of z=0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M{\_}{\{}*,z=0{\}}{\textgreater}{\$\sim${}}10{\^{}}{\{}9.5{\}}Msun, the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z=0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M{\_}{\{}*,z=0{\}}{\textgreater}{\$\sim${}}10{\^{}}{\{}9.5{\}}Msun experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies with M{\_}{\{}*,z=0{\}}{\textgreater}{\$\sim${}}10{\^{}}{\{}11{\}}Msun, the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main-sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z=0.}, -archivePrefix = {arXiv}, -arxivId = {1707.05327}, -author = {Genel, Shy and Nelson, Dylan and Pillepich, Annalisa and Springel, Volker and Pakmor, R{\"{u}}diger and Weinberger, Rainer and Hernquist, Lars and Naiman, Jill and Vogelsberger, Mark and Marinacci, Federico and Torrey, Paul}, -doi = {10.1093/mnras/stx3078}, -eprint = {1707.05327}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Galaxies: structure,Methods: numerical}, -number = {3}, -pages = {3976--3996}, -title = {{The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation}}, -url = {http://arxiv.org/abs/1707.05327}, -volume = {474}, -year = {2018} -} -@article{Bullock:2005aa, -author = {Bullock, J.$\sim$S. and Johnston, K.$\sim$V.}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bullock, Johnston - 2005 - Tracing Galaxy Formation with Stellar Halos. I. Methods.pdf:pdf}, -journal = {\apj}, -month = {dec}, -pages = {931--949}, -title = {{Tracing Galaxy Formation with Stellar Halos. I. Methods}}, -volume = {635}, -year = {2005} -} -@article{Naab2007, -abstract = {We describe high-resolution smoothed particle hydrodynamics (SPH) simulations of three approximately M* field galaxies starting from $\Lambda$CDM initial conditions. The simulations are made intentionally simple, and include photoionization, cooling of the intergalactic medium, and star formation, but not feedback from AGNs or supernovae. All of the galaxies undergo an initial burst of star formation at z$\sim$5, accompanied by the formation of a bubble of heated gas. Two out of three galaxies show early-type properties at present, whereas only one of them experienced a major merger. Heating from shocks and PdV work dominates over cooling so that for most of the gas the temperature is an increasing function of time. By z$\sim$1 a significant fraction of the final stellar system is in place and the spectral energy distribution resembles those of observed massive red galaxies. The galaxies have grown from z=1-->0 on average by 25% in mass and in size by gas-poor (dry) stellar mergers. By the present day the simulated galaxies are old ($\sim$10 Gyr), kinematically hot stellar systems surrounded by hot gaseous haloes. Stars dominate the mass of the galaxies up to $\sim$4 effective radii ($\sim$10 kpc). Kinematic and most photometric properties are in good agreement with those of observed elliptical galaxies. The galaxy with a major merger develops a counter-rotating core. Our simulations show that realistic intermediate-mass giant elliptical galaxies with plausible formation histories can be formed from $\Lambda$CDM initial conditions even without requiring recent major mergers or feedback from supernovae or AGNs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0512235}, -author = {Naab, Thorsten and Johansson, Peter H. and Ostriker, Jeremiah P. and Efstathiou, George}, -doi = {10.1086/510841}, -eprint = {0512235}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Naab et al. - 2007 - Formation of Early‐Type Galaxies from Cosmological Initial Conditions(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {710--720}, -primaryClass = {astro-ph}, -title = {{Formation of Early‐Type Galaxies from Cosmological Initial Conditions}}, -url = {http://stacks.iop.org/0004-637X/658/i=2/a=710}, -volume = {658}, -year = {2007} -} -@article{Negrello2014, -abstract = {We report on deep near-infrared observations obtained with the Wide Field Camera-3 (WFC3) onboard the Hubble Space Telescope (HST) of the first five confirmed gravitational lensing events discovered by the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We succeed in disentangling the background galaxy from the lens to gain separate photometry of the two components. The HST data allow us to significantly improve on previous constraints of the mass in stars of the lensed galaxy and to perform accurate lens modelling of these systems, as described in the accompanying paper by Dye et al. We fit the spectral energy distributions of the background sources from near-IR to millimetre wavelengths and use the magnification factors estimated by Dye et al. to derive the intrinsic properties of the lensed galaxies. We find these galaxies to have star-formations rates (SFR) $\sim$ 400-2000 M⊙ yr-1, with $\sim$(6-25) × 1010 M⊙ of their baryonic mass already turned into stars. At these rates of star formation, all remaining molecular gas will be exhausted in less than $\sim$100 Myr, reaching a final mass in stars of a few 1011 M⊙. These galaxies are thus proto-ellipticals caught during their major episode of star formation, and observed at the peak epoch (z $\sim$ 1.5-3) of the cosmic star formation history of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1311.5898}, -author = {Negrello, M. and Hopwood, R. and Dye, S. and da Cunha, E. and Serjeant, S. and Fritz, J. and Rowlands, K. and Fleuren, S. and Bussmann, R. S. and Cooray, A. and Dannerbauer, H. and Gonzalez-Nuevo, J. and Lapi, A. and Omont, A. and Amber, S. and Auld, R. and Baes, M. and Buttiglione, S. and Cava, A. and Danese, L. and Dariush, A. and {De Zotti}, G. and Dunne, L. and Eales, S. and Ibar, E. and Ivison, R. J. and Kim, S. and Leeuw, L. and Maddox, S. and Michalowski, M. J. and Massardi, M. and Pascale, E. and Pohlen, M. and Rigby, E. and Smith, D. J.B. and Sutherland, W. and Temi, P. and Wardlow, J.}, -doi = {10.1093/mnras/stu413}, -eprint = {1311.5898}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: formation,Gravitational lensing: strong,Infrared: galaxies,Submillimetre: galaxies}, -number = {3}, -pages = {1999--2012}, -title = {{Herschel *-ATLAS: Deep HST/WFC3 imaging of strongly lensed submillimetre galaxies}}, -url = {http://arxiv.org/abs/1311.5898}, -volume = {440}, -year = {2014} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10^11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r_vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of $\sim$25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r_vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bailin, Steinmetz - 2005 - Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos(2).pdf:pdf}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Libeskind2014, -abstract = {We examine the angular infall pattern of subhaloes on to host haloes in the context of the large-scale structure. We find that this infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are found to be preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is effectively universal in the sense that it is always aligned with the axis of weakest collapse of the velocity shear tensor. It is the same shear tensor that dictates the structure of the cosmic web and hence the shear field emerges as the key factor that governs the local anisotropic pattern of structure formation. Since the small (sub-Mpc) scale is strongly correlated with the mid-range (∼10 Mpc) scale - a scale accessible by current surveys of peculiar velocities - it follows that findings presented here open a new window into the relation between the observed large-scale structure unveiled by current surveys of peculiar velocities and the preferential infall direction of the Local Group. This may shed light on the unexpected alignments of dwarf galaxies seen in the Local Group. {\textcopyright}2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1407.0394}, -author = {Libeskind, Noam I and Knebe, Alexander and Hoffman, Yehuda and Gottl{\"{o}}ber, Stefan}, -doi = {10.1093/mnras/stu1216}, -eprint = {1407.0394}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Large-scale structure of universe}, -number = {2}, -pages = {1274--1280}, -title = {{The universal nature of subhalo accretion}}, -volume = {443}, -year = {2014} -} -@article{Mendez-Abreu2010, -abstract = {(Abridged) The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were analyzed to derive the intrinsic shape of their bulges. We developed a new method to derive the intrinsic shape of bulges based on the geometrical relationships between the apparent and intrinsic shapes of bulges and disks. The equatorial ellipticity and intrinsic flattening of bulges were obtained from the length of the apparent major and minor semi-axes of the bulge, twist angle between the apparent major axis of the bulge and the galaxy line of nodes, and galaxy inclination. We found that the intrinsic shape is well constrained for a subsample of 115 bulges with favorable viewing angles. A large fraction of them is characterized by an elliptical section (B/A{\textless}0.9). This fraction is 33{\%}, 55{\%}, and 43{\%} if using their maximum, mean, or median equatorial ellipticity, respectively. Most are flattened along their polar axis (C{\textless}(A+B)/2). The distribution of triaxiality is strongly bimodal. This bimodality is driven by bulges with Sersic index n{\textgreater}2, or equivalently, by the bulges of galaxies with a bulge-to-total ratio B/T{\textgreater}0.3. In particular, bulges with n{\$}\backslash{\$}leq2 and with B/T{\$}\backslash{\$}leq0.3 show a larger fraction of oblate axisymmetric (or nearly axisymmetric) bulges, a smaller fraction of triaxial bulges, and fewer prolate axisymmetric (or nearly axisymmetric) bulges with respect to bulges with n{\textgreater}2 and with B/T{\textgreater}0.3, respectively. According to predictions of the numerical simulations of bulge formation, bulges with n{\$}\backslash{\$}leq2, which show a high fraction of oblate axisymmetric (or nearly axisymmetric) shapes and have B/T{\$}\backslash{\$}leq0.3, could be the result of dissipational minor mergers. Both major dissipational and dissipationless mergers seem to be required to explain the variety of shapes found for bulges with n{\textgreater}2 and B/T{\textgreater}0.3.}, -archivePrefix = {arXiv}, -arxivId = {1006.5449}, -author = {Mendez-Abreu, J and Simonneau, E and Aguerri, J A L and Corsini, E M}, -doi = {10.1051/0004-6361/201014130}, -eprint = {1006.5449}, -issn = {00046361}, -journal = {Astronomy and Astrophysics}, -keywords = {cD,galaxies: bulges,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: spiral,galaxies: statistics,galaxies: structure}, -pages = {A71}, -title = {{Structural properties of disk galaxies. II. Intrinsic shape of bulges}}, -url = {http://arxiv.org/abs/1006.5449%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201014130}, -volume = {521}, -year = {2010} -} -@article{Shockley1952, -abstract = {The statistics of the recombination of holes and electrons in semiconductors is analyzed on the basis of a model in which the recombination occurs through the mechanism of trapping. A trap is assumed to have an energy level in the energy gap so that its charge may have either of two values differing by one electronic charge. The dependence of lifetime of injected carriers upon initial conductivity and upon injected carrier density is discussed. {\textcopyright} 1952 The American Physical Society.}, -author = {Shockley, W. and Read, W. T.}, -doi = {10.1103/PhysRev.87.835}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shockley, Read - 1952 - Statistics of the recombinations of holes and electrons.pdf:pdf}, -issn = {0031899X}, -journal = {Physical Review}, -keywords = {Shockley1952}, -mendeley-tags = {Shockley1952}, -number = {5}, -pages = {835--842}, -title = {{Statistics of the recombinations of holes and electrons}}, -volume = {87}, -year = {1952} -} -@article{Woo2014, -abstract = {We investigate the roles of two classes of quenching mechanisms for central and satellite galaxies in the Sloan Digital Sky Survey (z < 0.075): those involving the halo and those involving the formation of a compact centre. For central galaxies with inner compactness $\Sigma$1 kpc $\sim$ 109-9.4M⊙ kpc-2, the quenched fraction fq is strongly correlated with $\Sigma$1 kpc with only weak halo mass Mh dependence. However, at higher and lower $\Sigma$1 kpc, specific star formation rate (sSFR) is a strong function of Mh and mostly independent of $\Sigma$1 kpc. In other words, $\Sigma$1 kpc $\sim$ 109-9.4M⊙ kpc-2 divides galaxies into those with high sSFR below and low sSFR above this range. In both the upper and lower regimes, increasing Mh shifts the entire sSFR distribution to lower sSFR without a qualitative change in shape. This is true even at fixed M*, but varying M* at fixed Mh adds no quenching information. Most of the quenched centrals with Mh > 1011.8M⊙ are dense ($\Sigma$1 kpc > 109M⊙ kpc-2), suggesting compaction-related quenching maintained by halo-related quenching. However, 21 per cent are diffuse, indicating only halo quenching. For satellite galaxies in the outskirts of haloes, quenching is a strong function of compactness and a weak function of host Mh. In the inner halo, Mh dominates quenching, with $\sim$90 per cent of the satellites being quenched once Mh > 1013M⊙. This regional effect is greatest for the least massive satellites. As demonstrated via semi-analytic modelling with simple prescriptions for quenching, the observed correlations can be explained if quenching due to central compactness is rapid while quenching due to halo mass is slow.}, -archivePrefix = {arXiv}, -arxivId = {1406.5372}, -author = {Woo, Joanna and Dekel, Avishai and Faber, S. M. and Koo, David C.}, -doi = {10.1093/mnras/stu2755}, -eprint = {1406.5372}, -isbn = {0792388801}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: general,Galaxies: groups: general,Galaxies: haloes,Galaxies: star formation,Galaxies: structure}, -month = {mar}, -number = {1}, -pages = {237--251}, -title = {{Two conditions for galaxy quenching: Compact centres and massive haloes}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.448..237W}, -volume = {448}, -year = {2015} -} -@article{Morningstar2019, -abstract = {We present a machine learning method for the reconstruction of the undistorted images of background sources in strongly lensed systems. This method treats the source as a pixelated image and utilizes the Recurrent Inference Machine (RIM) to iteratively reconstruct the background source given a lens model. Our architecture learns to minimize the likelihood of the model parameters (source pixels) given the data using the physical forward model (ray tracing simulations) while implicitly learning the prior of the source structure from the training data. This results in better performance compared to linear inversion methods, where the prior information is limited to the 2-point covariance of the source pixels approximated with a Gaussian form, and often specified in a relatively arbitrary manner. We combine our source reconstruction network with a convolutional neural network that predicts the parameters of the mass distribution in the lensing galaxies directly from telescope images, allowing a fully automated reconstruction of the background source images and the foreground mass distribution.}, -archivePrefix = {arXiv}, -arxivId = {1901.01359}, -author = {Morningstar, Warren R and Levasseur, Laurence Perreault and Hezaveh, Yashar D and Blandford, Roger and Marshall, Phil and Putzky, Patrick and Rueter, Thomas D and Wechsler, Risa and Welling, Max}, -doi = {10.3847/1538-4357/ab35d7}, -eprint = {1901.01359}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {14}, -title = {{Data-driven Reconstruction of Gravitationally Lensed Galaxies Using Recurrent Inference Machines}}, -url = {http://arxiv.org/abs/1901.01359}, -volume = {883}, -year = {2019} -} -@article{Jin2017, -abstract = {We report the results from a recent 133 ks XMM-Newton observation of a highly super-Eddington narrow-line Type-1 QSO RX J0439.6-5311. This source has one of the steepest AGN hard X-ray slopes, in addition to a prominent and smooth soft X-ray excess. Strong variations are found throughout the 0.3 to 10 keV energy range on all time-scales covered by the observation, with the soft excess mainly showing low frequency variations below 0.1 mHz while the hard X-rays show stronger variability at higher frequencies. We perform a full set of spectral-timing analysis on the X-ray data, including a simultaneous modelling of the time-average spectra, frequency-dependent RMS and covariance spectra, lag-frequency and lag-energy spectra. Especially, we find a significant time-lag signal in the low frequency band, which indicates that the soft X-rays lead the hard by {\$}\backslashsim{\$}4 ks, with a broad continuum-like profile in the lag spectrum. Our analysis strongly supports the model where the soft X-ray excess is dominated by a separate low temperature, optically thick Comptonisation component rather than relativistic reflection or a jet. This soft X-ray emitting region is several tens or hundreds of {\$}R{\_}{\{}g{\}}{\$} away from the hot corona emitting hard X-rays, and is probably associated with a geometrically thick (`puffed-up') inner disc region.}, -archivePrefix = {arXiv}, -arxivId = {1703.07118}, -author = {Jin, Chichuan and Done, Chris and Ward, Martin}, -doi = {10.1093/mnras/stx718}, -eprint = {1703.07118}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {accretion,accretion discs - galaxies,active - galaxies,nuclei}, -number = {3}, -pages = {3663--3681}, -title = {{Super-Eddington QSO RX J0439.6−5311 – I. Origin of the soft X-ray excess and structure of the inner accretion flow}}, -url = {http://arxiv.org/abs/1703.07118%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx718}, -volume = {468}, -year = {2017} -} -@article{Nolan2011, -abstract = {We present a catalog of high-energy gamma-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi), during the first 11 months of the science phase of the mission, which began on 2008 August 4. The First Fermi-LAT catalog (1FGL) contains 1451 sources detected and characterized in the 100MeV to 100GeV range. Source detection was based on the average flux over the 11 month period, and the threshold likelihood Test Statistic is 25, corresponding to a significance of just over 4$\sigma$. The 1FGL catalog includes source location regions, defined in terms of elliptical fits to the 95% confidence regions and power-law spectral fits as well as flux measurements in five energy bands for each source. In addition, monthly light curves are provided. Using a protocol defined before launch we have tested for several populations of gamma-ray sources among the sources in the catalog. For individual LAT-detected sources we provide firm identifications or plausible associations with sources in other astronomical catalogs. Identifications are based on correlated variability with counterparts at other wavelengths, or on spin or orbital periodicity. For the catalogs and association criteria that we have selected, 630 of the sources are unassociated. Care was taken to characterize the sensitivity of the results to the model of interstellar diffuse gamma-ray emission used to model the bright foreground, with the result that 161 sources at low Galactic latitudes and toward bright local interstellar clouds are flagged as having properties that are strongly dependent on the model or as potentially being due to incorrectly modeled structure in the Galactic diffuse emission. {\textcopyright} 2010. The American Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1002.2280}, -author = {Abdo, A. A. and Ackermann, M. and Ajello, M. and Allafort, A. and Antolini, E. and Atwood, W. B. and Axelsson, M. and Baldini, L. and Ballet, J. and Barbiellini, G. and Bastieri, D. and Baughman, B. M. and Bechtol, K. and Bellazzini, R. and Belli, F. and Berenji, B. and Bisello, D. and Blandford, R. D. and Bloom, E. D. and Bonamente, E. and Bonnell, J. and Borgland, A. W. and Bouvier, A. and Bregeon, J. and Brez, A. and Brigida, M. and Bruel, P. and Burnett, T. H. and Busetto, G. and Buson, S. and Caliandro, G. A. and Cameron, R. A. and Campana, R. and Canadas, B. and Caraveo, P. A. and Carrigan, S. and Casandjian, J. M. and Cavazzuti, E. and Ceccanti, M. and Cecchi, C. and {\c{C}}elik, {\"{O}} and Charles, E. and Chekhtman, A. and Cheung, C. C. and Chiang, J. and Cillis, A. N. and Ciprini, S. and Claus, R. and Cohen-Tanugi, J. and Conrad, J. and Corbet, R. and Davis, D. S. and Deklotz, M. and {Den Hartog}, P. R. and Dermer, C. D. and {De Angelis}, A. and {De Luca}, A. and {De Palma}, F. and Digel, S. W. and Dormody, M. and {Do Couto E Silva}, E. and Drell, P. S. and Dubois, R. and Dumora, D. and Fabiani, D. and Farnier, C. and Favuzzi, C. and Fegan, S. J. and Ferrara, E. C. and Focke, W. B. and Fortin, P. and Frailis, M. and Fukazawa, Y. and Funk, S. and Fusco, P. and Gargano, F. and Gasparrini, D. and Gehrels, N. and Germani, S. and Giavitto, G. and Giebels, B. and Giglietto, N. and Giommi, P. and Giordano, F. and Giroletti, M. and Glanzman, T. and Godfrey, G. and Grenier, I. A. and Grondin, M. H. and Grove, J. E. and Guillemot, L. and Guiriec, S. and Gustafsson, M. and Hadasch, D. and Hanabata, Y. and Harding, A. K. and Hayashida, M. and Hays, E. and Healey, S. E. and Hill, A. B. and Horan, D. and Hughes, R. E. and Iafrate, G. and J{\'{o}}hannesson, G. and Johnson, A. S. and Johnson, R. P. and Johnson, T. J. and Johnson, W. N. and Kamae, T. and Katagiri, H. and Kataoka, J. and Kawai, N. and Kerr, M. and Kn{\"{o}}dlseder, J. and Kocevski, D. and Kuss, M. and Lande, J. and Landriu, D. and Latronico, L. and Lee, S. H. and Lemoine-Goumard, M. and Lionetto, A. M. and {Llena Garde}, M. and Longo, F. and Loparco, F. and Lott, B. and Lovellette, M. N. and Lubrano, P. and Madejski, G. M. and Makeev, A. and Marangelli, B. and Marelli, M. and Massaro, E. and Mazziotta, M. N. and McConville, W. and McEnery, J. E. and Michelson, P. F. and Minuti, M. and Mitthumsiri, W. and Mizuno, T. and Moiseev, A. A. and Mongelli, M. and Monte, C. and Monzani, M. E. and Moretti, E. and Morselli, A. and Moskalenko, I. V. and Murgia, S. and Nakajima, H. and Nakamori, T. and Naumann-Godo, M. and Nolan, P. L. and Norris, J. P. and Nuss, E. and Ohno, M. and Ohsugi, T. and Omodei, N. and Orlando, E. and Ormes, J. F. and Ozaki, M. and Paccagnella, A. and Paneque, D. and Panetta, J. H. and Parent, D. and Pelassa, V. and Pepe, M. and Pesce-Rollins, M. and Pinchera, M. and Piron, F. and Porter, T. A. and Poupard, L. and Rain{\`{o}}, S. and Rando, R. and Ray, P. S. and Razzano, M. and Razzaque, S. and Rea, N. and Reimer, A. and Reimer, O. and Reposeur, T. and Ripken, J. and Ritz, S. and Rochester, L. S. and Rodriguez, A. Y. and Romani, R. W. and Roth, M. and Sadrozinski, H. F.W. and Salvetti, D. and Sanchez, D. and Sander, A. and {Saz Parkinson}, P. M. and Scargle, J. D. and Schalk, T. L. and Scolieri, G. and Sgr{\`{o}}, C. and Shaw, M. S. and Siskind, E. J. and Smith, D. A. and Smith, P. D. and Spandre, G. and Spinelli, P. and Starck, J. L. and Stephens, T. E. and Striani, E. and Strickman, M. S. and Strong, A. W. and Suson, D. J. and Tajima, H. and Takahashi, H. and Takahashi, T. and Tanaka, T. and Thayer, J. B. and Thayer, J. G. and Thompson, D. J. and Tibaldo, L. and Tibolla, O. and Tinebra, F. and Torres, D. F. and Tosti, G. and Tramacere, A. and Uchiyama, Y. and Usher, T. L. and {Van Etten}, A. and Vasileiou, V. and Vilchez, N. and Vitale, V. and Waite, A. P. and Wallace, E. and Wang, P. and Watters, K. and Winer, B. L. and Wood, K. S. and Yang, Z. and Ylinen, T. and Ziegler, M.}, -doi = {10.1088/0067-0049/188/2/405}, -eprint = {1002.2280}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {Catalogs,Gamma rays: general}, -number = {2}, -pages = {405--436}, -title = {{Fermi large area telescope first source catalog}}, -url = {http://ads.nao.ac.jp/abs/2012ApJS..199...31N}, -volume = {188}, -year = {2010} -} -@article{Shao2016, -abstract = {The spatial distribution of the satellite populations of the Milky Way and Andromeda are puzzling in that they are nearly perpendicular to the discs of their central galaxies. To understand the origin of such configurations we study the alignment of the central galaxy, satellite system and dark matter halo in the largest of the 'Evolution and Assembly of GaLaxies and their Environments' (eagle) simulation. We find that centrals and their satellite systems tend to be well aligned with their haloes, with a median misalignment angle of 33° in both cases. While the centrals are better aligned with the inner 10 kpc halo, the satellite systems are better aligned with the entire halo indicating that satellites preferentially trace the outer halo. The central-satellite alignment is weak (median misalignment angle of 52°) and we find that around 20 per cent of systems have a misalignment angle larger than 78°, which is the value for the Milky Way. The central-satellite alignment is a consequence of the tendency of both components to align with the dark matter halo. As a consequence, when the central is parallel to the satellite system, it also tends to be parallel to the halo. In contrast, if the central is perpendicular to the satellite system, as in the case of the Milky Way and Andromeda, then the central-halo alignment is much weaker. Dispersion-dominated (spheroidal) centrals have a stronger alignment with both their halo and their satellites than rotation-dominated (disc) centrals. We also found that the halo, the central galaxy and the satellite system tend to be aligned with the surrounding large-scale distribution of matter, with the halo being the better aligned of the three.}, -archivePrefix = {arXiv}, -arxivId = {1605.01728}, -author = {Shao, Shi and Cautun, Marius and Frenk, Carlos S. and Gao, Liang and Crain, Robert A. and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stw1247}, -eprint = {1605.01728}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Shao et al. - 2016 - Alignments between galaxies, satellite systems and haloes.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: haloes,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3772--3783}, -title = {{Alignments between galaxies, satellite systems and haloes}}, -volume = {460}, -year = {2016} -} -@article{Powell2020, -abstract = {We present a new gravitational lens modelling technique designed to model high-resolution interferometric observations with large numbers of visibilities without the need to pre-average the data in time or frequency. We demonstrate the accuracy of the method using validation tests on mock observations. Using small data sets with ∼103 visibilities, we first compare our approach with the more traditional direct Fourier transform (DFT) implementation and direct linear solver. Our tests indicate that our source inversion is indistinguishable from that of the DFT. Our method also infers lens parameters to within 1 to 2 per cent of both the ground truth and DFT, given sufficiently high signal-to-noise ratio (SNR). When the SNR is as low as 5, both approaches lead to errors of several tens of per cent in the lens parameters and a severely disrupted source structure, indicating that this is related to the SNR and choice of priors rather than the modelling technique itself. We then analyze a large data set with ∼108 visibilities and a SNR matching real global Very Long Baseline Interferometry observations of the gravitational lens system MG J0751+2716. The size of the data is such that it cannot be modelled with traditional implementations. Using our novel technique, we find that we can infer the lens parameters and the source brightness distribution, respectively, with an RMS error of 0.25 and 0.97 per cent relative to the ground truth.}, -archivePrefix = {arXiv}, -arxivId = {2005.03609}, -author = {Powell, Devon and Vegetti, Simona and McKean, John P and Spingola, Cristiana and Rizzo, Francesca and Stacey, Hannah R}, -doi = {10.1093/mnras/staa2740}, -eprint = {2005.03609}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Powell et al. - 2020 - A novel approach to visibility-space modelling of interferometric gravitational lens observations at high angular.pdf:pdf}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {data analysis,gravitational lensing,high angular resolution,image,methods,processing,strong,techniques}, -number = {October}, -pages = {515--530}, -title = {{A novel approach to visibility-space modelling of interferometric gravitational lens observations at high angular resolution}}, -volume = {501}, -year = {2020} -} -@article{Humphrey2012, -abstract = {The Elliptical Isolated X-ray (ElIXr) Galaxy Survey is a volume-limited ({\textless}110Mpc) study of optically selected, isolated, L * elliptical galaxies to provide an X-ray census of galaxy-scale (virial mass, M vir ≲ 1013 M ⊙) objects and identify candidates for detailed hydrostatic mass modeling. In this paper, we present a Chandra and XMM study of one such candidate, NGC 1521, and constrain its distribution of dark and baryonic matter. We find a morphologically relaxed hot gas halo, extending almost to R 500, that is well described by hydrostatic models similar to the benchmark, baryonically closed, Milky Way mass elliptical galaxy NGC 720. We obtain good constraints on the enclosed gravitating mass (M 500 = [3.8 ± 1.0] × 1012 M ⊙, slightly higher than NGC 720) and baryon fraction (f b, 500 = 0.13 ± 0.03). We confirm at 8.2$\sigma$ the presence of a dark matter (DM) halo consistent with $\Lambda$CDM. Assuming a Navarro-Frenk-White DM profile, our self-consistent, physical model enables meaningful constraints beyond R 500, revealing that most of the baryons are in the hot gas. Within the virial radius, fb is consistent with the cosmic mean, suggesting that the predicted massive, quasi-hydrostatic gas halos may be more common than previously thought. We confirm that the DM and stars conspire to produce an approximately power-law total mass profile ($\rho$totr -$\alpha$) that follows the recently discovered scaling relation between $\alpha$ and optical effective radius. Our conclusions are insensitive to modest, observationally motivated, deviations from hydrostatic equilibrium. Finally, after correcting for the enclosed gas fraction, the entropy profile is close to the self-similar prediction of gravitational structure formation simulations, as observed in massive galaxy clusters. {\textcopyright}2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1204.3095}, -author = {Humphrey, Philip J and Buote, David A and O'Sullivan, Ewan and Ponman, Trevor J}, -doi = {10.1088/0004-637X/755/2/166}, -eprint = {1204.3095}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {X-rays: galaxies,cD,dark matter,galaxies: ISM,galaxies: elliptical and lenticular,galaxies: formation,galaxies: fundamental parameters,galaxies: individual (NGC 1521)}, -number = {2}, -pages = {1--18}, -title = {{The ElIXr galaxy survey. II. baryons and dark matter in an isolated elliptical galaxy}}, -volume = {755}, -year = {2012} -} -@article{Shirazi2013, -abstract = {We present an analysis of near-infrared integral field unit spectroscopy of the 8 o'clock arc, a gravitationally lensed Lyman break galaxy, taken with SINFONI. We explore the shape of the spatially resolved H$\beta$ profile and demonstrate that we can decompose it into three components that partially overlap (spatially) but are distinguishable when we include dynamical information. We use existing B and H imaging from the Hubble Space Telescope to construct a rigorous lens model using a Bayesian grid-based lens modelling technique. We apply this lens model to the SINFONI data cube to construct the de-lensed H$\beta$ line-flux velocity and velocity dispersion maps of the galaxy. We find that the 8 o'clock arc has a complex velocity field that is not simply explained by a single rotating disc. The H$\beta$ profile of the galaxy shows a blueshifted wing suggesting gas outflows of $\sim$200 km s-1. We confirm that the 8 o'clock arc lies on the stellar mass-oxygen abundance-star formation rate plane found locally, but it has nevertheless significantly different gas surface density (a factor of 2-4 higher) and electron density in the ionized gas (five times higher) from those in similar nearby galaxies, possibly indicating a higher density interstellar medium for this galaxy. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1306.6282}, -author = {Shirazi, M. and Vegetti, S. and Nesvadba, N. and Allam, S. and Brinchmann, J. and Tucker, D.}, -doi = {10.1093/mnras/stu316}, -eprint = {1306.6282}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: ISM,Galaxies: evolution,Galaxies: formation,Galaxies: high-redshift,Galaxies: kinematics and dynamics,Gravitational lensing: strong}, -number = {3}, -pages = {2201--2221}, -title = {{The physical nature of the 8 o'clock arc based on near-IR IFU spectroscopy with SINFONI}}, -volume = {440}, -year = {2014} -} -@article{Goulding2016a, -abstract = {Studies of the physical properties of local elliptical galaxies (e.g., gas temperatures, halo masses, stellar kinematics) are shedding new light on galaxy formation. Here we present the hot X-ray gas properties of 33 early-type systems within the MASSIVE galaxy survey sample that have archival Chandra X-ray observations. Through careful X-ray spectral modeling, we derive X-ray luminosities (L{\_}X) and plasma temperatures (T{\_}gas) for the diffuse gas components in these galaxies. We combine the MASSIVE sample with 41 galaxies from the ATLAS{\^{}}3D survey to investigate the X-ray and optical properties of a statistically significant sample of nearby early-type galaxies across a wide-range of environments. We deduce that all early-type galaxies (independent of galaxy mass and rotational support) follow a universal scaling law such that L{\_}X{\$\sim${}}T{\_}gas{\^{}}4.5. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, the wide-scale environment does not contribute to the intrinsic scatter ({\$\sim${}}0.5dex) within the scaling relation. We further demonstrate that the scatter in L{\_}X around both K-band luminosity (L{\_}K) and the galaxy stellar velocity dispersion is primarily driven by T{\_}gas, with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the origin of the gas directly to either the stellar mass or the galaxy potential. Indeed, our data require a steeper relation between L{\_}X, L{\_}K, and sigma{\_}e than predicted by standard mass-loss models. Finally, we find a statistically significant correlation between sigma{\_}e and T{\_}gas, suggesting that T{\_}gas is set by the galaxy potential inside the optical effective radius. We conclude that within the inner-most 10-30kpc region, early-types maintain pressure-supported hot gas, with a minimum T{\_}gas set by the virial temperature, but the majority show evidence for some additional heating.}, -archivePrefix = {arXiv}, -arxivId = {1604.01764}, -author = {Goulding, Andy D and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Bogdan, Akos and Nyland, Kristina and Blakeslee, John P and McConnell, Nicholas J and Thomas, Jens}, -doi = {10.3847/0004-637X/826/2/167}, -eprint = {1604.01764}, -issn = {0004-637X}, -title = {{The MASSIVE Survey IV.: The X-ray halos of the most massive early-type galaxies in the nearby Universe}}, -url = {http://arxiv.org/abs/1604.01764%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/826/2/167}, -year = {2016} -} -@article{Gadotti2008a, -abstract = {We have performed 2D bulge/bar/disc decompositions using g, r and i-band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for the bulge-to-total ratio than the global S{\'{e}}rsic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour-magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between the bulge S{\'{e}}rsic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass-size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass-size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs. {\textcopyright}2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0810.1953}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2008.14257.x}, -eprint = {0810.1953}, -isbn = {0372-9311 (Print)$\backslash$r0372-9311 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {1531--1552}, -pmid = {20063786}, -title = {{Structural properties of pseudo-bulges, classical bulges and elliptical galaxies: A Sloan Digital Sky Survey perspective}}, -url = {http://arxiv.org/abs/0810.1953%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2008.14257.x}, -volume = {393}, -year = {2009} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and $\backslash$nspectroscopic ESA cornerstone mission, currently scheduled for launch in$\backslash$nlate 2011. Its primary science drivers are the composition, formation$\backslash$nand evolution of the Galaxy. Gaia will not achieve its scientific$\backslash$nrequirements without detailed calibration and correction for radiation$\backslash$ndamage. Microscopic models of Gaia's CCDs are being developed to$\backslash$nsimulate the effect of radiation damage, charge trapping, which causes$\backslash$ncharge transfer inefficiency. The key to calculating the probability of$\backslash$na photoelectron being captured by a trap is the 3D electron density$\backslash$nwithin each CCD pixel. However, this has not been physically modelled$\backslash$nfor Gaia CCD pixels. In this paper, the first of a series, we motivate$\backslash$nthe need for such specialised 3D device modelling and outline how its$\backslash$nfuture results will fit into Gaia's overall radiation calibration$\backslash$nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -isbn = {0277-786X}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy III}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Irsic2017, -abstract = {We present new measurements of the free-streaming of warm dark matter (WDM) from Lyman-$\alpha$ flux-power spectra. We use data from the medium resolution, intermediate redshift XQ-100 sample observed with the X-shooter spectrograph (z=3-4.2) and the high-resolution, high-redshift sample used in Viel et al. (2013) obtained with the HIRES/MIKE spectrographs (z=4.2-5.4). Based on further improved modelling of the dependence of the Lyman-$\alpha$ flux-power spectrum on the free-streaming of dark matter, cosmological parameters, as well as the thermal history of the intergalactic medium (IGM) with hydrodynamical simulations, we obtain the following limits, expressed as the equivalent mass of thermal relic WDM particles. The XQ-100 flux power spectrum alone gives a lower limit of 1.4 keV, the re-analysis of the HIRES/MIKE sample gives 4.1 keV while the combined analysis gives our best and significantly strengthened lower limit of 5.3 keV (all 2$\sigma$ C.L.). The further improvement in the joint analysis is partly due to the fact that the two data sets have different degeneracies between astrophysical and cosmological parameters that are broken when the data sets are combined, and more importantly on chosen priors on the thermal evolution. These results all assume that the temperature evolution of the IGM can be modeled as a power law in redshift. Allowing for a nonsmooth evolution of the temperature of the IGM with sudden temperature changes of up to 5000 K reduces the lower limit for the combined analysis to 3.5 keV. A WDM with smaller thermal relic masses would require, however, a sudden temperature jump of 5000 K or more in the narrow redshift interval z=4.6-4.8, in disagreement with observations of the thermal history based on high-resolution resolution Lyman-$\alpha$ forest data and expectations for photo-heating and cooling in the low density IGM at these redshifts.}, -archivePrefix = {arXiv}, -arxivId = {1702.01764}, -author = {Ir{\v{s}}i{\v{c}}, Vid and Viel, Matteo and Haehnelt, Martin G and Bolton, James S and Cristiani, Stefano and Becker, George D and D'Odorico, Valentina and Cupani, Guido and Kim, Tae Sun and Berg, Trystyn A M and L{\'{o}}pez, Sebastian and Ellison, Sara and Christensen, Lise and Denney, Kelly D and Worseck, G{\'{a}}bor}, -doi = {10.1103/PhysRevD.96.023522}, -eprint = {1702.01764}, -issn = {24700029}, -journal = {Physical Review D}, -number = {2}, -pages = {1--15}, -title = {{New constraints on the free-streaming of warm dark matter from intermediate and small scale Lyman- $\alpha$ forest data}}, -volume = {96}, -year = {2017} -} -@article{Cappellari2002, -abstract = {We describe a simple, efficient, robust and fully automatic algorithm for the determination of a multi-Gaussian expansion (MGE) fit to galaxy images, to be used as a parametrization for the galaxy stellar surface brightness. In most cases the least-squares solution found by this method essentially corresponds to the minimax, constant relative error, MGE approximation of the galaxy surface brightness, with the chosen number of Gaussians. The algorithm is well suited to be used with multiple-resolution images (e.g. Hubble Space Telescope (HST) and ground-based images). It works orders of magnitude faster and is more accurate than currently available methods. An alternative, more computing-intensive, fully linear algorithm that is guaranteed to converge to the smallest X2 solution is also discussed. Examples of MGE fits are presented for objects with HST or ground-based photometry, including galaxies with significant isophote twist.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0201430}, -author = {Cappellari, Michelle}, -doi = {10.1046/j.1365-8711.2002.05412.x}, -eprint = {0201430}, -file = {:C\:/Users/Jammy/Documents/Papers/GaussianLinearModels/Cappelari2002MGE.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Galaxies: kinematics and dynamics,Galaxies: photometry,Galaxies: structure,Stellar dynamics,Techniques: image processing}, -number = {2}, -pages = {400--410}, -primaryClass = {astro-ph}, -title = {{Efficient multi-Gaussian expansion of galaxies}}, -volume = {333}, -year = {2002} -} -@article{Minka2009, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture models is not well captured by factor graphs unless the entire mixture is represented by one factor, because the message equations have a containment structure. Gates capture this containment structure graphically, allowing both the independences and the message-passing equations for a model to be readily visualized. Different variational approximations for mixture models can be understood as different ways of drawing the gates in a model. We present general equations for expectation propagation and variational message passing in the presence of gates.}, -author = {Minka, Tom and Winn, John}, -doi = {10.5790/hongkong/9789888083091.003.0088}, -isbn = {9781605609492}, -issn = {0018702X}, -journal = {Advances in Neural Information Processing Systems 21 - Proceedings of the 2008 Conference}, -pages = {1073--1080}, -title = {{Gates}}, -year = {2009} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work conducted to interpret this phenomenon has found that it is due to the non-spherical nature of dark matter halos. However, most studies overpredict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shapes of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations where satellite galaxies without associated subhalos ("orphan galaxies") are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region. {\textcopyright}2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W P and Kang, X and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%7B%5C%25%7D5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem%7B%5C&%7Dsid=IOPP%7B%5C%25%7D3Ajnl%7B%5C_%7Dref%7B%5C&%7Dspage=305%7B%5C&%7Dtitle=ArA%7B%5C&%7Dvolume=5%7B%5C&%7Ddate=1969%7B%5C&%7Dv%7B%5C}, -volume = {786}, -year = {2014} -} -@article{Harvey2015, -abstract = {Collisions between galaxy clusters provide a test of the nongravitational forces acting on dark matter. Dark matter's lack of deceleration in the "bullet cluster" collision constrained its self-interaction cross section $\sigma$DM/m {\textless} 1.25 square centimeters per gram (cm2/g) [68{\%} confidence limit (CL)] ($\sigma$DM, self-interaction cross section; m, unit mass of dark matter) for long-ranged forces. Using the Chandra and Hubble Space Telescopes, we have now observed 72 collisions, including both major and minor mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6s significance. The position of the dark mass has remained closely aligned within 5.8 T 8.2 kiloparsecs of associated stars, implying a self-interaction cross section $\sigma$DM/m {\textless} 0.47 cm2/g (95{\%} CL) and disfavoring some proposed extensions to the standard model.}, -archivePrefix = {arXiv}, -arxivId = {1503.07675}, -author = {Harvey, David and Massey, Richard and Kitching, Thomas and Taylor, Andy and Tittley, Eric}, -doi = {10.1126/science.1261381}, -eprint = {1503.07675}, -issn = {10959203}, -journal = {Science}, -number = {6229}, -pages = {1462--1465}, -pmid = {25814581}, -title = {{The nongravitational interactions of dark matter in colliding galaxy clusters}}, -volume = {347}, -year = {2015} -} -@article{Schombert2013, -abstract = {Surface photometry of 311 ellipticals from the 2MASS imaging database is analyzed with respect to the two most common fitting functions: the r 1/4 law and the S{\'{e}}rsic r 1/n model. The advantages and disadvantages of each fitting function are examined. In particular, the r 1/4 law performs well in the middle regions, but is inadequate for the core (inner 5 kpc) and the outer regions (beyond the half-light radius) which do not have r 1/4 shapes. It is found that the S{\'{e}}rsic r 1/n model produces good fits to the core regions of ellipticals (r3.0.CO;2-L}, -file = {:C\:/Users/Jammy/Documents/Papers/GaussianLinearModels/brodejong1997fnnlks.pdf:pdf}, -issn = {08869383}, -journal = {Journal of Chemometrics}, -keywords = {Multiway,NNLS,Non-negativity,PARAFAC}, -number = {5}, -pages = {393--401}, -title = {{A fast non-negativity-constrained least squares algorithm}}, -volume = {11}, -year = {1997} -} -@article{Yang2006a, -abstract = {We use galaxy groups selected from the Sloan Digital Sky Survey to examine the alignment between the orientation of the central galaxy (defined as the brightest group member) and the distribution of satellite galaxies. By construction, we therefore only address the alignment on scales smaller than the halo virial radius. We find a highly significant alignment of satellites with the major axis of their central galaxy. This is in qualitative agreement with the recent study of Brainerd (2005), but inconsistent with several previous studies who detected a preferential minor axis alignment. The alignment strength in our sample is strongest between red central galaxies and red satellites. On the contrary, the satellite distribution in systems with a blue central galaxy is consistent with isotropic. We also find that the alignment strength is stronger in more massive haloes and at smaller projected radii from the central galaxy. In addition, there is a weak indication that fainter (relative to the central galaxy) satellites are more strongly aligned. We present a detailed comparison with previous studies, and discuss the implications of our findings for galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0601040}, -author = {Yang, Xiaohu and {Van Den Bosch}, Frank C and Mo, H J and Mao, Shude and Kang, Xi and Weinmann, Simone M and Guo, Yicheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2006.10373.x}, -eprint = {0601040}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {3}, -pages = {1293--1302}, -primaryClass = {astro-ph}, -title = {{The alignment between the distribution of satellites and the orientation of their central galaxy}}, -volume = {369}, -year = {2006} -} -@article{Morganti2013, -abstract = {NGC 4494 is one of several intermediate-luminosity elliptical galaxies inferred to have an unusually diffuse dark matter halo. We use the $\chi$2-made-to-measure particle code nmagic to construct axisymmetric models of NGC 4494 from photometric and various kinematic data. The extended kinematics include light spectra in multiple slitlets out to 3.5Re, and hundreds of planetary nebula velocities out to ≃7Re, thus allowing us to probe the dark matter content and orbital structure in the halo. We use Monte Carlo simulations to estimate confidence boundaries for the halo parameters, given our data and modelling set-up. We find that the true potential of the dark matter halo is recovered within $\Delta$G (merit function) ≲ 26 ($\Delta$$\chi$2 ≲ 59) at the 70 per cent confidence level (CL), and within $\Delta$G ≲ 32 ($\Delta$$\chi$2 ≲ 70) at the 90 per cent CL. These numbers are much larger than the usually assumed $\Delta$$\chi$2  2.3 (4.6) for the 70 per cent (90 per cent) CL for two free parameters, perhaps case dependent, but calling into question the general validity of the standard assumptions used for halo and black hole mass determinations. The best-fitting models for NGC 4494 have a dark matter fraction of about 0.6 ± 0.1 at 5Re (70 per cent CL) and are embedded in a dark matter halo with circular velocity ∼200 km s-1. The total circular velocity curve (CVC) is approximately flat at vc  220 km s-1 outside ∼0.5Re. The orbital anisotropy of the stars is moderately radial. These results are independent of the assumed inclination of the galaxy, and edge-on models are preferred. Comparing with the haloes of NGC 3379 and NGC 4697, whose velocity dispersion profiles also decrease rapidly from the centre outwards, the outer CVCs and dark matter haloes are quite similar. NGC 4494 shows a particularly high dark matter fraction inside ∼ 3Re, and a strong concentration of baryons in the centre. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1303.2688}, -author = {Morganti, Lucia and Gerhard, Ortwin and Coccato, Lodovico and Martinez-valpuesta, Inma and Arnaboldi, Magda}, -doi = {10.1093/mnras/stt442}, -eprint = {1303.2688}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Morganti et al. - 2013 - Elliptical galaxies with rapidly decreasing velocity dispersion profiles Nmagic models and dark halo paramet(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular, cD,Galaxies: haloes,Galaxies: individual: NGC 4494,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {4}, -pages = {3570--3588}, -title = {{Elliptical galaxies with rapidly decreasing velocity dispersion profiles: Nmagic models and dark halo parameter estimates for NGC 4494}}, -volume = {431}, -year = {2013} -} -@article{Guo:2008aa, -author = {Guo, Q and White, S.$\sim$D.$\sim$M.}, -journal = {\mnras}, -month = {feb}, -pages = {2--10}, -title = {{Galaxy growth in the concordance {$\Lambda$}CDM cosmology}}, -volume = {384}, -year = {2008} -} -@article{Buitrago2008, -abstract = {We measure the sizes of 82 massive (M>10^11 M_sun) galaxies at 1.72, confirming the extreme compactness of these galaxies. We split our sample into disk-like (n<2) and spheroid-like (n>2) galaxies based on their Sersic indices, and find that at a given stellar mass disk-like galaxies at z$\sim$2.3 are a factor of 2.6+/-0.3 smaller than present day equal mass systems, and spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than comparatively massive elliptical galaxies today. At z>2 our results are compatible with both a leveling off, or a mild evolution in size. Furthermore, the high density ($\sim$2x10^10 M_sun kpc^-3) of massive galaxies at these redshifts, which are similar to present day globular clusters, possibly makes any further evolution in sizes beyond z=3 unlikely.}, -archivePrefix = {arXiv}, -arxivId = {0807.4141}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Conselice, Christopher J. and Bouwens, Rychard J. and Dickinson, Mark and Yan, Haojing}, -doi = {10.1086/592836}, -eprint = {0807.4141}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Buitrago et al. - 2008 - Size Evolution of the Most Massive Galaxies at 1.7 z 3 from GOODS NICMOS Survey Imaging.pdf:pdf}, -isbn = {1005-0302}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L61--L64}, -title = {{ Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging }}, -url = {http://arxiv.org/abs/0807.4141%0Ahttp://dx.doi.org/10.1086/592836}, -volume = {687}, -year = {2008} -} -@article{Ding2018a, -abstract = {Strong gravitational lenses with measured time delay are a powerful tool to measure cosmological parameters, especially the Hubble constant ({\$}H{\_}0{\$}). Recent studies show by combining just three multiply-imaged AGN systems, one can determine {\$}H{\_}0{\$} down to 3{\%} precision. Furthermore, the number of time-delay lens is growing rapidly, enabling the determination of {\$}H{\_}0{\$} to 1{\%} precision in the near future. However, it is important to ensure that systematic errors and biases remain subdominant. For this purpose, challenges with simulated datasets are a key component. Following the experience of the past challenge on time delay, where it was shown that time delays can be measured precisely and accurately at the sub-percent level, we now present the "Time Delay Lens Modeling Challenge" (TDLMC). The goal of TDLMC is to assess the present capabilities of lens modeling codes and assumptions and test the level of accuracy of inferred cosmological parameters given realistic mock datasets. We invite scientists to model a set of simulated HST observations of 50 mock lens systems. The systems are organized in rungs, with the complexity and realism increasing going up the ladder. The goal of the challenge is to infer {\$}H{\_}0{\$} for each rung, given the HST images, the time delay, and a stellar velocity dispersion of the deflector, for a fixed background cosmology. The TDLMC challenge will start with the mock data release on 2018 January 8th. The deadline for blind submission is different for each rung. The deadline for Rung0-1 is 2018 Sept. 8; the deadline for Rung2 is 2019 Apr. 8 and the one for Rung3 is 2019 Sept. 8. This first paper gives an overview of the challenge including the data design, and a set of metrics to quantify the modeling performance and challenge details. After the deadline, the results of the challenge will be presented in a companion paper with all challenge participants as co-authors.}, -archivePrefix = {arXiv}, -arxivId = {1801.01506}, -author = {Ding, Xuheng and Treu, Tommaso and Shajib, Anowar J and Xu, Dandan and Chen, Geoff C -F. and More, Anupreeta and Despali, Giulia and Frigo, Matteo and Fassnacht, Christopher D and Gilman, Daniel and Hilbert, Stefan and Marshall, Philip J and Sluse, Dominique and Vegetti, Simona}, -eprint = {1801.01506}, -title = {{Time Delay Lens Modeling Challenge: I. Experimental Design}}, -url = {http://arxiv.org/abs/1801.01506}, -year = {2018} -} -@article{Leauthaud2017, -abstract = {We present high signal-to-noise galaxy-galaxy lensing measurements of the Baryon Oscillation Spectroscopic Survey constant mass (CMASS) sample using 250 deg2 of weak-lensing data from Canada-France-Hawaii Telescope Lensing Survey and Canada-France-Hawaii Telescope Stripe 82 Survey. We compare this signal with predictions from mock catalogues trained to match observables including the stellar mass function and the projected and twodimensional clustering of CMASS. We show that the clustering of CMASS, together with standard models of the galaxy-halo connection, robustly predicts a lensing signal that is 20-40 per cent larger than observed. Detailed tests show that our results are robust to a variety of systematic effects. Lowering the value of S8 = $\sigma$8 √ $\Omega$m/0.3 compared to Planck Collaboration XIII reconciles the lensing with clustering. However, given the scale of our measurement (r < 10 h-1 Mpc), other effects may also be at play and need to be taken into consideration. We explore the impact of baryon physics, assembly bias, massive neutrinos and modifications to general relativity on $\Delta$$\Sigma$ and show that several of these effects may be non-negligible given the precision of our measurement. Disentangling cosmological effects from the details of the galaxy-halo connection, the effect of baryons, and massive neutrinos, is the next challenge facing joint lensing and clustering analyses. This is especially true in the context of large galaxy samples from Baryon Acoustic Oscillation surveys with precise measurements but complex selection functions.}, -archivePrefix = {arXiv}, -arxivId = {1611.08606}, -author = {Leauthaud, Alexie and Saito, Shun and Hilbert, Stefan and Barreira, Alexandre and More, Surhud and White, Martin and Alam, Shadab and Behroozi, Peter and Bundy, Kevin and Coupon, Jean and Erben, Thomas and Heymans, Catherine and Hildebrandt, Hendrik and Mandelbaum, Rachel and Miller, Lance and Moraes, Bruno and Pereira, Maria E.S. and Rodr{\'{i}}guez-Torres, Sergio A. and Schmidt, Fabian and Shan, Huan Yuan and Viel, Matteo and Villaescusa-Navarro, Francisco}, -doi = {10.1093/mnras/stx258}, -eprint = {1611.08606}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Leauthaud et al. - 2017 - Lensing is low Cosmology, galaxy formation or new physics(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Gravitational lensing: weak,Large-scale structure of Universe}, -number = {3}, -pages = {3024--3047}, -title = {{Lensing is low: Cosmology, galaxy formation or new physics?}}, -volume = {467}, -year = {2017} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 {\textless} z {\textless} 0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 percent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1201.0763}, -author = {Lackner, C N and Gunn, J E}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data%7B%5C_%7Dquery?bibcode=2012arXiv1201.0763L%7B%5C&%7Dlink%7B%5C_%7Dtype=ABSTRACT%7B%5C%25%7D5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Birrer2018, -abstract = {We present a blind time-delay strong lensing (TDSL) cosmographic analysis of the doubly imaged quasar SDSS 1206+4332. We combine the relative time delay between the quasar images, Hubble Space Telescope imaging, the Keck stellar velocity dispersion of the lensing galaxy, and wide-field photometric and spectroscopic data of the field to constrain two angular diameter distance relations. The combined analysis is performed by forward modelling the individual data sets through a Bayesian hierarchical framework, and it is kept blind until the very end to prevent experimenter bias. After unblinding, the inferred distances imply a Hubble constant H 0 = 68.8 +5.4-5.1 km s '1 Mpc '1, assuming a flat cold dark matter cosmology with uniform prior on m in [0.05, 0.5]. The precision of our cosmographic measurement with the doubly imaged quasar SDSS 1206+4332 is comparable with those of quadruply imaged quasars and opens the path to perform on selected doubles the same analysis as anticipated for quads. Our analysis is based on a completely independent lensing code than our previous three H0LiCOW systems and the new measurement is fully consistent with those. We provide the analysis scripts paired with the publicly available software to facilitate independent analysis (footnote with link to www.h0licow.org). The consistency between blind measurements with independent codes provides an important sanity check on lens modelling systematics. By combining the likelihoods of the four systems under the same prior, we obtain H 0 = 72.5 +2.1-2.3 km s '1 Mpc '1. This measurement is independent of the distance ladder and other cosmological probes.}, -archivePrefix = {arXiv}, -arxivId = {1809.01274}, -author = {Birrer, S. and Treu, T. and Rusu, C. E. and Bonvin, V. and Fassnacht, C. D. and Chan, J. H.H. and Agnello, A. and Shajib, A. J. and Chen, G. C.F. and Auger, M. and Courbin, F. and Hilbert, S. and Sluse, D. and Suyu, S. H. and Wong, K. C. and Marshall, P. and Lemaux, B. C. and Meylan, G.}, -doi = {10.1093/mnras/stz200}, -eprint = {1809.01274}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Birrer et al. - 2019 - H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 12064332 and a new measurement of the Hub(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmological parameters,dark energy,ravitational lensing: strong}, -number = {4}, -pages = {4726--4753}, -title = {{H0LiCOW - IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant}}, -url = {http://arxiv.org/abs/1809.01274}, -volume = {484}, -year = {2019} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Walsh1979, -abstract = {0957+561 A,B are two QSOs of mag 17 with 5.7 arc s separation at redshift 1.405. Their spectra leave little doubt that they are associated. Difficulties arise in describing them as two distinct objects and the possibility that they are two images of the same object formed by a gravitational lens is discussed. {\textcopyright} 1979 Nature Publishing Group.}, -author = {Walsh, D. and Carswell, R. F. and Weymann, R. J.}, -doi = {10.1038/279381a0}, -issn = {00280836}, -journal = {Nature}, -keywords = {Absorption Spectra,Emission Spectra,Gravitational Lenses,Quasars,Radio Spectroscopy,Spectrum Analysis,Stellar Spectra}, -month = {may}, -number = {5712}, -pages = {381--384}, -pmid = {16068158}, -title = {{0957+561 A, B: Twin quasistellar objects or gravitational lens?}}, -url = {http://dx.doi.org/10.1038/279381a0}, -volume = {279}, -year = {1979} -} -@article{Cooper:2015aa, -archivePrefix = {arXiv}, -arxivId = {arXiv:1501.04630v2}, -author = {Cooper, P and Parry, Owen H and Lowing, Ben and Cole, Shaun and Frenk, Carlos}, -eprint = {arXiv:1501.04630v2}, -journal = {$\backslash$mnras}, -keywords = {formation,galaxies,haloes,methods,numerical}, -month = {dec}, -number = {October}, -pages = {1--17}, -title = {{Formation of In Situ Stellar Haloes in Milky Way-Mass Galaxies arXiv : 1501 . 04630v2 [ astro-ph . GA ] 4 Oct 2015}}, -volume = {17}, -year = {2015} -} -@article{DiCintio2014, -abstract = {We use a suite of 31 simulated galaxies drawn from the MaGICC project to investigate the effects of baryonic feedback on the density profiles of dark matter haloes. The sample covers a wide mass range: 9.4×109 108 M{\textregistered} with more than 5$\sigma$ detection significance in each lens, if the abundance of substructure is consistent with previous lensing results. The full ALMA array, with its significantly enhanced sensitivity and resolution, should improve these estimates considerably. Given the sample of ∼100 lenses provided by surveys such as the South Pole Telescope, our understanding of dark matter substructure in typical galaxy halos is poised to improve dramatically over the next few years. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1210.4562}, -author = {Hezaveh, Yashar and Dalal, Neal and Holder, Gilbert and Kuhlen, Michael and Marrone, Daniel and Murray, Norman and Vieira, Joaquin}, -doi = {10.1088/0004-637X/767/1/9}, -eprint = {1210.4562}, -isbn = {doi:10.1088/0004-637X/767/1/9}, -issn = {15384357}, -journal = {ApJ}, -keywords = {dark matter,galaxies: dwarf,galaxies: luminosity function,galaxies: structure,gravitational lensing: strong,mass function}, -month = {apr}, -number = {1}, -pages = {9}, -title = {{Dark matter substructure detection using spatially resolved spectroscopy of lensed dusty galaxies}}, -url = {http://adsabs.harvard.edu/abs/2013ApJ...767....9H}, -volume = {767}, -year = {2013} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work conducted to interpret this phenomenon has found that it is due to the non-spherical nature of dark matter halos. However, most studies overpredict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shapes of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations where satellite galaxies without associated subhalos ("orphan galaxies") are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region. {\textcopyright} 2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W. P. and Kang, X. and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V.}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2014 - Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulati.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem&sid=IOPP%3Ajnl_ref&spage=305&title=ArA&volume=5&date=1969&v_showaffiliations=no&aulast=Holmberg%5Cnhttp://stacks.iop.org/0004-637X/786/i=1/a=8?key=cro}, -volume = {786}, -year = {2014} -} -@article{Nierenberg2014, -abstract = {Strong gravitational lenses can be used to detect low-mass subhaloes, based on deviations in image fluxes and positions from what can be achieved with a smooth mass distribution. So far, this method has been limited by the small number of (radio-loud, microlensing-free) systems which can be analysed for the presence of substructure. Using the gravitational lens B1422+231, we demonstrate that adaptive optics integral field spectroscopy can also be used to detect dark substructures. We analyse data obtained with OH Suppressing Infra-Red Imaging Spectrograph on the Keck I Telescope, using a Bayesian method that accounts for uncertainties relating to the point spread function and image positions in the separate exposures. The narrow-line [OIII] fluxes measured for the lensed images are consistent with those measured in the radio, and show a significant deviation from what would be expected in a smooth mass distribution, consistent with the presence of a perturbing low-mass halo. Detailed lens modelling shows that image fluxes and positions are fitted significantly better when the lens is modelled as a system containing a single perturbing subhalo in addition to the main halo, rather than by the main halo on its own, indicating the significant detection of substructure. The inferred mass of the subhalo depends on the subhalo mass density profile: the 68 per cent confidence intervals for the perturber mass within 600 pc are 8.2+0.6-0.8, 8.2+0.6-1 and 7.6 ± 0.3log10[Msub/M(], respectively, for a singular isothermal sphere, a pseudo-Jaffe and a Navarro-Frenk-White mass profile. This method can extend the study of flux ratio anomalies to virtually all quadruply imaged quasars, and therefore offers great potential to improve the determination of the subhalo mass function in the near future.{\textcopyright} 2014 The Authors.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1402.1496v1}, -author = {Nierenberg, A. M. and Treu, T. and Wright, S. A. and Fassnacht, C. D. and Auger, M. W.}, -doi = {10.1093/mnras/stu862}, -eprint = {arXiv:1402.1496v1}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {dark matter,dwarf,galaxies,haloes}, -number = {3}, -pages = {2434--2445}, -title = {{Detection of substructure with adaptive optics integral field spectroscopy of the gravitational lens b1422+231}}, -volume = {442}, -year = {2014} -} -@article{Johnston2016, -abstract = {With the availability of large integral field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, howgalaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present bulge-disc decomposition of IFU data cubes (BUDDI), a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GALFITM, a modified form of GALFIT which can fit multiwaveband images simultaneously. The benefit of this technique over traditional multiwaveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the Sloan Digital Sky Survey-IV Mapping Nearby Galaxies atAPO(MaNGA)survey with redshifts z {\textless} 0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec full width at half-maximum and field of view of {\textgreater} 22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from theMaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data.}, -archivePrefix = {arXiv}, -arxivId = {1611.00609}, -author = {Johnston, Evelyn J and H{\"{a}}u{\ss}ler, Boris and Arag{\'{o}}n-Salamanca, Alfonso and Merrifield, Michael R and Bamford, Steven and Bershady, Matthew A and Bundy, Kevin and Drory, Niv and Fu, Hai and Law, David and Nitschelm, Christian and Thomas, Daniel and Lopes, Alexandre Roman and Wake, David and Yan, Renbin}, -doi = {10.1093/mnras/stw2823}, -eprint = {1611.00609}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content,Galaxies: structure}, -number = {2}, -pages = {2317--2341}, -title = {{SDSS-IV MaNGA: Bulge-disc decomposition of IFU data cubes (BUDDI)}}, -url = {http://arxiv.org/abs/1611.00609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2823}, -volume = {465}, -year = {2017} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}1011 to {\textgreater} 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1086/507084}, -eprint = {0505272}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Rasmussen2016, -author = {Rasmussen, Carl Edward}, -pages = {1--13}, -title = {{Factor Graphs and message passing Key concepts}}, -year = {2016} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L. Gabriel and Arg{\"{u}}elles, C. R. and Perlick, Volker and Rueda, J. A. and Ruffini, R.}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/G{\'{o}}mez et al. - 2016 - Strong lensing by fermionic dark matter in galaxies(2).pdf:pdf}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Hopkins2012, -abstract = {Feedback from massive stars is believed to play a critical role in driving galactic super-winds that enrich the intergalactic medium and shape the galaxy mass function, mass-metallicity relation and other global galaxy properties. In previous papers, we have introduced new numerical methods for implementing stellar feedback on sub-giant molecular cloud (sub-GMC) through galactic scales in numerical simulations of galaxies; the key physical processes include radiation pressure in the ultraviolet through infrared, supernovae (Type I and Type II), stellar winds ('fast' O star through 'slow' asymptotic giant branch winds), and Hii photoionization. Here, we show that these feedback mechanisms drive galactic winds with outflow rates as high as ∼10-20 times the galaxy star formation rate. The mass-loading efficiency (wind mass-loss rate divided by the star formation rate) scales roughly as M wind/M* ∞ V c-1 (where V c is the galaxy circular velocity), consistent with simple momentum-conservation expectations. We use our suite of simulations to study the relative contribution of each feedback mechanism to the generation of galactic winds in a range of galaxy models, from Small Magellanic Cloud like dwarfs and Milky Way (MW) analogues to z∼ 2 clumpy discs. In massive, gas-rich systems (local starbursts and high-z galaxies), radiation pressure dominates the wind generation. By contrast, for MW-like spirals and dwarf galaxies the gas densities are much lower and sources of shock-heated gas such as supernovae and stellar winds dominate the production of large-scale outflows. In all of our models, however, the winds have a complex multiphase structure that depends on the interaction between multiple feedback mechanisms operating on different spatial scales and time-scales: any single feedback mechanism fails to reproduce the winds observed. We use our simulations to provide fitting functions to the wind mass loading and velocities as a function of galaxy properties, for use in cosmological simulations and semi-analytic models. These differ from typically adopted formulae with an explicit dependence on the gas surface density that can be very important in both low-density dwarf galaxies and high-density gas-rich galaxies. {\textcopyright}2012 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.4638}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2012.20593.x}, -eprint = {1110.4638}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Stars: formation}, -number = {4}, -pages = {3522--3537}, -title = {{Stellar feedback in galaxies and the origin of galaxy-scale winds}}, -volume = {421}, -year = {2012} -} -@article{Oguri2021, -abstract = {We present a new approach for fast calculation of gravitational lensing properties, including the lens potential, deflection angles, convergence, and shear, of elliptical Navarro–Frenk–White (NFW) and Hernquist density profiles, by approximating them by superpositions of elliptical density profiles for which simple analytic expressions of gravitational lensing properties are available. This model achieves high fractional accuracy better than 10−4 in the range of the radius normalized by the scale radius of 10−4–103 . These new approximations are ∼300 times faster in solving the lens equation for a point source compared with the traditional approach resorting to expensive numerical integrations, and are implemented in glafic software.}, -archivePrefix = {arXiv}, -arxivId = {2106.11464}, -author = {Oguri, Masamune}, -doi = {10.1088/1538-3873/AC12DB}, -eprint = {2106.11464}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Oguri2021CSE.pdf:pdf}, -issn = {00046280}, -journal = {Publ. Astron. Soc. Pac.}, -keywords = {dark matter,gravitational lensing,methods,strong,weak}, -number = {1025}, -pages = {6}, -title = {{Fast calculation of gravitational lensing properties of elliptical navarro–frenk–white and hernquist density profiles}}, -volume = {133}, -year = {2021} -} -@article{Hartigan1979, -abstract = {The K-means clustering algorithm is described indetail by Hartigan(1975). An efficient version of the algorithm is presented here.$\backslash$nThe aim of the K-means algorithm is to divide M points in N dimensions into K clusters so that the within-cluster sum of squares is minimized. It is not practical to require that the solution has minimal sum of squares against all partitions except when M,N are small and K = 2. We seek instead "local" optima, solution such that no movement of a point from one cluster to another will reduce the within cluster sum of squares.}, -author = {Hartigan, J A and Wong, M A}, -doi = {10.2307/2346830}, -isbn = {00359254}, -issn = {00359254}, -journal = {Applied Statistics}, -keywords = {k-means clustering algorithm,transfer algorithm}, -number = {1}, -pages = {100}, -pmid = {8705250}, -title = {{Algorithm AS 136: A K-Means Clustering Algorithm}}, -url = {http://www.jstor.org/stable/10.2307/2346830?origin=crossref}, -volume = {28}, -year = {2006} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A. and Birnboim, Y. and Engel, G. and Freundlich, J. and Goerdt, T. and Mumcuoglu, M. and Neistein, E. and Pichon, C. and Teyssier, R. and Zinger, E.}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel et al. - 2009 - Cold streams in early massive hot haloes as the main mode of galaxy formation.pdf:pdf}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {https://ui.adsabs.harvard.edu/#abs/2009Natur.457..451D/abstract}, -volume = {457}, -year = {2009} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from $\sim$1011 to > 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above $\sim$1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K.}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/K{\"{u}}ng et al. - 2018 - Models of gravitational lens candidates from SpaceWarps CFHTLS(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Croton2006, -abstract = {We simulate the growth of galaxies and their central supermassive black holes by implementing a suite of semi-analytic models on the output of the Millennium Run, a very large simulation of the concordance $\Lambda$ cold dark matter cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In this first paper we supplement previous treatments of the growth and activity of central black holes with a new model for 'radio' feedback from those active galactic nuclei that lie at the centre of a quasi-static X-ray-emitting atmosphere in a galaxy group or cluster. We show that for energetically and observationally plausible parameters such a model can simultaneously explain: (i) the low observed mass drop-out rate in cooling flows; (ii) the exponential cut-off at the bright end of the galaxy luminosity function; and (iii) the fact that the most massive galaxies tend to be bulge-dominated systems in clusters and to contain systematically older stars than lower mass galaxies. This success occurs because static hot atmospheres form only in the most massive structures, and radio feedback (in contrast, for example, to supernova or starburst feedback) can suppress further cooling and star formation without itself requiring star formation. We discuss possible physical models that might explain the accretion rate scalings required for our phenomenological 'radio mode' model to be successful. {\textcopyright} 2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0508046}, -author = {Croton, Darren J. and Springel, Volker and White, Simon D.M. and {De Lucia}, G. and Frenk, C. S. and Gao, L. and Jenkins, A. and Kauffmann, G. and Navarro, J. F. and Yoshida, N.}, -doi = {10.1111/j.1365-2966.2005.09675.x}, -eprint = {0508046}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Croton et al. - 2006 - The many lives of active galactic nuclei Cooling flows, black holes and the luminosities and colours of galaxi(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cooling flows,Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation}, -number = {1}, -pages = {11--28}, -pmid = {22266574}, -primaryClass = {astro-ph}, -title = {{The many lives of active galactic nuclei: Cooling flows, black holes and the luminosities and colours of galaxies}}, -volume = {365}, -year = {2006} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Devour2017, -abstract = {Accurate measurement of galaxy structures is a prerequisite for quantitative investigation of galaxy properties or evolution. Yet, the impact of galaxy inclination and dust on commonly used metrics of galaxy structure is poorly quantified. We use infrared data sets to select inclination-independent samples of disc and flattened elliptical galaxies. These samples show strong variation in S\'{e}rsic index, concentration, and half-light radii with inclination. We develop novel inclination-independent galaxy structures by collapsing the light distribution in the near-infrared on to the major axis, yielding inclination-independent `linear' measures of size and concentration. With these new metrics we select a sample of Milky Way analogue galaxies with similar stellar masses, star formation rates, sizes and concentrations. Optical luminosities, light distributions, and spectral properties are all found to vary strongly with inclination: When inclining to edge-on, $r$-band luminosities dim by $>$1 magnitude, sizes decrease by a factor of 2, `dust-corrected' estimates of star formation rate drop threefold, metallicities decrease by 0.1 dex, and edge-on galaxies are half as likely to be classified as star forming. These systematic effects should be accounted for in analyses of galaxy properties.}, -archivePrefix = {arXiv}, -arxivId = {1702.06528}, -author = {Devour, Brian M. and Bell, Eric F.}, -doi = {10.1093/mnrasl/slx021}, -eprint = {1702.06528}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Devour, Bell - 2017 - Revealing strong bias in common measures of galaxy properties using new inclination-independent structures(2).pdf:pdf}, -issn = {1745-3925}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {dust,extinction,galaxies,general,photometric,techniques}, -number = {1}, -pages = {L31--L35}, -pmid = {18462818}, -title = {{Revealing strong bias in common measures of galaxy properties using new inclination-independent structures}}, -url = {http://arxiv.org/abs/1702.06528%0Ahttp://dx.doi.org/10.1093/mnrasl/slx021}, -volume = {468}, -year = {2017} -} -@article{Schneider2013, -abstract = {The light travel time dierences in strong gravitational lensing systems allows an independent determination of the Hubble constant. This method has been successfully applied to several lens systems. The formally most precise measurements are, however, in tension with the recent determination of H0 from the Planck satellite for a spatially flat six-parameters CDM cosmology. We reconsider the uncertainties of the method, concerning the mass profile of the lens galaxies, and show that the formal precision relies on the assumption that the mass profile is a perfect power law. Simple analytical arguments and numerical experiments reveal that masssheet like transformations yield significant freedom in choosing the mass profile, even when exquisite Einstein rings are observed. Furthermore, the characterization of the environment of the lens does not break that degeneracy which is not physically linked to extrinsic convergence. We present an illustrative example where the multiple imaging properties of a composite (baryons + dark matter) lens can be extremely well reproduced by a power-law model having the same velocity dispersion, but with predictions for the Hubble constant that deviate by 20%. Hence we conclude that the impact of degeneracies between parametrized models have been underestimated in current H0 measurements from lensing, and need to be carefully reconsidered. {\textcopyright} ESO 2013.}, -archivePrefix = {arXiv}, -arxivId = {1306.0901}, -author = {Schneider, Peter and Sluse, Dominique}, -doi = {10.1051/0004-6361/201321882}, -eprint = {1306.0901}, -issn = {00046361}, -journal = {A\&A}, -keywords = {Cosmological parameters,Gravitational lensing: strong}, -month = {nov}, -pages = {A37}, -title = {{Mass-sheet degeneracy, power-law models and external convergence: Impact on the determination of the Hubble constant from gravitational lensing}}, -url = {http://arxiv.org/abs/1306.0901%0Ahttp://dx.doi.org/10.1051/0004-6361/201321882}, -volume = {559}, -year = {2013} -} -@article{Elias2018a, -abstract = {The existence of stellar halos around galaxies is a natural prediction of the hierarchical nature of the $\Lambda$CDM model. Recent observations of Milky Way-like galaxies have revealed a wide range in stellar halo mass, including cases with no significant detection of a stellar halo, as in the case of M101, NGC 3351 and NGC 1042. We use the Illustris simulation to investigate the scatter in stellar halo content and, in particular, to study the formation of galaxies in the range M200 = 8 × 1011-2 × 1012 M⊙ with the smallest fraction of this diffuse component. Stellar halos are far from spherical, which diminishes the surface brightness of the stellar halo for face-on disks. Once accounting for projection effects, we find that the stellar halo fraction fSH correlates strongly with galaxy morphology and star formation rate, but not with environment, in agreement with observations. Galaxies with the lowest stellar halo fractions are disk-dominated, star-forming, and assemble their dark matter halos earlier than galaxies with similar masses. They have also accreted more low-mass satellites at earlier infall times than centrals with high fSH. In situ rather than accreted stars dominate the stellar halos of galaxies with the lowest stellar halo fractions, with a transition radius from in situ to accretiondominated r $\sim$ 45 kpc. Our results extrapolated to real galaxies such as M101 may indicate that these galaxies inhabit old halos which endured mergers at higher redshifts and evolved unperturbed in the last $\sim$10 Gyrs.}, -archivePrefix = {arXiv}, -arxivId = {1801.07273}, -author = {Elias, Lydia M. and Sales, Laura V. and Creasey, Peter and Cooper, Michael C. and Bullock, James S. and {Michael Rich}, R. and Hernquist, Lars}, -doi = {10.1093/mnras/sty1718}, -eprint = {1801.07273}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Elias et al. - 2018 - Stellar halos in illustris Probing the histories of milky way-mass galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: haloes,Methods: numerical}, -number = {3}, -pages = {4004--4016}, -title = {{Stellar halos in illustris: Probing the histories of milky way-mass galaxies}}, -url = {http://arxiv.org/abs/1801.07273}, -volume = {479}, -year = {2018} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{Jacob2009, -abstract = {The main focus of this paper is to derive a memory efficient approximation to the nonuniform Fourier transform of a support limited sequence. We show that the standard nonuniform fast Fourier transform (NUFFT) scheme is a shift invariant approximation of the exact Fourier transform. Based on the theory of shift-invariant representations, we derive an exact expression for the worst-case mean square approximation error. Using this metric, we evaluate the optimal scale-factors and the interpolator that provides the least approximation error. We also derive the upper-bound for the error component due to the lookup table based evaluation of the interpolator; we use this metric to ensure that this component is not the dominant one. Theoretical and experimental comparisons with standard NUFFT schemes clearly demonstrate the significant improvement in accuracy over conventional schemes, especially when the size of the uniform fast Fourier transform (FFT) is small. Since the memory requirement of the algorithm is dependent on the size of the uniform FFT, the proposed developments can lead to iterative signal reconstruction algorithms with significantly lower memory demands. {\textcopyright} 2009 IEEE.}, -author = {Jacob, Mathews}, -doi = {10.1109/TSP.2009.2014809}, -file = {:C\:/Users/Jammy/Documents/Papers/NUFFTPAper.pdf:pdf}, -issn = {1053587X}, -journal = {IEEE Transactions on Signal Processing}, -keywords = {Fourier transform,Interpolation,Nonuniform,Sampling,Shift-invariant}, -number = {6}, -pages = {2165--2177}, -title = {{Optimized least-square nonuniform fast Fourier transform}}, -volume = {57}, -year = {2009} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within ∼30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M and a factor of 3 at 107 M. The most massive subhalos with 1010 M survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://adsabs.harvard.edu/abs/2010ApJ...709.1138D}, -volume = {709}, -year = {2010} -} -@article{Morishita2018a, -abstract = {Observations have revealed log M*/Msun {\textgreater}11 galaxies that were already dead when the universe was only {\$\sim${}}2Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interests. In this paper, we study star formation and metallicity enrichment histories of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple HST surveys allows robust determination of their SEDs. Our new SED modeling provides mass accumulation/stellar metallicity enrichment histories of those galaxies over the past {\$\sim${}}3Gyr, with no functional assumptions on their star formation histories. We find that most of our massive galaxies have formed {\textgreater}50{\%} of their extant masses by {\$\sim${}}1.5Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Most of our galaxies already have stellar metallicities compatible with, or even higher than, those of local early-type galaxies, with a median value of log Z*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. By using reconstructed star formation history, we reveal their rapid metallicity enrichment history from z{\$\sim${}}5.5 to 2.2 at a rate of {\$\sim${}}0.2dex/Gyr in logZ*/Zsun. The inferred metallicities are on average {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies at the time of formation. This supports a view where quenched galaxies continue to form stars at low-level until recently, rather than abrupt termination of star formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -eprint = {1812.06980}, -keywords = {evolution,formation,galaxies,star formation}, -title = {{Massive Dead Galaxies at z{\$\sim${}}2 with HST Grism Spectroscopy I. Star Formation and Metallicity Enrichment Histories}}, -url = {http://arxiv.org/abs/1812.06980}, -year = {2018} -} -@article{Xia2017, -abstract = {In this paper we use high-resolution cosmological simulations to study halo intrinsic alignment and its dependence on mass, formation time and large-scale environment. In agreement with previous studies using N-body simulations, it is found that massive halos have stronger alignment. For given mass, older halos have stronger alignment than younger ones. By identifying the cosmic environment of halo using Hessian matrix, we find that for given mass, halos in cluster regions also have stronger alignment than those in filament. The existing theory has not addressed these dependencies explicitly. In this work we extend the linear alignment model with inclusion of halo bias and find that the halo alignment with its mass and formation time dependence can be explained by halo bias. However, the model can not account for the environment dependence, as it is found that halo bias is lower in cluster and higher in filament. Our results suggest that halo bias and environment are independent factors in determining halo alignment. We also study the halo alignment correlation function and find that halos are strongly clustered along their major axes and less clustered along the minor axes. The correlated halo alignment can extend to scale as large as {\$}100h{\^{}}{\{}-1{\}}{\$}Mpc where its feature is mainly driven by the baryon acoustic oscillation effect.}, -archivePrefix = {arXiv}, -arxivId = {1706.07814}, -author = {Xia, Qianli and Kang, Xi and Wang, Peng and Luo, Yu and Yang, Xiaohu and Jing, Yipeng and Wang, Huiyuan and Mo, Houjun}, -doi = {10.3847/1538-4357/aa8d17}, -eprint = {1706.07814}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {22}, -title = {{Halo Intrinsic Alignment: Dependence on Mass, Formation Time, and Environment}}, -url = {http://arxiv.org/abs/1706.07814%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8d17}, -volume = {848}, -year = {2017} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful numbers of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag 24 - 25 limits. But gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z {\$\sim${}} 5 - 7 for LSST. We find that the LSST main survey could detect {\$\sim${}} 1 - 2 lensed Population III (Pop III) SN but 130-1400 Pop I/II SNe. An alternative deep survey with a one-year cadence could find {\$\sim${}}10 Pop III SNe with an 84h exposure and {\$\sim${}}50 SNe with a 420h exposure.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes-Erik and Whalen, Daniel J and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S}, -eprint = {1805.02662}, -keywords = {cos-,cosmology,dark ages,early universe,first stars,galaxies,gravitational lensing,high-redshift,mology,observations,population iii,reionization,stars,strong}, -number = {May}, -pages = {1--12}, -title = {{Detecting strongly lensed supernovae at z {\$\sim${}} 5-7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {12}, -year = {2018} -} -@article{Gunn1965, -abstract = {Not Available}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1011.1669v3}, -author = {Gunn, James E. and Peterson, Bruce A.}, -doi = {10.1086/148444}, -eprint = {arXiv:1011.1669v3}, -isbn = {doi:10.1086/148444}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -month = {nov}, -pages = {1633}, -pmid = {25246403}, -title = {{On the Density of Neutral Hydrogen in Intergalactic Space.}}, -url = {http://adsabs.harvard.edu/doi/10.1086/148444}, -volume = {142}, -year = {1965} -} -@article{Kang2007, -abstract = {Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM concordance cosmology. To that extent we use a large {\$}N{\$}-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as function of halo mass and galaxy color. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by {\$}\backslashbackslashsim 40{\^{}}{\{}\backslashbackslashcirc{\{}\backslash{\}}{\}}{\$} (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the color of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the color of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0701130}, -author = {Kang, X and {Van Den Bosch}, Frank C and Yang, Xiaohu and Mao, Shude and Mo, H J and Li, Cheng and Jing, Y P}, -doi = {10.1111/j.1365-2966.2007.11902.x}, -eprint = {0701130}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Large-scale structure of Universe,Methods: statistical}, -number = {4}, -pages = {1531--1542}, -primaryClass = {astro-ph}, -title = {{The alignment between satellites and central galaxies: Theory versus observations}}, -volume = {378}, -year = {2007} -} -@article{Woo2014, -abstract = {We investigate the roles of two classes of quenching mechanisms for central and satellite galaxies in the Sloan Digital Sky Survey (z < 0.075): those involving the halo and those involving the formation of a compact centre. For central galaxies with inner compactness $\Sigma$1 kpc $\sim$ 109-9.4M⊙ kpc-2, the quenched fraction fq is strongly correlated with $\Sigma$1 kpc with only weak halo mass Mh dependence. However, at higher and lower $\Sigma$1 kpc, specific star formation rate (sSFR) is a strong function of Mh and mostly independent of $\Sigma$1 kpc. In other words, $\Sigma$1 kpc $\sim$ 109-9.4M⊙ kpc-2 divides galaxies into those with high sSFR below and low sSFR above this range. In both the upper and lower regimes, increasing Mh shifts the entire sSFR distribution to lower sSFR without a qualitative change in shape. This is true even at fixed M*, but varying M* at fixed Mh adds no quenching information. Most of the quenched centrals with Mh > 1011.8M⊙ are dense ($\Sigma$1 kpc > 109M⊙ kpc-2), suggesting compaction-related quenching maintained by halo-related quenching. However, 21 per cent are diffuse, indicating only halo quenching. For satellite galaxies in the outskirts of haloes, quenching is a strong function of compactness and a weak function of host Mh. In the inner halo, Mh dominates quenching, with $\sim$90 per cent of the satellites being quenched once Mh > 1013M⊙. This regional effect is greatest for the least massive satellites. As demonstrated via semi-analytic modelling with simple prescriptions for quenching, the observed correlations can be explained if quenching due to central compactness is rapid while quenching due to halo mass is slow.}, -archivePrefix = {arXiv}, -arxivId = {1406.5372}, -author = {Woo, Joanna and Dekel, Avishai and Faber, S. M. and Koo, David C.}, -doi = {10.1093/mnras/stu2755}, -eprint = {1406.5372}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: general,Galaxies: groups: general,Galaxies: haloes,Galaxies: star formation,Galaxies: structure}, -month = {mar}, -number = {1}, -pages = {237--251}, -title = {{Two conditions for galaxy quenching: Compact centres and massive haloes}}, -url = {http://adsabs.harvard.edu/abs/2015MNRAS.448..237W}, -volume = {448}, -year = {2015} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in ≲10 dynamical times, or ≲0.5 Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, 100 M yr-1, and each clump converts into stars in 0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z 3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z 1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies. {\textcopyright}2009 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Reynolds2015, -abstract = {Compact radio sources sometimes exhibit intervals of large, rapid changes in their flux-density, due to lensing by interstellar plasma crossing the line-of-sight. A novel survey program has made it possible to discover these "Extreme Scattering Events" (ESEs) in real time, resulting in a high-quality dynamic spectrum of an ESE observed in PKS 1939-315. Here we present a method for determining the column-density profile of a plasma lens, given only the dynamic radio spectrum of the lensed source, under the assumption that the lens is either axisymmetric or totally anisotropic. Our technique relies on the known, strong frequency dependence of the plasma refractive index in order to determine how points in the dynamic spectrum map to positions on the lens. We apply our method to high-frequency (4.2-10.8 GHz) data from the Australia Telescope Compact Array of the PKS 1939-315 ESE. The derived electron column-density profiles are very similar for the two geometries we consider, and both yield a good visual match to the data. However, the fit residuals are substantially above the noise level, and deficiencies are evident when we compare the predictions of our model to lower-frequency (1.6-3.1 GHz) data on the same ESE, thus motivating future development of more sophisticated inversion techniques.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1512.03411}, -author = {Tuntsov, Artem V. and Walker, Mark A. and Koopmans, Leon V. E. and Bannister, Keith W. and Stevens, Jamie and Johnston, Simon and Reynolds, Cormac and Bignall, Hayley E.}, -doi = {10.3847/0004-637x/817/2/176}, -eprint = {1512.03411}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Tuntsov et al. - 2016 - Dynamic Spectral Mapping of Interstellar Plasma Lenses(2).pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {176}, -title = {{Dynamic Spectral Mapping of Interstellar Plasma Lenses}}, -url = {http://arxiv.org/abs/1512.03411%0Ahttp://dx.doi.org/10.3847/0004-637X/817/2/176}, -volume = {817}, -year = {2016} -} -@article{Despali2017, -abstract = {We investigate the impact of baryonic physics on the subhalo population by analysing the results of two recent hydrodynamical simulations (EAGLE and Illustris), which have very similar configuration, but a different model of baryonic physics. We concentrate on haloes with a mass between 1012.5 and 1014M⊙ h-1 and redshift between 0.2 and 0.5, comparing with observational results and subhalo detections in early-type galaxy lenses. We compare the number and the spatial distribution of subhaloes in the fully hydro runs and in their darkmatter- only (DMO) counterparts, focusing on the differences between the two simulations. We find that the presence of baryons reduces the number of subhaloes, especially at the lowmass end (≤1010M⊙h-1), by different amounts depending on the model. The variations in the subhalo mass function are strongly dependent on those in the halo mass function, which is shifted by the effect of stellar and AGN feedback. Finally, we search for analogues of the observed lenses (Sloan Lens ACS) in the simulations, selecting them in velocity dispersion and dynamical properties. We use the selected galaxies to quantify detection expectations based on the subhalo populations in the different simulations, calculating the detection probability and the predicted values for the projected dark matter fraction in subhaloes fDM and the slope of the mass function $\alpha$. We compare these values with those derived from subhalo detections in observations and conclude that the DMO and hydro EAGLE runs are both compatible with observational results, while results from the hydro Illustris run do not lie within the errors.}, -archivePrefix = {arXiv}, -arxivId = {1608.06938}, -author = {Despali, Giulia and Vegetti, Simona}, -doi = {10.1093/mnras/stx966}, -eprint = {1608.06938}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Despali, Vegetti - 2017 - The impact of baryonic physics on the subhalo mass function and implications for gravitational lensing.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmology: Theory,Dark matter,Galaxies: Haloes,Methods: numerical}, -number = {2}, -pages = {1997--2010}, -title = {{The impact of baryonic physics on the subhalo mass function and implications for gravitational lensing}}, -volume = {469}, -year = {2017} -} -@article{Hoyos2011, -abstract = {We present a catalogue of structural parameters for 8814 galaxies in the 25 fields of the Hubble Space Telescope/ACS Coma Treasury Survey. Parameters from S{\'{e}}rsic fits to the two-dimensional surface brightness distributions are given for all galaxies from our published Coma photometric catalogue with mean effective surface brightness brighter than 26.0magarcsec-2 and brighter than 24.5mag (equivalent to absolute magnitude -10.5), as given by the fits, all in F814W(AB). The sample comprises a mixture of Coma members and background objects; 424 galaxies have redshifts and of these 163 are confirmed members. The fits were carried out using both the gim2dand galfit codes. We provide the following parameters: galaxy ID, RA, Dec., the total corrected automatic magnitude from the photometric catalogue, the total magnitude of the model (F814WAB), the geometric mean effective radius Re, the mean surface brightness within the effective radius 〈$\mu$〉e, the S{\'{e}}rsic index n, the ellipticity and the source position angle. The selection limits of the catalogue and the errors listed for the S{\'{e}}rsic parameters come from extensive simulations of the fitting process using synthetic galaxy models. The agreement between gim2d and galfit parameters is sensitive to details of the fitting procedure; for the settings employed here the agreement is excellent over the range of parameters covered in the catalogue. We define and present two goodness-of-fit indices which quantify the degree to which the image can be approximated by a S{\'{e}}rsic model with concentric, coaxial elliptical isophotes; such indices may be used to objectively select galaxies with more complex structures such as bulge-disc, bars or nuclear components. We make the catalogue available in electronic format at astro-wise and MAST. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1010.2352}, -author = {Hoyos, Carlos and {Den Brok}, Mark and Kleijn, Gijs Verdoes and Carter, David and Balcells, Marc and Guzm{\'{a}}n, Rafael and Peletier, Reynier and Ferguson, Henry C. and Goudfrooij, Paul and Graham, Alister W. and Hammer, Derek and Karick, Arna M. and Lucey, John R. and Matkovi{\'{c}}, Ana and Merritt, David and Mouhcine, Mustapha and Valentijn, Edwin}, -doi = {10.1111/j.1365-2966.2010.17855.x}, -eprint = {1010.2352}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: individual: Coma,Galaxies: dwarf,Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: fundamental parameters}, -number = {4}, -pages = {2439--2460}, -title = {{The HST/ACS Coma Cluster Survey - III. Structural parameters of galaxies using single S{\'{e}}rsic fits}}, -url = {http://arxiv.org/abs/1010.2352v1%7B%25%7D5Cnfile:///Users/boris/Documents/Papers/2010/Hoyos/arXiv 2010}, -volume = {411}, -year = {2011} -} -@article{RomanoDiaz2008, -abstract = {We study the central dark matter (DM) cusp evolution in cosmological galactic halos. Models with and without baryons (baryons+DM, hereafter BDM model, and pure DM, PDM model, respectively) are advanced from identical initial conditions. The DM cusp properties are contrasted by a direct comparison of pure DM and baryonic models. We find a divergent evolution between the PDM and BDM models within the inner $\sim$10 kpc region. The PDM model forms a R^{-1} cusp as expected, while the DM in the BDM model forms a larger isothermal cusp R^{-2} instead. The isothermal cusp is stable until z$\sim$1 when it gradually levels off. This leveling proceeds from inside out and the final density slope is shallower than -1 within the central 3 kpc (i.e., expected size of the R^{-1} cusp), tending to a flat core within $\sim$2 kpc. This effect cannot be explained by a finite resolution of our code which produces only a 5% difference between the gravitationally softened force and the exact Newtonian force of point masses at 1 kpc from the center. Neither is it related to the energy feedback from stellar evolution or angular momentum transfer from the bar. Instead it can be associated with the action of DM+baryon subhalos heating up the cusp region via dynamical friction and forcing the DM in the cusp to flow out and to `cool' down. The process described here is not limited to low z and can be efficient at intermediate and even high z.}, -archivePrefix = {arXiv}, -arxivId = {0808.0195}, -author = {Romano-D{\'{i}}az, Emilio and Shlosman, Isaac and Hoffman, Yehuda and Heller, Clayton}, -doi = {10.1086/592687}, -eprint = {0808.0195}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Evolution,Galaxies: Formation,Galaxies: Halos,Galaxies: Interactions,Galaxies: Kinematics and Dynamics}, -month = {oct}, -number = {2}, -pages = {L105--L108}, -title = {{Erasing Dark Matter Cusps in Cosmological Galactic Halos with Baryons}}, -url = {http://arxiv.org/abs/0808.0195%0Ahttp://dx.doi.org/10.1086/592687}, -volume = {685}, -year = {2008} -} -@article{Greene2017, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Kormendy2009, -abstract = {New surface photometry of all known elliptical galaxies in the Virgo cluster is combined with published data to derive composite profiles of brightness, ellipticity, position angle, isophote shape, and color over large radius ranges. These provide enough leverage to show that S{\'{e}}rsic log I r 1/n functions fit the brightness profiles I(r) of nearly all ellipticals remarkably well over large dynamic ranges. Therefore, we can confidently identify departures from these profiles that are diagnostic of galaxy formation. Two kinds of departures are seen at small radii. All 10 of our ellipticals with total absolute magnitudes MVT ≤ -21.66 have cuspy cores - "missing light" - at small radii. Cores are well known and naturally scoured by binary black holes (BHs) formed in dissipationless ("dry") mergers. All 17 ellipticals with -21.54 ≤ MVT ≤ -15.53 do not have cores. We find a new distinct component in these galaxies: all coreless ellipticals in our sample have extra light at the center above the inward extrapolation of the outer S{\'{e}}rsic profile. In large ellipticals, the excess light is spatially resolved and resembles the central components predicted in numerical simulations of mergers of galaxies that contain gas. In the simulations, the gas dissipates, falls toward the center, undergoes a starburst, and builds a compact stellar component that, as in our observations, is distinct from the S{\'{e}}rsic-function main body of the elliptical. But ellipticals with extra light also contain supermassive BHs. We suggest that the starburst has swamped core scouring by binary BHs. That is, we interpret extra light components as a signature of formation in dissipative ("wet") mergers. Besides extra light, we find three new aspects to the ("E-E") dichotomy into two types of elliptical galaxies. Core galaxies are known to be slowly rotating, to have relatively anisotropic velocity distributions, and to have boxy isophotes. We show that they have S{\'{e}}rsic indices n > 4 uncorrelated with MVT . They also are $\alpha$-element enhanced, implying short star-formation timescales. And their stellar populations have a variety of ages but mostly are very old. Extra light ellipticals generally rotate rapidly, are more isotropic than core Es, and have disky isophotes. We show that they have n ≃ 3 1 almost uncorrelated with MVT and younger and less $\alpha$-enhanced stellar populations. These are new clues to galaxy formation. We suggest that extra light ellipticals got their low S{\'{e}}rsic indices by forming in relatively few binary mergers, whereas giant ellipticals have n > 4 because they formed in larger numbers of mergers of more galaxies at once plus later heating during hierarchical clustering. We confirm that core Es contain X-ray-emitting gas whereas extra light Es generally do not. This leads us to suggest why the E-E dichotomy arose. If energy feedback from active galactic nuclei (AGNs) requires a "working surface" of hot gas, then this is present in core galaxies but absent in extra light galaxies. We suggest that AGN energy feedback is a strong function of galaxy mass: it is weak enough in small Es not to prevent merger starbursts but strong enough in giant Es and their progenitors to make dry mergers dry and to protect old stellar populations from late star formation. Finally, we verify that there is a strong dichotomy between elliptical and spheroidal galaxies. Their properties are consistent with our understanding of their different formation processes: mergers for ellipticals and conversion of late-type galaxies into spheroidals by environmental effects and by energy feedback from supernovae. In an appendix, we develop machinery to get realistic error estimates for S{\'{e}}rsic parameters even when they are strongly coupled. And we discuss photometric dynamic ranges necessary to get robust results from S{\'{e}}rsic fits. {\textcopyright} 2009. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0810.1681}, -author = {Kormendy, John and Fisher, David B. and Cornell, Mark E. and Bender, Ralf}, -doi = {10.1088/0067-0049/182/1/216}, -eprint = {0810.1681}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Kormendy et al. - 2009 - Structure and formation of elliptical and spheroidal galaxies.pdf:pdf}, -isbn = {0067-0049, 1538-4365}, -issn = {00670049}, -journal = {ApJS}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: nuclei,Galaxies: photometry,Galaxies: structure,cD}, -number = {1}, -pages = {216--309}, -title = {{Structure and formation of elliptical and spheroidal galaxies}}, -volume = {182}, -year = {2009} -} -@article{Savorgnan2015, -abstract = {The S$\backslash$'ersic {\$}R{\^{}}{\{}1/n{\}}{\$} model is the best approximation known to date for describing the light distribution of stellar spheroidal and disk components, with the S$\backslash$'ersic index {\$}n{\$} providing a direct measure of the central radial concentration of stars. The S$\backslash$'ersic index of a galaxy's spheroidal component, {\$}n{\_}{\{}sph{\}}{\$}, has been shown to tightly correlate with the mass of the central supermassive black hole, {\$}M{\_}{\{}BH{\}}{\$}. The {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} correlation is also expected from other two well known scaling relations involving the spheroid luminosity, {\$}L{\_}{\{}sph{\}}{\$}: the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and the {\$}M{\_}{\{}BH{\}}-L{\_}{\{}sph{\}}{\$}. Obtaining an accurate estimate of the spheroid S$\backslash$'ersic index requires a careful modelling of a galaxy's light distribution and some studies have failed to recover a statistically significant {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} correlation. With the aim of re-investigating the {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} and other black hole mass scaling relations, we performed a detailed (i.e.{\$\sim${}}bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, that had been imaged at {\$}3.6\backslashrm{\\sim{}}\backslashmu m{\$} with Spitzer. In this paper, the third of this series, we present an analysis of the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}-n{\_}{\{}sph{\}}{\$} diagrams. While early-type (elliptical+lenticular) and late-type (spiral) galaxies split into two separate relations in the {\$}L{\_}{\{}sph{\}}-n{\_}{\{}sph{\}}{\$} and {\$}M{\_}{\{}BH{\}}-L{\_}{\{}sph{\}}{\$} diagrams, they reunite into a single {\$}M{\_}{\{}BH{\}} \backslashpropto n{\_}{\{}sph{\}}{\^{}}{\{}3.39 \backslashpm 0.15{\}}{\$} sequence with relatively small intrinsic scatter ({\$}\backslashepsilon \backslashsimeq 0.25 \backslashrm{\\sim{}}dex{\$}). The black hole mass appears to be closely related to the spheroid central concentration of stars, which mirrors the inner gradient of the spheroid gravitational potential.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1603.01910}, -author = {Savorgnan, Giulia A D}, -doi = {10.3847/0004-637x/821/2/88}, -eprint = {1603.01910}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {88}, -title = {{ SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE M BH – n sph CORRELATION }}, -url = {http://arxiv.org/abs/1603.01910%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/821/2/88}, -volume = {821}, -year = {2016} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-$\alpha$ emission from the host galaxy of SDSS$\sim$J2222+2745, a strongly lensed quasar at $z = 2.8$. Spectroscopic follow-up clearly reveals extended Lyman-$\alpha$ in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as $\sim$200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-$\alpha$ emission to its physical origin on one side of the host galaxy at radii $\sim$0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-$\alpha$ and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-$\alpha$, host galaxy Lyman-$\alpha$, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B. and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D. and Rigby, Jane R. and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bayliss et al. - 2017 - Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy(2).pdf:pdf}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Treu2016, -abstract = {Gravitational time delays, observed in strong lens systems where the variable background source is multiply imaged by a massive galaxy in the foreground, provide direct measurements of cosmological distance that are very complementary to other cosmographic probes. The success of the technique depends on the availability and size of a suitable sample of lensed quasars or supernovae, precise measurements of the time delays, accurate modeling of the gravitational potential of the main deflector, and our ability to characterize the distribution of mass along the line of sight to the source. We review the progress made during the last 15 years, during which the first competitive cosmological inferences with time delays were made, and look ahead to the potential of significantly larger lens samples in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1605.05333}, -author = {Treu, Tommaso and Marshall, Philip J.}, -doi = {10.1007/s00159-016-0096-8}, -eprint = {1605.05333}, -issn = {09354956}, -journal = {Astronomy and Astrophysics Review}, -keywords = {Cosmology,Dark energy,Gravitational lensing,Gravity}, -month = {may}, -number = {1}, -title = {{Time delay cosmography}}, -volume = {24}, -year = {2016} -} -@article{Irsic2017, -abstract = {We present new measurements of the free-streaming of warm dark matter (WDM) from Lyman-$\alpha$ flux-power spectra. We use data from the medium resolution, intermediate redshift XQ-100 sample observed with the X-shooter spectrograph (z=3-4.2) and the high-resolution, high-redshift sample used in Viel et al. (2013) obtained with the HIRES/MIKE spectrographs (z=4.2-5.4). Based on further improved modelling of the dependence of the Lyman-$\alpha$ flux-power spectrum on the free-streaming of dark matter, cosmological parameters, as well as the thermal history of the intergalactic medium (IGM) with hydrodynamical simulations, we obtain the following limits, expressed as the equivalent mass of thermal relic WDM particles. The XQ-100 flux power spectrum alone gives a lower limit of 1.4 keV, the re-analysis of the HIRES/MIKE sample gives 4.1 keV while the combined analysis gives our best and significantly strengthened lower limit of 5.3 keV (all 2$\sigma$ C.L.). The further improvement in the joint analysis is partly due to the fact that the two data sets have different degeneracies between astrophysical and cosmological parameters that are broken when the data sets are combined, and more importantly on chosen priors on the thermal evolution. These results all assume that the temperature evolution of the IGM can be modeled as a power law in redshift. Allowing for a nonsmooth evolution of the temperature of the IGM with sudden temperature changes of up to 5000 K reduces the lower limit for the combined analysis to 3.5 keV. A WDM with smaller thermal relic masses would require, however, a sudden temperature jump of 5000 K or more in the narrow redshift interval z=4.6-4.8, in disagreement with observations of the thermal history based on high-resolution resolution Lyman-$\alpha$ forest data and expectations for photo-heating and cooling in the low density IGM at these redshifts.}, -archivePrefix = {arXiv}, -arxivId = {1702.01764}, -author = {Ir{\v{s}}i{\v{c}}, Vid and Viel, Matteo and Haehnelt, Martin G. and Bolton, James S. and Cristiani, Stefano and Becker, George D. and D'Odorico, Valentina and Cupani, Guido and Kim, Tae Sun and Berg, Trystyn A.M. and L{\'{o}}pez, Sebastian and Ellison, Sara and Christensen, Lise and Denney, Kelly D. and Worseck, G{\'{a}}bor}, -doi = {10.1103/PhysRevD.96.023522}, -eprint = {1702.01764}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Ir{\v{s}}i{\v{c}} et al. - 2017 - New constraints on the free-streaming of warm dark matter from intermediate and small scale Lyman- $\alpha$ forest data.pdf:pdf}, -issn = {24700029}, -journal = {Physical Review D}, -number = {2}, -pages = {1--15}, -title = {{New constraints on the free-streaming of warm dark matter from intermediate and small scale Lyman- $\alpha$ forest data}}, -volume = {96}, -year = {2017} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and discs are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disc components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to Calar Alto Integral Field Area integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux, they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Dynamics,Galaxies: elliptical and lenticular,Galaxies: kinematics}, -number = {2}, -pages = {2024--2033}, -title = {{Untangling galaxy components: Full spectral bulge-disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {466}, -year = {2017} -} -@article{Quinn2016, -abstract = {We present the new Very Large Array 22 GHz and extended Multi-Element Remote-Linked Interferometer Network 5 GHz observations of CLASS B1030+074, a two-image strong gravitational lens system whose background source is a compact flat-spectrum radio quasar. In such systems we expect a third image of the background source to form close to the centre of the lensing galaxy. The existence and brightness of such images is important for investigation of the central mass distributions of lensing galaxies, but only one secure detection has been made so far in a galaxy-scale lens system. The noise levels achieved in our new B1030+074 images reach 3 $\mu$Jy beam-1 and represent an improvement in central image constraints of nearly an order of magnitude over previous work, with correspondingly better resulting limits on the shape of the central mass profile of the lensing galaxy. Simple models with an isothermal outer power-law slope now require either the influence of a central supermassive black hole (SMBH), or an inner power-law slope very close to isothermal, in order to suppress the central image below our detection limit. Using the central mass profiles inferred from light distributions in Virgo galaxies, moved to z = 0.5, and matching to the observed Einstein radius, we now find that 45 per cent of such mass profiles should give observable central images, 10 per cent should give central images with a flux density still below our limit, and the remaining systems have extreme demagnification produced by the central SMBH. Further observations of similar objects will therefore allow proper statistical constraints to be placed on the central properties of elliptical galaxies at high redshift.}, -archivePrefix = {arXiv}, -arxivId = {1604.00173}, -author = {Quinn, Jonathan and Jackson, Neal and Tagore, Amitpal and Biggs, Andrew and Birkinshaw, Mark and Chapman, Scott and {De Zotti}, Gianfranco and McKean, John and P{\'{e}}rez-Fournon, Ismael and Scott, Douglas and Serjeant, Stephen}, -doi = {10.1093/mnras/stw773}, -eprint = {1604.00173}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Galaxies: evolution,Gravitational lensing: strong,Quasars: individual: CLASS B1030+074}, -month = {apr}, -number = {3}, -pages = {2394--2407}, -title = {{A new VLA/e-MERLIN limit on central images in the gravitational lens system CLASS B1030+074}}, -volume = {459}, -year = {2016} -} -@article{Ullio2002, -abstract = {We investigate the prospects of detecting weakly interacting massive particle (WIMP) dark matter by measuring the contribution to the extragalactic gamma-ray radiation induced, in any dark matter halo and at all redshifts, by WIMP pair annihilations into high-energy photons. We perform a detailed analysis of the very distinctive spectral features of this signal, recently proposed in a short letter by three of the authors: The gamma-ray flux which arises from the decay of (Formula presented) mesons produced in the fragmentation of annihilation final states shows a severe cutoff close to the value of the WIMP mass. An even more spectacular signature appears for the monochromatic gamma-ray components, generated by WIMP annihilations into two-body final states containing a photon: the combined effect of cosmological redshift and absorption along the line of sight produces sharp bumps, peaked at the rest frame energy of the lines and asymmetrically smeared to lower energies. The level of the flux depends both on the particle physics scenario for WIMP dark matter (we consider, as our template case, the lightest supersymmetric particle in a few supersymmetry breaking schemes), and on the question of how dark matter clusters. Uncertainties introduced by the latter are thoroughly discussed implementing a realistic model inspired by results of the state-of-the-art N-body simulations and semianalytic modeling in the cold dark matter structure formation theory. We also address the question of the potential gamma-ray background originating from active galaxies, presenting a novel calculation and critically discussing the assumptions involved and the induced uncertainties. Furthermore, we apply a realistic model for the absorption of gamma-rays on the optical and near-IR intergalactic radiation field to derive predictions for both the signal and background. Comparing the two, we find that there are viable configurations, in the combined parameter space defined by the particle physics setup and the structure formation scenario, for which the WIMP induced extragalactic gamma-ray signal will be detectable in the new generation of gamma-ray telescopes such as GLAST. {\textcopyright} 2002 The American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0207125v1}, -author = {Lacey, Cedric and Edsj{\"{o}}, Joakim}, -doi = {10.1103/PhysRevD.66.123502}, -eprint = {0207125v1}, -issn = {15502368}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -number = {12}, -pages = {123502}, -primaryClass = {arXiv:astro-ph}, -title = {{Cosmological dark matter annihilations into [Formula Presented] rays: A closer look}}, -volume = {66}, -year = {2002} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2012} -} -@article{Minka2008, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms for probabilistic inference, such as expectation propagation. However, message passing in mixture models is not well captured by factor graphs unless the entire mixture is represented by one factor, because the message equations have a containment structure. Gates capture this containment structure graphically, allowing both the independences and the message-passing equations for a model to be readily visualized. Different variational approximations for mixture models can be understood as different ways of drawing the gates in a model. We present general equations for expectation propagation and variational message passing in the presence of gates.}, -author = {Minka, Tom and Winn, John}, -month = {dec}, -number = {MSR-TR-2008-185}, -title = {{Gates : A graphical notation for mixture models}}, -url = {https://www.microsoft.com/en-us/research/publication/gates-a-graphical-notation-for-mixture-models/}, -year = {2008} -} -@article{Keres2005, -abstract = {We examine the temperature history of gas accreted by forming galaxies in smoothed particle hydrodynamics simulations. About half of the gas follows the track expected in the conventional picture of galaxy formation, shock heating to roughly the virial temperature of the galaxy potential well (T ∼ 10 6 K for a Milky Way type galaxy) before cooling, condensing and forming stars. However, the other half radiates its acquired gravitational energy at much lower temperatures, typically T {\textless} 105 K, and the histogram of maximum gas temperatures is clearly bimodal. The 'cold mode' of gas accretion dominates for low-mass galaxies (baryonic mass M gal ≲ 1010.3 M⊙ or halo mass M halo ≲ 1011.4 M⊙),while the conventional 'hot mode' dominates the growth of high-mass systems. Cold accretion is often directed along filaments, allowing galaxies to efficiently draw gas from large distances, while hot accretion is quasispherical. The galaxy and halo mass dependence leads to redshift and environment dependence of cold and hot accretion rates, with the cold mode dominating at high redshift and in low-density regions today, and the hot mode dominating in group and cluster environments at low redshift. The simulations reproduce an important feature of the observed relation between the galaxy star formation rate (SFR) and the environment, namely a break in star formation rates at surface densities $\Sigma$ ∼ 1 h752 Mpc-2, outside the virial radii of large groups and clusters. The cosmic SFR tracks the overall history of gas accretion, and its decline at low redshift follows the combined decline of cold and hot accretion rates. The drop in cold accretion is driven by the decreasing infall rate on to haloes, while for hot accretion this slower mass growth is further modified by the longer cooling times within haloes. If we allowed hot accretion to be suppressed by conduction or active galactic nuclei feedback, then the simulation predictions would change in interesting ways, perhaps resolving conflicts with the colours of ellipticals and the cut-off of the galaxy luminosity function. The transition at Mhalo ∼ 1011.4 M⊙ between cold-mode domination and hot-mode domination is similar to that found by Birnboim {\&} Dekel using one-dimensional simulations and analytic arguments. The corresponding baryonic mass is tantalizingly close to the scale at which Kauffmann et al. find a marked shift in galaxy properties, and we speculate on possible connections between these theoretical and observational transitions. {\textcopyright}2005 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0407095}, -author = {Kere{\v{s}}, Du{\v{s}}an and Katz, Neal and Weinberg, David H and Dav{\'{e}}, Romeel}, -doi = {10.1111/j.1365-2966.2005.09451.x}, -eprint = {0407095}, -isbn = {doi:10.1111/j.1365-2966.2005.09451.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cooling flows,Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {oct}, -number = {1}, -pages = {2--28}, -pmid = {16417727}, -primaryClass = {astro-ph}, -title = {{How do galaxies get their gas?}}, -volume = {363}, -year = {2005} -} -@article{MinkaT.2008, -abstract = {Gates are a new notation for representing mixture models and context-sensitive independence in factor graphs. Factor graphs provide a natural representation for message-passing algorithms, such as expectation propagation. However, message passing in mixture}, -author = {Zarocostas, John}, -doi = {10.1136/bmj.d706}, -issn = {14685833}, -journal = {BMJ (Clinical research ed.)}, -pages = {16}, -pmid = {21285225}, -title = {{Gates and Cameron pledge new money to eradicate polio.}}, -volume = {342}, -year = {2011} -} -@article{Belfiore2017, -abstract = {We study radial profiles in H{\$}\backslashalpha{\$} equivalent width and specific star formation rate (sSFR) derived from spatially-resolved SDSS-IV MaNGA spectroscopy to gain insight on the physical mechanisms that suppress star formation and determine a galaxy's location in the SFR-{\$}\backslashrm M{\_}\backslashstar{\$} diagram. Even within the star-forming `main sequence', the measured sSFR decreases with stellar mass, both in an integrated and spatially-resolved sense. Flat sSFR radial profiles are observed for {\$}\backslashrm log(M{\_}\backslashstar/ M{\_}\backslashodot) {\textless} 10.5{\$}, while star-forming galaxies of higher mass show a significant decrease in sSFR in the central regions, a likely consequence of both larger bulges and an inside-out growth history. Our primary focus is the green valley, constituted by galaxies lying below the star formation main sequence, but not fully passive. In the green valley we find sSFR profiles that are suppressed with respect to star-forming galaxies of the same mass at all galactocentric distances out to 2 effective radii. The responsible quenching mechanism therefore appears to affect the entire galaxy, not simply an expanding central region. The majority of green valley galaxies of {\$}\backslashrm log(M{\_}\backslashstar/ M{\_}\backslashodot) {\textgreater} 10.0{\$} are classified spectroscopically as central low-ionisation emission-line regions (cLIERs). Despite displaying a higher central stellar mass concentration, the sSFR suppression observed in cLIER galaxies is not simply due to the larger mass of the bulge. Drawing a comparison sample of star forming galaxies with the same {\$}\backslashrm M{\_}\backslashstar{\$} and {\$}\backslashrm \backslashSigma{\_}{\{}1{\\sim{}}kpc{\}}{\$} (the mass surface density within 1 kpc), we show that a high {\$}\backslashrm \backslashSigma{\_}{\{}1{\\sim{}}kpc{\}}{\$} is not a sufficient condition for determining central quiescence.}, -archivePrefix = {arXiv}, -arxivId = {1710.05034}, -author = {Belfiore, Francesco and Maiolino, Roberto and Bundy, Kevin and Masters, Karen and Bershady, Matthew and Oyarz{\'{u}}n, Grecco A and Lin, Lihwai and Cano-Diaz, Mariana and Wake, David and Spindler, Ashley and Thomas, Daniel and Brownstein, Joel R and Drory, Niv and Yan, Renbin}, -doi = {10.1093/mnras/sty768}, -eprint = {1710.05034}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Evolution,Galaxies: Fundamental parameters,Galaxies: ISM}, -number = {3}, -pages = {3014--3029}, -title = {{SDSS IV MaNGA - sSFR profiles and the slow quenching of discs in green valley galaxies}}, -url = {http://arxiv.org/abs/1710.05034}, -volume = {477}, -year = {2018} -} -@article{Brooks2015a, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Tenneti2016, -abstract = {We study the shapes and intrinsic alignments of discs and elliptical galaxies in the MassiveBlack-II (MBII) and Illustris cosmological hydrodynamic simulations, with volumes of (100 h-1 Mpc)3and (75 h-1 Mpc)3, respectively. We find that simulated disc galaxies are more oblate in shape and more misaligned with the shape of their host dark matter subhalo when compared with ellipticals. The discmajor axis is found to be oriented towards the location of nearby elliptical galaxies. We also find that the discs are thinner in MBII and misalignments with dark matter halo orientations are smaller in both discs and ellipticals when compared with Illustris. As a result, the intrinsic alignment correlation functions at fixed mass have a higher amplitude in MBII than in Illustris. Finally, at scales above {\$\sim${}}0.1 h-1 Mpc, the intrinsic alignment two-point correlation functions for disc galaxies in both simulations are consistent with a null detection, unlike those for ellipticals. Despite significant differences in the treatments of hydrodynamics and baryonic physics in the simulations, we find that the w$\delta$ + correlation function scales similarly with transverse separation. However, the less massive galaxies show different scale dependence in the ellipticity-direction correlation. This result indicates that, while hydrodynamic simulations are a promising tool to study intrinsic alignments, further study is needed to understand the impact of differences in the implementations of hydrodynamics and baryonic feedback.}, -archivePrefix = {arXiv}, -arxivId = {1510.07024}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana}, -doi = {10.1093/mnras/stw1823}, -eprint = {1510.07024}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies,Gravitational lensing: weak,Hydrodynamics,Kinematics and dynamics,Methods,Numerical}, -number = {3}, -pages = {2668--2680}, -title = {{Intrinsic alignments of disc and elliptical galaxies in the MassiveBlack-II and Illustris simulations}}, -volume = {462}, -year = {2016} -} -@article{Newman2012a, -abstract = {The presence of extremely compact galaxies at z ∼ 2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 galaxies selected with 0.4 {\textless} z {\textless} 2.5 and stellar masses M* {\textgreater} 1010.7 M {\textperiodcentered}in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and the mean size of these systems at fixed stellar mass grows by a factor of 3.5 0.3 over this redshift interval. The data are sufficiently deep to identify companions to these hosts whose stellar masses are ten times smaller. By searching for these around 404 quiescent hosts within a physical annulus 10 h -1 kpc {\textless} R {\textless} 30 h -1 kpc, we estimate the minor merger rate over 0.4 {\textless} z {\textless} 2. We find that 13{\%}-18{\%} of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6{\%} ± 2{\%} per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers may explain most of the size evolution observed at z ≲ 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes. {\textcopyright}2012 The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1110.1637}, -author = {Newman, Andrew B and Ellis, Richard S and Bundy, Kevin and Treu, Tommaso}, -doi = {10.1088/0004-637X/746/2/162}, -eprint = {1110.1637}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: fundamental parameters,galaxies: structure}, -number = {2}, -title = {{Can minor merging account for the size growth of quiescent galaxies? New results from the CANDELS survey}}, -volume = {746}, -year = {2012} -} -@article{Geometryee, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Thomas2016, -abstract = {Quasars are associated with and powered by the accretion of material onto massive black holes; the detection of highly luminous quasars with redshifts greater than z = 6 suggests that black holes of up to ten billion solar masses already existed 13 billion years ago. Two possible present-day 'dormant' descendants of this population of 'active' black holes have been found in the galaxies NGC 3842 and NGC 4889 at the centres of the Leo and Coma galaxy clusters, which together form the central region of the Great Wall - the largest local structure of galaxies. The most luminous quasars, however, are not confined to such high-density regions of the early Universe; yet dormant black holes of this high mass have not yet been found outside of modern-day rich clusters. Here we report observations of the stellar velocity distribution in the galaxy NGC 1600 - a relatively isolated elliptical galaxy near the centre of a galaxy group at a distance of 64 megaparsecs from Earth. We use orbit superposition models to determine that the black hole at the centre of NGC 1600 has a mass of 17 billion solar masses. The spatial distribution of stars near the centre of NGC 1600 is rather diffuse. We find that the region of depleted stellar density in the cores of massive elliptical galaxies extends over the same radius as the gravitational sphere of influence of the central black holes, and interpret this as the dynamical imprint of the black holes.}, -author = {Thomas, Jens and Ma, Chung Pei and McConnell, Nicholas J. and Greene, Jenny E. and Blakeslee, John P. and Janish, Ryan}, -doi = {10.1038/nature17197}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Thomas2017ABigBH.pdf:pdf}, -issn = {14764687}, -journal = {Nature}, -number = {7599}, -pages = {340--342}, -title = {{A 17-billion-solar-mass black hole in a group galaxy with a diffuse core}}, -volume = {532}, -year = {2016} -} -@article{Oman2017, -abstract = {We use 'mock' interferometric HI measurements and a conventional tilted-ring modelling procedure to estimate rotation curves of dwarf galaxy discs from the APOSTLE suite of {\{}{\$}\backslash{\$}Lambda{\}}CDM cosmological hydrodynamical simulations. The modelling yields a large diversity of rotation curves for an individual galaxy, depending on the line-of-sight orientation. The diversity is driven by non-circular motions in the gas; in particular, by strong bisymmetric fluctuations in the azimuthal velocities that the tilted-ring model is ill-suited to account for and that are difficult to detect in model residuals. Large under-estimates of the circular velocity can result when the kinematic major axis coincides with the minima of the fluctuation pattern, mimicking the presence of kiloparsec-scale 'cores', when none are actually present. The thickness of APOSTLE discs accentuates the effect, as slowly-rotating extraplanar gas systematically reduces the average line-of-sight speeds in the inner regions. APOSTLE dwarf galaxies compare favourably with observations in terms of the mass, size and kinematics of their HI discs, although the amplitude of their non-circular motions appears somewhat larger than in quiescent discs from the THINGS and LITTLE THINGS surveys. Non-circular motions provide a compelling explanation for the large apparent cores observed in galaxies such as DDO 47 and DDO 87, where such motions are clearly present and might have negatively affected estimates of the inner circular velocities. We argue that non-circular motions might help reconcile the inner rotation cuves of disc galaxies with the 'cusps' expected in cold dark matter-dominated galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1706.07478}, -author = {Oman, Kyle A and Marasco, Antonino and Navarro, Julio F and Frenk, Carlos S and Schaye, Joop and Ben{\'{i}}tez-Llambay, Alejandro}, -eprint = {1706.07478}, -issn = {16740068}, -keywords = {dark matter,dy-,galaxies,haloes,ism,kinematics,structure}, -number = {June}, -title = {{Apparent cores and non-circular motions in the HI discs of simulated galaxies}}, -url = {http://arxiv.org/abs/1706.07478}, -volume = {000}, -year = {2017} -} -@article{Wang2013, -abstract = {We investigate the spatial distribution of galactic satellites in high-resolution simulations of structure formation in the $\Lambda$ cold dark matter ($\Lambda$CDM) model: the Aquarius dark matter simulations of individual haloes and the Millennium-II simulation of a large cosmological volume. To relate the simulations to observations of the Milky Way we use two alternative models to populate dark haloes with 'visible' galaxies: a semi-analytic model of galaxy formation and an abundance matching technique. We find that the radial density profile of massive satellites roughly follows that of the dark matter halo (unlike the distribution of dark matter subhaloes). Furthermore, our two galaxy formation models give resultsconsistent with the observed profile of the 11 classical satellites of the Milky Way. Our simulations predict that larger, fainter samples of satellites should still retain this profile at least up to samples of 100 satellites. The angular distribution of the classical satellites of the Milky Way is known to be highly anisotropic. Depending on the exact measure of flattening, 5-10 per cent of satellite systems in our simulations are as flat as the Milky Way's and this fraction does not change when we correct for possible obscuration of satellites by the Galactic disc. A moderate flattening ofsatellite systems is a general property of $\Lambda$CDM, best understood as the consequence of preferential accretion along filaments of the cosmic web. Accretion of a single rich group of satellites can enhance the flattening due to such anisotropic accretion. We verify that a typical Milky Way-mass cold dark matter halo does not acquire its 11 most massive satellites from a small number of rich groups. Single-group accretion becomes more likely for less massive satellites. Our model predictions should be testable with forthcoming studies of satellite systems in other galaxies and surveys of fainter satellites in the MilkyWay. {\textcopyright}2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1206.1340}, -author = {Wang, Jie and Frenk, Carlos S and Cooper, Andrew P}, -doi = {10.1093/mnras/sts442}, -eprint = {1206.1340}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxy: formation,Galaxy: structure,Methods: numerical}, -number = {2}, -pages = {1502--1513}, -title = {{The spatial distribution of galactic satellites in the $\Lambda$ cold dark matter cosmology}}, -volume = {429}, -year = {2013} -} -@article{Kormendy2013a, -abstract = {We construct the Faber-Jackson correlation between velocity dispersion $\sigma$ and total galaxy luminosity LV separately for elliptical galaxies with and without cores. The coreless ellipticals show the well-known, steep relationship dlog $\sigma$/dlog LV = 0.268 or LV $\alpha$$\sigma$3.74. This corresponds to dlog $\sigma$/dlog M = 0.203, where M is the stellar mass and we use M/L$\alpha$L 0.32. In contrast, the velocity dispersions of core ellipticals increase much more slowly with LV and M: dlog $\sigma$/dlog LV = 0.120, LV $\alpha$$\sigma$8.33, and dlog $\sigma$/dlog M = 0.091. Dissipationless major galaxy mergers are expected to preserve $\sigma$ according to the simplest virial-theorem arguments. However, numerical simulations show that $\sigma$ increases slowly in dry major mergers, with dlog $\sigma$/dlog M ≃ +0.15. In contrast, minor mergers cause $\sigma$ to decrease, with dlog $\sigma$/dlog M ≃ -0.05. Thus, the observed relation argues for dry major mergers as the dominant growth mode of the most massive ellipticals. This is consistent with what we know about the formation of cores. We know no viable way to explain galaxy cores except through dissipationless mergers of approximately equal-mass galaxies followed by core scouring by binary supermassive black holes. The observed, shallow relation for core ellipticals provides further evidence that they formed in dissipationless and predominantly major mergers. Also, it explains the observation that the correlation of supermassive black hole mass with velocity dispersion, M •$\alpha$$\sigma$4, "saturates" at high M • such that M • becomes almost independent of $\sigma$. {\textcopyright} 2013. The American Astronomical Society. All rights reserved..}, -author = {Kormendy, John and Bender, Ralf}, -doi = {10.1088/2041-8205/769/1/L5}, -file = {:C\:/Users/Jammy/Documents/Papers/SMBHs/Kormendy2013CoresEll.pdf:pdf}, -issn = {20418205}, -journal = {ApJL}, -keywords = {black hole physics,cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: formation,galaxies: structure}, -number = {1}, -pages = {5}, -title = {{The L $\alpha$ $\sigma$8 correlation for elliptical galaxies with cores: Relation with black hole mass}}, -volume = {769}, -year = {2013} -} -@article{Smail1999, -abstract = {We present the first results of a sub-millimeter survey of distant clusters using the new Sub-mm Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope. We have mapped fields in two massive, concentrated clusters, A370 at z=0.37 and Cl2244-02 at z=0.33, at wavelengths of 450 and 850-um. The resulting continuum maps cover a total area of about 10 sq. arcmin to 1 sigma noise levels less than 14 and 2 mJy per beam at the two wavelengths, 2-3 orders of magnitude deeper than was previously possible. We have concentrated on lensing clusters to exploit the amplification of all background sources by the cluster, improving the sensitivity by a factor of 1.3--2 as compared with a blank-field survey. A cumulative source surface density of (2.4+/-1.0) x 10^3 per sq. degree is found to a 50% completeness limit of $\sim$4 mJy at 850-um. The sub-mm spectral properties of these sources indicate that the majority lie at high redshift, z>1. Without correcting for lens amplification, our observations limit the blank-field counts at this depth. The surface density is 3 orders of magnitude greater than the expectation of a non-evolving ber density of strongly star-forming galaxies in the high-redshift Universe and suggest that optical surveys may have substantial underestimated the star formation density in the distant Universe. Deeper sub-mm surveys with SCUBA should detect large numbers of star-forming galaxies at high redshift, and so provide strong constraints on the formation of normal galaxies.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9708135}, -author = {Smail, Ian and Ivison, R. J. and Blain, A. W.}, -doi = {10.1086/311017}, -eprint = {9708135}, -issn = {0004637X}, -journal = {The Astrophysical Journal}, -keywords = {COSMOLOGY: EARLY UNIVERSE,COSMOLOGY: GRAVITATIONAL LENSING,COSMOLOGY: OBSERVATIONS,Cosmology: Early Universe,Cosmology: Gravitational Lensing,Cosmology: Observations,GALAXIES: EVOLUTION,GALAXIES: FORMATION,Galaxies: Evolution,Galaxies: Formation,RADIO CONTINUUM: GALAXIES,Radio Continuum: Galaxies}, -number = {1}, -pages = {L5--L8}, -primaryClass = {astro-ph}, -title = {{A Deep Submillimeter Survey of Lensing Clusters: A New Window on Galaxy Formation and Evolution}}, -url = {http://arxiv.org/abs/astro-ph/9708135%0Ahttp://dx.doi.org/10.1086/311017}, -volume = {490}, -year = {1997} -} -@article{He2024, -abstract = {In a strong gravitational lensing system, the distorted light from a source is analysed to infer the properties of the lens. However, light emitted by the lens itself can contaminate the image of the source, introducing systematic errors in the analysis. We present a simple and efficient lens light model based on the well-tested multi-Gaussian expansion (MGE) method for representing galaxy surface brightness profiles, which we combine with a semi-linear inversion scheme for pixelized source modelling. Testing it against realistic mock lensing images, we show that our scheme can fit the lensed images to the noise level, with relative differences between the true input and best-fit lens light model remaining below 5%. We apply the MGE lens light model to 38 lenses from the HST SLACS sample. We find that the new scheme provides a good fit for the majority of the sample with only 3 exceptions -- these show clear asymmetric residuals in the lens light. We examine the radial dependence of the ellipticity and position angles and confirm that it is common for a typical lens galaxy to exhibit twisting, non-elliptical isophotes and boxy / disky isophotes. Our MGE lens light model will be a valuable tool for understanding the hidden complexity of the lens mass distribution.}, -archivePrefix = {arXiv}, -arxivId = {2403.16253}, -author = {He, Qiuhan and Nightingale, James W. and Amvrosiadis, Aris and Robertson, Andrew and Cole, Shaun and Frenk, Carlos S. and Massey, Richard and Li, Ran and Cao, Xiaoyue and Lange, Samuel C. and Fran{\c{c}}a, Jo{\~{a}}o Paulo C.}, -eprint = {2403.16253}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/He2024MGE.pdf:pdf}, -keywords = {galaxies,gravitational lensing,image processing,photometry,strong,structure,techniques}, -number = {March}, -pages = {1--20}, -title = {{Unveiling Lens Light Complexity with A Novel Multi-Gaussian Expansion Approach for Strong Gravitational Lensing}}, -url = {http://arxiv.org/abs/2403.16253}, -volume = {20}, -year = {2024} -} -@article{Bois2011, -abstract = {We study the formation of early-type galaxies (ETGs) through mergers with a sample of 70 high-resolution (softening length <60pc and 12 × 10 6 particles) numerical simulations of binary mergers of disc galaxies (with 10 per cent of gas) and 16 simulations of ETG remergers. These simulations, designed to accompany observations and models conducted within the ATLAS 3D project, encompass various mass ratios (from 1:1 to 6:1), initial conditions and orbital parameters. The progenitor disc galaxies are spiral-like with bulge-to-disc ratios typical of Sb and Sc galaxies and high central baryonic angular momentum. We find that binary mergers of disc galaxies with mass ratios of 3:1 and 6:1 are nearly always classified as fast rotators according to the ATLAS 3D criterion (based on the $\lambda$ R parameter - ATLAS 3D Paper III): they preserve the structure of the input fast rotating spiral progenitors. They have intrinsic ellipticities larger than 0.5, cover intrinsic $\lambda$ R values between 0.2 and 0.6, within the range of observed fast rotators. The distribution of the observed fastest rotators does in fact coincide with the distribution of our disc progenitors. Major disc mergers (mass ratios of 2:1 and 1:1) lead to both fast and slow rotators. Most of the fast rotators produced in major mergers have intermediate flattening, with ellipticities $\epsilon$ between 0.4 and 0.6. Most slow rotators formed in these binary disc mergers hold a stellar kinematically distinct core (KDC) in their $\sim$1-3 central kiloparsec: these KDCs are built from the stellar components of the progenitors. However, these remnants are still very flat with $\epsilon$ often larger than 0.45 and sometimes as high as 0.65. Besides a handful of specific observed systems - the counter-rotating discs (2$\sigma$ galaxies, ATLAS 3D Paper II) - these therefore cannot reproduce the observed population of slow rotators in the nearby Universe. This sample of simulations supports the notion of slow and fast rotators: these two families of ETGs present distinct characteristics in term of their angular momentum content (at all radii) and intrinsic properties - the slow rotators are not simply velocity-scaled down versions of fast rotators. The mass ratio of the progenitors is a fundamental parameter for the formation of slow rotators in these binary mergers, but it also requires a retrograde spin for the earlier-type (Sb) progenitor galaxy with respect to the orbital angular momentum. We also study remergers of these merger remnants: these produce relatively round fast rotators or systems near the threshold for slow rotators. In such cases, the orbital angular momentum dominates the central region, and these systems no longer exhibit a KDC, as KDCs are destroyed during the remergers and do not re-form in these relatively dry events. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1105.4076}, -author = {Bois, Maxime and Emsellem, Eric and Bournaud, Fr{\'{e}}d{\'{e}}ric and Alatalo, Katherine and Blitz, Leo and Bureau, Martin and Cappellari, Michele and Davies, Roger L. and Davis, Timothy A. and de Zeeuw, P. T. and Duc, Pierre Alain and Khochfar, Sadegh and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Weijmans, Anne Marie and Young, Lisa M.}, -doi = {10.1111/j.1365-2966.2011.19113.x}, -eprint = {1105.4076}, -isbn = {9781595937629}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: formation,Galaxies: interactions,Galaxies: kinematics and dynamics,Methods: numerical}, -number = {3}, -pages = {1654--1679}, -title = {{The ATLAS 3D project - VI. Simulations of binary galaxy mergers and the link with fast rotators, slow rotators and kinematically distinct cores}}, -url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.19113.x%5Cnhttp://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.19113.x/full}, -volume = {416}, -year = {2011} -} -@article{Er2019, -abstract = {Plasma lensing is the refraction of low-frequency electromagnetic rays due to free electrons in the interstellar medium. Although the phenomenon has a distinct similarity to gravitational lensing, particularly in its mathematical description, plasma lensing introduces other additional features, such as wavelength dependence, radial rather than tangential image distortions, and strong demagnification of background sources. Axisymmetrical models of plasma lenses have been well studied in the literature, but density distributions with more complicated shapes can provide new and exotic image configurations and increase the richness of the magnification properties. As a first step towards non-axisymmetrical distributions, we study two families of elliptical plasma lens, softened power law, and exponential plasma distributions. We perform numerical studies on each lens model, and present them over a parameter space. In addition to deriving elliptical plasma lens formulae, we also investigate the number of critical curves that the lens can produce by studying the lens parameter space, in particular the dependence on the lensing ellipticity. We find that the introduction of ellipticity into the plasma distribution can enhance the lensing effects as well as the complexity of the magnification map.}, -archivePrefix = {arXiv}, -arxivId = {1907.10787}, -author = {Er, Xinzhong and Rogers, Adam}, -doi = {10.1093/mnras/stz2073}, -eprint = {1907.10787}, -file = {:C\:/Users/Jammy/Documents/Papers/FRBLenses/Er2019TwoFamiliesPlasmaLenses.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: micro,Gravitational lensing: strong,Interstellar medium: general}, -number = {4}, -pages = {5651--5664}, -title = {{Two families of elliptical plasma lenses}}, -volume = {488}, -year = {2019} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo {\textgreater} 1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from {\$\sim${}}30° to 10° for M {\$\sim${}} 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles. {\textcopyright}2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@article{Hall2014, -abstract = {The science goals of space missions from the Hubble Space Telescope through to Gaia and Euclid require ultraprecise positional, photometric, and shape measurement information. However, in the radiation environment of the space telescopes, damage to the focal plane detectors through high-energy protons leads to the creation of traps, a loss of charge transfer efficiency, and a consequent deterioration in measurement accuracy. An understanding of the traps produced and their properties in the CCD during operation is essential to allow optimization of the devices and suitable modeling to correct the effect of the damage through the postprocessing of images. The technique of 'pumping single traps' has allowed the study of individual traps in high detail that cannot be achieved with other techniques, such as deep level transient spectroscopy, whilst also locating each trap to the subpixel level in the device. Outlining the principles used, we have demonstrated the technique for the A-center, the most influential trap in serial readout, giving results consistent with the more general theoretical values, but here showing new results indicating the spread in the emission times achieved and the variation in capture probability of individual traps with increasing signal levels. This technique can now be applied to other time and temperature regimes in the CCD to characterize individual traps in situ under standard operating conditions such that dramatic improvements can be made to optimization processes and modeling techniques. {\textcopyright}2013 IEEE.}, -author = {Hall, David J and Murray, Neil J and Holland, Andrew D and Gow, Jason and Clarke, Andrew and Burt, David}, -doi = {10.1109/TNS.2013.2295941}, -isbn = {9781467350570}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {A-centre,CCD image sensors,Euclid,Si-A,defect,pocket pumping,radiation damage,trap pumping}, -number = {4}, -pages = {1826--1833}, -title = {{Determination of in situ trap properties in CCDs using a "single-trap pumping" technique}}, -volume = {61}, -year = {2014} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ($\sim$100 deg2) and deep (>28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of $\sim$7000 massive galaxies at z $\sim$ 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E. and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Huang et al. - 2018 - Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 z 0.5 using Hyper Suprime-Cam(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 < z < 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Handley2015a, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W. J. and Hobson, M. P. and Lasenby, A. N.}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Handley, Hobson, Lasenby - 2015 - POLYCHORD Next-generation nested sampling(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Lee2016, -abstract = {We study how properties of discrete dark matter halos depend on halo environment, characterized by the mass density around the halos on scales from 0.5 to 16 {\$}h{\^{}}{\{}-1{\}}{\{}\backslashrm Mpc{\}}{\$}. We find that low mass halos (those less massive than the characteristic mass {\$}M{\_}{\{}\backslashrm C{\}}{\$} of halos collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations, and rounder shapes than halos in median density environments. Halos in median and low-density environments have similar accretion rates and concentrations, but halos in low density environments have lower spins and are more elongated. Halos of a given mass in high-density regions accrete material earlier than halos of the same mass in lower-density regions. All but the most massive halos in high-density regions are losing mass (i.e., being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low mass halos in high density regions at low redshifts {\$}z {\textless} 1{\$}, by preferentially removing higher angular momentum material from halos. Halos in low-density regions have lower than average spins because they lack nearby halos whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an Extreme Value Distribution, and that the density distribution becomes broader with cosmic time.}, -archivePrefix = {arXiv}, -arxivId = {1610.02108}, -author = {Lee, Christoph T and Primack, Joel R and Behroozi, Peter and Rodr{\'{i}}guez-Puebla, Aldo and Hellinger, Doug and Dekel, Avishai}, -doi = {10.1093/mnras/stw3348}, -eprint = {1610.02108}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology,Halos -Methods,Large Scale Structure -Dark Matter -Galaxies,Numerical}, -number = {4}, -pages = {3834--3858}, -title = {{Properties of dark matter haloes as a function of local environment density}}, -url = {http://arxiv.org/abs/1610.02108%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3348}, -volume = {466}, -year = {2017} -} -@article{Tian2017, -abstract = {We study the Mass Discrepancy-Acceleration Relation (MDAR) of 57 elliptical galaxies by their Einstein rings from the Sloan Lens ACS Survey (SLACS). The mass discrepancy between the lensing mass and the baryonic mass derived from population synthesis is larger when the acceleration of the elliptical galaxy lenses is smaller. The MDAR is also related to surface mass density discrepancy. At the Einstein ring, these lenses belong to high-surface-mass density galaxies. Similarly, we find that the discrepancy between the lensing and stellar surface mass density is small. It is consistent with the recent discovery of dynamical surface mass density discrepancy in disk galaxies where the discrepancy is smaller when surface density is larger. We also find relativistic modified Newtonian dynamics (MOND) can naturally explain the MDAR and surface mass density discrepancy in 57 Einstein rings. Moreover, the lensing mass, the dynamical mass and the stellar mass of these galaxies are consistent with each other in relativistic MOND.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1702.00183}, -author = {Tian, Yong and Ko, Chung Ming}, -doi = {10.1093/MNRAS/STX2056}, -eprint = {1702.00183}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: kinematics and dynamics,Dark matter,Galaxies: elliptical and lenticular,Gravitation,Gravitational lensing: strong}, -number = {1}, -pages = {765--771}, -title = {{Mass discrepancy-acceleration relation in Einstein rings}}, -url = {http://arxiv.org/abs/1702.00183}, -volume = {472}, -year = {2017} -} -@article{Schombert2015a, -abstract = {Using isophotal radius correlations for a sample of 2MASS ellipticals, we have constructed a series of template surface brightness profiles to describe the profile shapes of ellipticals as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that ellipticals are weakly non-homologous with respect to structure. Through comparison to the templates, it is discovered that ellipticals are divided into two families; those well matched to the templates and a second class of ellipticals with distinctly shallower profile slopes. We refer to these second type of ellipticals as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D ellipticals cover the same range of luminosity, size and kinematics as normal ellipticals, but maintain a signature of recent equal mass dry mergers. We propose that normal ellipticals grow after an initial dissipation formation era by accretion of low mass companions as outlined in hierarchical formation scenarios, while D ellipticals are the result of later equal mass mergers producing shallow luminosity profiles.}, -archivePrefix = {arXiv}, -arxivId = {1509.08381}, -author = {Schombert, James M}, -doi = {10.1088/0004-6256/150/5/162}, -eprint = {1509.08381}, -isbn = {doi:10.1088/0004-6256/150/5/162}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: structure}, -number = {5}, -pages = {162}, -publisher = {IOP Publishing}, -title = {{The structure of galaxies. III. Two structural families of ellipticals}}, -url = {http://dx.doi.org/10.1088/0004-6256/150/5/162}, -volume = {150}, -year = {2015} -} -@article{Clifton2012, -abstract = {In this review we present a thoroughly comprehensive survey of recent work on modified theories of gravity and their cosmological consequences. Amongst other things, we cover General Relativity, scalar-tensor, Einstein-{\ae}ther, and Bimetric theories, as well as TeVeS, . f(R), general higher-order theories, Hořava-Lifschitz gravity, Galileons, Ghost Condensates, and models of extra dimensions including Kaluza-Klein, Randall-Sundrum, DGP, and higher co-dimension braneworlds. We also review attempts to construct a Parameterised Post-Friedmannian formalism, that can be used to constrain deviations from General Relativity in cosmology, and that is suitable for comparison with data on the largest scales. These subjects have been intensively studied over the past decade, largely motivated by rapid progress in the field of observational cosmology that now allows, for the first time, precision tests of fundamental physics on the scale of the observable Universe. The purpose of this review is to provide a reference tool for researchers and students in cosmology and gravitational physics, as well as a self-contained, comprehensive and up-to-date introduction to the subject as a whole. {\textcopyright} 2012 Elsevier B.V.}, -archivePrefix = {arXiv}, -arxivId = {1106.2476}, -author = {Clifton, Timothy and Ferreira, Pedro G. and Padilla, Antonio and Skordis, Constantinos}, -doi = {10.1016/j.physrep.2012.01.001}, -eprint = {1106.2476}, -isbn = {0370-1573}, -issn = {03701573}, -journal = {Physics Reports}, -keywords = {Cosmology,General relativity,Gravitational physics,Modified gravity}, -number = {1-3}, -pages = {1--189}, -pmid = {24273347}, -title = {{Modified gravity and cosmology}}, -url = {http://adsabs.harvard.edu/abs/2012PhR...513....1C}, -volume = {513}, -year = {2012} -} -@article{Collett2015, -abstract = {Ongoing and future imaging surveys represent significant improvements in depth, area, and seeing compared to current data sets. These improvements offer the opportunity to discover up to three orders of magnitude more galaxy-galaxy strong lenses than are currently known. In this work we forecast the number of lenses that will be discoverable in forthcoming surveys and simulate their properties. We generate a population of statistically realistic strong lenses and simulate observations of this population for the Dark Energy Survey (DES), the Large Synoptic Survey Telescope (LSST), and Euclid surveys. We verify our model against the galaxy-scale lens search of the Canada-France-Hawaii Telescope Legacy Survey, predicting 250 discoverable lenses compared to 220 found by Gavazzi et al. The predicted Einstein radius distribution is also remarkably similar to that found by Sonnenfeld et al. For future surveys we find that, assuming Poisson limited lens galaxy subtraction, searches of the DES, LSST, and Euclid data sets should discover 2400, 120000, and 170000 galaxy-galaxy strong lenses, respectively. Finders using blue-minus-red (g - i) difference imaging for lens subtraction can discover 1300 and 62000 lenses in DES and LSST. The uncertainties on the model are dominated by the high-redshift source population, which typically gives fractional errors on the discoverable lens number at the level of tens of percent. We find that doubling the signal-to-noise ratio required for a lens to be detectable approximately halves the number of detectable lenses in each survey, indicating the importance of understanding the selection function and the sensitivity of future lens finders in interpreting strong lens statistics. We make our population forecasting and simulated observation codes publicly available so that the selection function of strong lens finders can easily be calibrated.}, -archivePrefix = {arXiv}, -arxivId = {1507.02657}, -author = {Collett, Thomas E.}, -doi = {10.1088/0004-637X/811/1/20}, -eprint = {1507.02657}, -isbn = {0004-637x}, -issn = {15384357}, -journal = {ApJ}, -keywords = {gravitational lensing: strong}, -number = {1}, -pages = {20}, -title = {{The population of galaxy-galaxy strong lenses in forthcoming optical imaging surveys}}, -url = {http://arxiv.org/abs/1507.02657}, -volume = {811}, -year = {2015} -} -@article{Libeskind2005, -abstract = {The 11 known satellite galaxies within 250 kpc of the Milky Way lie close to a great circle on the sky. We use high resolution N-body simulations of galactic dark matter halos to test if this remarkable property can be understood within the context of the cold dark matter cosmology. We construct halo merger trees from the simulations and use a semianalytic model to follow the formation of satellite galaxies. We find that in all 6 of our simulations, the 11 brightest satellites are indeed distributed along thin, disk-like structures analogous to that traced by the Milky Way's satellites. This is in sharp contrast to the overall distributions of dark matter in the halo and of subhalos within it which, although triaxial, are not highly aspherical. We find that the spatial distribution of satellites is significantly different from that of the most massive subhalos but is similar to that of the subset of subhalos that had the most massive progenitors at earlier times. The elongated disk-like structure delineated by the satellites has its long axis aligned with the major axis of the dark matter halo. We interpret our results as reflecting the preferential infall of satellites along the spines of a few filaments of the cosmic web.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0503400}, -author = {Libeskind, Noam I and Frenk, Carlos S and Cole, Shaun and Helly, John C and Jenkins, Adrian and Navarro, Julio F and Power, Chris}, -doi = {10.1111/j.1365-2966.2005.09425.x}, -eprint = {0503400}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes}, -number = {1}, -pages = {146--152}, -primaryClass = {astro-ph}, -title = {{The distribution of satellite galaxies: The great pancake}}, -volume = {363}, -year = {2005} -} -@article{Mercier2024, -abstract = {Aims. We provide an in-depth analysis of the COSMOS-Web ring, an Einstein ring at z ≈ 2 that we serendipitously discovered during the data reduction of the COSMOS-Web survey and that could be the most distant lens discovered to date. Methods. We extracted the visible and near-infrared photometry of the source and the lens from more than 25 bands. We combined these observations with far-infrared detections to study the dusty nature of the source and we derived the photometric redshifts and physical properties of both the lens and the source with three different spectral energy distribution (SED) fitting codes. Using JWST/NIRCam images, we also produced two lens models to (i) recover the total mass of the lens, (ii) derive the magnification of the system, (iii) reconstruct the morphology of the lensed source, and (iv) measure the slope of the total mass density profile of the lens. Results. We find the lens to be a very massive elliptical galaxy at z = 2.02 ± 0.02 with a total mass within the Einstein radius of Mtot(<$\theta$Ein = (3.66 ± 0.36) × 1011 M{\textperiodcentered} and a total stellar mass of M∗ = 1.37-0.11+0.14 × 1011 M{\textperiodcentered}. We also estimate it to be compact and quiescent with a specific star formation rate below 10-13 yr. Compared to stellar-to-halo mass relations from the literature, we find that the total mass of the lens within the Einstein radius is consistent with the presence of a dark matter (DM) halo of total mass Mh = 1.09-0.57+1.46 × 1013 M{\textperiodcentered}. In addition, the background source is a M∗ = (1.26 ± 0.17) × 1010 M{\textperiodcentered} star-forming galaxy (SFR ≈ (78 ± 15) M{\textperiodcentered} yr) at z = 5.48 ± 0.06. The morphology reconstructed in the source plane shows two clear components with different colors. Dust attenuation values from SED fitting and nearby detections in the far infrared also suggest that the background source could be at least partially dust-obscured. Conclusions. We find the lens at z ≈ 2. Its total, stellar, and DM halo masses are consistent within the Einstein ring, so we do not need any unexpected changes in our description of the lens such as changing its initial mass function or including a non-negligible gas contribution. The most likely solution for the lensed source is at z ≈ 5.5. Its reconstructed morphology is complex and highly wavelength dependent, possibly because it is a merger or a main sequence galaxy with a heterogeneous dust distribution.}, -archivePrefix = {arXiv}, -arxivId = {2309.15986}, -author = {Mercier, W. and Shuntov, M. and Gavazzi, R. and Nightingale, J. W. and Arango, R. and Ilbert, O. and Amvrosiadis, A. and Ciesla, L. and Casey, C. M. and Jin, S. and Faisst, A. L. and Andika, I. T. and Drakos, N. E. and Enia, A. and Franco, M. and Gillman, S. and Gozaliasl, G. and Hayward, C. C. and Huertas-Company, M. and Kartaltepe, J. S. and Koekemoer, A. M. and Laigle, C. and {Le Borgne}, D. and Magdis, G. and Mahler, G. and Maraston, C. and Martin, C. L. and Massey, R. and McCracken, H. J. and Moutard, T. and Paquereau, L. and Rhodes, J. D. and Robertson, B. E. and Sanders, D. B. and Toft, S. and Trebitsch, M. and Tresse, L. and Vijayan, A. P.}, -doi = {10.1051/0004-6361/202348095}, -eprint = {2309.15986}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Mercier2024COSMOSRing.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Galaxies: distances and redshifts,Galaxies: elliptical and lenticular,Galaxies: halos,Galaxies: high-redshift,Gravitation,Gravitational lensing: strong,cD}, -title = {{The COSMOS-Web ring: In-depth characterization of an Einstein ring lensing system at z ∼ 2}}, -volume = {687}, -year = {2024} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and discs are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disc components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to Calar Alto Integral Field Area integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux, they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Dynamics,Galaxies: elliptical and lenticular,Galaxies: kinematics}, -number = {2}, -pages = {2024--2033}, -title = {{Untangling galaxy components: Full spectral bulge-disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {466}, -year = {2017} -} -@article{Bellstedt2018, -abstract = {We apply the Jeans Anisotropic Multi-Gaussian Expansion dynamical modelling method to SAGES Legacy Unifying Globulars and GalaxieS (SLUGGS) survey data of early-type galaxies in the stellar mass range 1010 < M*/M⊙ < 1011.6 that cover a large radial range of 0.1-4.0 effective radii.We combine SLUGGS and ATLAS3D data sets to model the total-mass profiles of a sample of 21 fast-rotator galaxies, utilizing a hyperparameter method to combine the two independent data sets. The total-mass density profile slope values derived for these galaxies are consistent with those measured in the inner regions of galaxies by other studies. Furthermore, the total-mass density slopes ($\gamma$tot) appear to be universal over this broad stellar mass range, with an average value of $\gamma$tot= -2.24± 0.05, i.e. slightly steeper than isothermal. We compare our results to model galaxies from the Magneticum and EAGLE cosmological hydrodynamic simulations, in order to probe the mechanisms that are responsible for varying total-mass density profile slopes. The simulated-galaxy slopes are shallower than the observed values by $\sim$0.3-0.5, indicating that the physical processes shaping the mass distributions of galaxies in cosmological simulations are still incomplete. For galaxies with M* > 1010.7M⊙ in the Magneticum simulations, we identify a significant anticorrelation between total-mass density profile slopes and the fraction of stellar mass formed ex situ (i.e. accreted), whereas this anticorrelation is weaker for lower stellar masses, implying that the measured total-mass density slopes for low-mass galaxies are less likely to be determined by merger activity.}, -archivePrefix = {arXiv}, -arxivId = {1803.02373}, -author = {Bellstedt, Sabine and Forbes, Duncan A. and Romanowsky, Aaron J. and Remus, Rhea Silvia and Stevens, Adam R.H. and Brodie, Jean P. and Poci, Adriano and McDermid, Richard and Alabi, Adebusola and Chevalier, Leonie and Adams, Caitlin and Ferr{\'{e}}-Mateu, Anna and Wasserman, Asher and Pandya, Viraj}, -doi = {10.1093/mnras/sty456}, -eprint = {1803.02373}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bellstedt et al. - 2018 - The SLUGGS survey A comparison of total-mass profiles of early-type galaxies from observations and cosmologica.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: kinematics and dynamics}, -number = {4}, -pages = {4543--4564}, -title = {{The SLUGGS survey: A comparison of total-mass profiles of early-type galaxies from observations and cosmological simulations, to $\sim$4 effective radii}}, -url = {http://arxiv.org/abs/1803.02373%0Ahttp://dx.doi.org/10.1093/mnras/sty456}, -volume = {476}, -year = {2018} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum {\$}j{\_}\backslashstar{\$} and the stellar mass {\$}M{\_}\backslashstar{\$} in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction {\$}f{\_}{\{}\backslashrm inf{\}}{\$} of baryons that infall toward the central regions of galaxies where star formation can occur. We find {\$}f{\_}{\{}\backslashrm inf{\}}\backslashapprox 1{\$} for LTGs and {\$}\backslashapprox 0.4{\$} for ETGs with an uncertainty of about {\$}0.25{\$} dex, consistent with a biased collapse. By comparing with the locally observed {\$}j{\_}\backslashstar{\$} vs. {\$}M{\_}\backslashstar{\$} relations for LTGs and ETGs we estimate the fraction {\$}f{\_}j{\$} of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find {\$}f{\_}j\backslashapprox 1.11{\^{}}{\{}+0.75{\}}{\_}{\{}-0.44{\}}{\$}, in line with the classic disc formation picture; for ETGs we infer {\$}f{\_}j\backslashapprox 0.64{\^{}}{\{}+0.20{\}}{\_}{\{}-0.16{\}}{\$}, that can be traced back to a {\$}z{\textless}1{\$} evolution via dry mergers. We also show that the observed scatter in the {\$}j{\_}{\{}\backslashstar{\}}{\$} vs. {\$}M{\_}{\{}\backslashstar{\}}{\$} relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at {\$}z\backslashsim 2{\$} is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, J and Lapi, A and Mancuso, C and Wang, H and Danese, L}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {2}, -pages = {105}, -title = {{Angular Momentum of Early- and Late-type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -volume = {843}, -year = {2017} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10^11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r_vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of $\sim$25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r_vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bailin, Steinmetz - 2005 - Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos(2).pdf:pdf}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S{\`{e}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as Mh(M*) ∝ reff$\eta$ (M*). We find that, on average, our lens galaxies have an $\eta$ = 0.42 ± 0.12, i.e. larger galaxies live in more massive dark matter haloes. The $\eta$ is strongest for high-mass luminous red galaxies. Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed M*, satellite galaxies have a larger $\eta$ and greater scatter in the Mh and reff relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J L and Hudson, Michael J and Balogh, Michael L and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for {\$\sim${}}20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disk galaxies. Under this bulge-formation model, though, the high rates of mergers in Cold Dark Matter galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disk galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from $\sim$1011 to > 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above $\sim$1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K.}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/K{\"{u}}ng et al. - 2018 - Models of gravitational lens candidates from SpaceWarps CFHTLS(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Banik2019, -abstract = {Strong lensing of active galactic nuclei in the radio can result in razor-thin arcs, with a thickness of less than a milliarcsecond, if observed at the resolution achievable with very long baseline interferometry (VLBI). Such razor-thin arcs provide a unique window on the coarseness of the matter distribution between source and observer. In this paper, we investigate to what extent such razor-thin arcs can constrain the number density and mass function of ‘free-floating' black holes, defined as black holes that do not, or no longer, reside at the centre of a galaxy. These can be either primordial in origin or arise as by-products of the evolution of supermassive black holes in galactic nuclei. When sufficiently close to the line of sight, free-floating black holes cause kink-like distortions in the arcs, which are detectable by eye in the VLBI images as long as the black hole mass exceeds ∼1000 Solar masses. Using a crude estimate for the detectability of such distortions, we analytically compute constraints on the matter density of free-floating black holes resulting from null-detections of distortions along a realistic, fiducial arc, and find them to be comparable to those from quasar milli-lensing. We also use predictions from a large hydrodynamical simulation for the demographics of free-floating black holes that are not primordial in origin and show that their predicted mass density is roughly four orders of magnitude below the constraints achievable with a single razor-thin arc.}, -archivePrefix = {arXiv}, -arxivId = {1811.00637}, -author = {Banik, Uddipan and van den Bosch, Frank C. and Tremmel, Michael and More, Anupreeta and Despali, Giulia and More, Surhud and Vegetti, Simona and McKean, John P.}, -doi = {10.1093/mnras/sty3267}, -eprint = {1811.00637}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Banik2019SMBHRazorArc.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Gravitational lensing: strong,Quasars: supermassive black holes,Techniques: high angular resolution}, -number = {2}, -pages = {1558--1573}, -title = {{Constraining the mass density of free-floating black holes using razor-thin lensing arcs}}, -volume = {483}, -year = {2019} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L. Gabriel and Arg{\"{u}}elles, C. R. and Perlick, Volker and Rueda, J. A. and Ruffini, R.}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/G{\'{o}}mez et al. - 2016 - Strong lensing by fermionic dark matter in galaxies(2).pdf:pdf}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Vulcani2014, -abstract = {We investigate the relationship between colour and structure within galaxies using a large, volume-limited sample of bright, low-redshift galaxies with optical-near-infrared imaging from the Galaxy AndMass Assembly survey.We fit single-component,wavelength-dependent, elliptical S{\'{e}}rsic models to all passbands simultaneously, using software developed by the MegaMorph project. Dividing our sample by n and colour, the recovered wavelength variations in effective radius (Re) and S{\'{e}}rsic index (n) reveal the internal structure, and hence formation history, of different types of galaxies. All these trends depend on n; some have an additional dependence on galaxy colour. Late-type galaxies (nr < 2.5) show a dramatic increase in S{\'{e}}rsic index with wavelength. This might be a result of their two-component (bulge-disc) nature, though stellar population gradients within each component and dust attenuation are likely to play a role. All galaxies show a substantial decrease in Re with wavelength. This is strongest for early types (nr > 2.5), even though they maintain constant n with wavelength, revealing that ellipticals are a superimposition of different stellar populations associated with multiple collapse and merging events. Processes leading to structures with larger Re must be associated with lower metallicity or younger stellar populations. This appears to rule out the formation of young cores through dissipative gas accretion as an important mechanism in the recent lives of luminous elliptical galaxies. {\textcopyright} 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1404.0377}, -author = {Vulcani, Benedetta and Bamford, Steven P. and H{\"{a}}u{\ss}ler, Boris and Vika, Marina and Rojas, Alex and Agius, Nicola K. and Baldry, Ivan and Bauer, Amanda E. and Brown, Michael J.I. and Driver, Simon and Graham, Alister W. and Kelvin, Lee S. and Liske, Jochen and Loveday, Jon and Popescu, Cristina C. and Robotham, Aaron S.G. and Tuffs, Richard J.}, -doi = {10.1093/mnras/stu632}, -eprint = {1404.0377}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxies: fundamental parameters,Galaxies: general,Galaxies: structure}, -month = {jun}, -number = {2}, -pages = {1340--1362}, -title = {{Galaxy and mass assembly (GAMA): The wavelength-dependent sizes and profiles of galaxies revealed by megamorph}}, -volume = {441}, -year = {2014} -} -@inproceedings{Janesick1991, -abstract = {Recent analytical and experimental work has provided new insights into the production of damage sites in silicon Charge-Coupled Devices (CCDs) by energetic particles and into the effects of these sites on CCD performance. An approximate correlation is presented between experimental results and a prediction of proton-induced displacement damage, and possible explanations for remaining inconsistencies are discussed. As a consequence of this agreement, it is now possible to predict the effect of complicated space proton environments upon CCD charge transfer efficiency and other CCD perlormance parameters. This prediction requires evaluation of the damage resulting from only a small number ({\textless}6) of quasi-monoenergetic proton exposures to calibrate the susceptibility of a given device. Finally, prospects for extending this technique to other types of radiation are discussed}, -author = {Janesick, James R and Soli, George B and Elliott, Tom S and Collins, Stewart A}, -booktitle = {Charge-Coupled Devices and Solid State Optical Sensors II}, -doi = {10.1117/12.45317}, -editor = {Blouke, M.\$\sim$M.}, -isbn = {0819405469}, -issn = {0277786X}, -month = {jul}, -number = {2}, -pages = {87--108}, -series = {procspie}, -title = {{Effects of proton damage on charge-coupled devices}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?articleid=960633}, -volume = {1447}, -year = {1991} -} -@article{Dutton2011, -abstract = {We investigate the origin of the relations between stellar mass and optical circular velocity for early-type galaxies (ETGs) and late-type galaxies (LTGs) - the Faber-Jackson (FJ) and Tully-Fisher (TF) relations. We combine measurements of dark halo masses (from satellite kinematics and weak lensing), and the distribution of baryons in galaxies (from a new compilation of galaxy scaling relations), with constraints on dark halo structure from cosmological simulations. The principal unknowns are the halo response to galaxy formation and the stellar initial mass function (IMF). The slopes of the TF and FJ relations are naturally reproduced for a wide range of halo response and IMFs. However, models with a universal IMF and universal halo response cannot simultaneously reproduce the zero-points of both the TF and FJ relations. For a model with a universal Chabrier IMF, LTGs require halo expansion, while ETGs require halo contraction. A Salpeter IMF is permitted for high-mass ($\sigma$≳ 180kms-1) ETGs, but is inconsistent for intermediate masses, unless Vcirc(Re)/$\sigma$e≳ 1.6. If the IMF is universal and close to Chabrier, we speculate that the presence of a major merger may be responsible for the contraction in ETGs while clumpy accreting streams and/or feedback leads to expansion in LTGs. Alternatively, a recently proposed variation in the IMF disfavours halo contraction in both types of galaxies. Finally we show that our models naturally reproduce flat and featureless circular velocity profiles within the optical regions of galaxies without fine-tuning. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1012.5859}, -author = {Dutton, Aaron A. and Conroy, Charlie and van den Bosch, Frank C. and Simard, Luc and Mendel, J. Trevor and Courteau, St{\'{e}}phane and Dekel, Avishai and More, Surhud and Prada, Francisco}, -doi = {10.1111/j.1365-2966.2011.19038.x}, -eprint = {1012.5859}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: elliptical and lenticular, cD,Galaxies: fundamental parameters,Galaxies: haloes,Galaxies: spiral,Galaxies: structure}, -month = {sep}, -number = {1}, -pages = {322--345}, -title = {{Dark halo response and the stellar initial mass function in early-type and late-type galaxies}}, -volume = {416}, -year = {2011} -} -@article{Hopkins2012, -abstract = {Feedback from massive stars is believed to play a critical role in driving galactic super-winds that enrich the intergalactic medium and shape the galaxy mass function, mass-metallicity relation and other global galaxy properties. In previous papers, we have introduced new numerical methods for implementing stellar feedback on sub-giant molecular cloud (sub-GMC) through galactic scales in numerical simulations of galaxies; the key physical processes include radiation pressure in the ultraviolet through infrared, supernovae (Type I and Type II), stellar winds ('fast' O star through 'slow' asymptotic giant branch winds), and Hii photoionization. Here, we show that these feedback mechanisms drive galactic winds with outflow rates as high as ∼10-20 times the galaxy star formation rate. The mass-loading efficiency (wind mass-loss rate divided by the star formation rate) scales roughly as M wind/M* ∞ V c-1 (where V c is the galaxy circular velocity), consistent with simple momentum-conservation expectations. We use our suite of simulations to study the relative contribution of each feedback mechanism to the generation of galactic winds in a range of galaxy models, from Small Magellanic Cloud like dwarfs and Milky Way (MW) analogues to z∼ 2 clumpy discs. In massive, gas-rich systems (local starbursts and high-z galaxies), radiation pressure dominates the wind generation. By contrast, for MW-like spirals and dwarf galaxies the gas densities are much lower and sources of shock-heated gas such as supernovae and stellar winds dominate the production of large-scale outflows. In all of our models, however, the winds have a complex multiphase structure that depends on the interaction between multiple feedback mechanisms operating on different spatial scales and time-scales: any single feedback mechanism fails to reproduce the winds observed. We use our simulations to provide fitting functions to the wind mass loading and velocities as a function of galaxy properties, for use in cosmological simulations and semi-analytic models. These differ from typically adopted formulae with an explicit dependence on the gas surface density that can be very important in both low-density dwarf galaxies and high-density gas-rich galaxies. {\textcopyright}2012 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.4638}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2012.20593.x}, -eprint = {1110.4638}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Stars: formation}, -number = {4}, -pages = {3522--3537}, -title = {{Stellar feedback in galaxies and the origin of galaxy-scale winds}}, -volume = {421}, -year = {2012} -} -@article{Hermans2019, -abstract = {Posterior inference with an intractable likelihood is becoming an increasingly common task in scientific domains which rely on sophisticated computer simulations. Typically, these forward models do not admit tractable densities forcing practitioners to make use of approximations. This work introduces a novel approach to address the intractability of the likelihood and the marginal model. We achieve this by learning a flexible amortized estimator which approximates the likelihood-to-evidence ratio. We demonstrate that the learned ratio estimator can be embedded in MCMC samplers to approximate likelihood-ratios between consecutive states in the Markov chain, allowing us to draw samples from the intractable posterior. Techniques are presented to improve the numerical stability and to measure the quality of an approximation. The accuracy of our approach is demonstrated on a variety of benchmarks against well-established techniques. Scientific applications in physics show its applicability.}, -archivePrefix = {arXiv}, -arxivId = {1903.04057}, -author = {Hermans, Joeri and Begy, Volodimir and Louppe, Gilles}, -eprint = {1903.04057}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hermans, Begy, Louppe - 2019 - Likelihood-free MCMC with Amortized Approximate Ratio Estimators.pdf:pdf}, -number = {i}, -title = {{Likelihood-free MCMC with Amortized Approximate Ratio Estimators}}, -url = {http://arxiv.org/abs/1903.04057}, -year = {2019} -} -@article{Fergus2014, -abstract = {High dynamic-range imagers aim to block out or null light from a very bright primary star to make it possible to detect and measure far fainter companions; in real systems a small fraction of the primary light is scattered, diffracted, and unocculted. We introduce S4, a flexible data-driven model for the unocculted (and highly speckled) light in the P1640 spectroscopic coronograph. The model uses Principal Components Analysis (PCA) to capture the spatial structure and wavelength dependence of the speckles but not the signal produced by any companion. Consequently, the residual typically includes the companion signal. The companion can thus be found by filtering this error signal with a fixed companion model. The approach is sensitive to companions that are of order a percent of the brightness of the speckles, or up to {\$}10{\^{}}{\{}-7{\}}{\$} times the brightness of the primary star. This outperforms existing methods by a factor of 2-3 and is close to the shot-noise physical limit.}, -archivePrefix = {arXiv}, -arxivId = {1408.4248}, -author = {Fergus, Rob and Hogg, David W and Oppenheimer, Rebecca and Brenner, Douglas and Pueyo, Laurent}, -doi = {10.1088/0004-637X/794/2/161}, -eprint = {1408.4248}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {infrared: planetary systems,planetary systems,techniques: image processing}, -number = {2}, -title = {{S4: A spatial-spectral model for speckle suppression}}, -volume = {794}, -year = {2014} -} -@article{Bolton2012, -abstract = {We present an analysis of the evolution of the central mass-density profile of massive elliptical galaxies from the SLACS and BELLS strong gravitational lens samples over the redshift interval z ≈ 0.1-0.6, based on the combination of strong-lensing aperture mass and stellar velocity-dispersion constraints. We find a significant trend toward steeper mass profiles (parameterized by the power-law density model with $\rho$ ∝ r-$\gamma$) at later cosmic times, with magnitude d 〈$\gamma$〉/dz = -0.60 ± 0.15. We show that the combined lens-galaxy sample is consistent with a non-evolving distribution of stellar velocity dispersions. Considering possible additional dependence of 〈$\gamma$〉 on lens-galaxy stellar mass, effective radius, and S{\'{e}}rsic index, we find marginal evidence for shallower mass profiles at higher masses and larger sizes, but with a significance that is subdominant to the redshift dependence. Using the results of published Monte Carlo simulations of spectroscopic lens surveys, we verify that our mass-profile evolution result cannot be explained by lensing selection biases as a function of redshift. Interpreted as a true evolutionary signal, our result suggests that major dry mergers involving off-axis trajectories play a significant role in the evolution of the average mass-density structure of massive early-type galaxies over the past 6Gyr. We also consider an alternative non-evolutionary hypothesis based on variations in the strong-lensing measurement aperture with redshift, which would imply the detection of an "inflection zone" marking the transition between the baryon-dominated and dark-matter halo-dominated regions of the lens galaxies. Further observations of the combined SLACS+BELLS sample can constrain this picture more precisely, and enable a more detailed investigation of the multivariate dependences of galaxy mass structure across cosmic time. {\textcopyright} 2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1201.2988}, -author = {Bolton, Adam S. and Brownstein, Joel R. and Kochanek, Christopher S. and Shu, Yiping and Schlegel, David J. and Eisenstein, Daniel J. and Wake, David A. and Connolly, Natalia and Maraston, Claudia and Arneson, Ryan A. and Weaver, Benjamin A.}, -doi = {10.1088/0004-637X/757/1/82}, -eprint = {1201.2988}, -issn = {15384357}, -journal = {ApJ}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: structure,Gravitational lensing: strong,cD}, -number = {1}, -pages = {82}, -title = {{The BOSS emission-line lens survey. II. Investigating mass-density profile evolution in the SLACS+BELLS strong gravitational lens sample}}, -url = {http://arxiv.org/abs/1201.2988}, -volume = {757}, -year = {2012} -} -@article{Skottfelt, -author = {Skottfelt, Jesper and Hall, David J and Dryer, Ben and Lee-payne, Zoe and Holland, Andrew D and Ccd, Euclid}, -file = {:C\:/Users/Jammy/Documents/Papers/Euclid_TP_serial.pdf:pdf}, -title = {{Trap pumping schemes for the Euclid CCD273 detector II : Serial register}} -} -@article{Bezanson2009, -abstract = {Recent studies have shown that massive quiescent galaxies at high redshift are much more compact than present-day galaxies of the same mass. Here we compare the radial stellar density profiles and the number density of a sample of massive galaxies at z 2.3 to nearby massive elliptical galaxies. We confirm that the average stellar densities of the z 2.3 galaxies within the effective radius, $\rho$(+0.47 -0.49 kpc, where the 68 per cent confidence limit includes both statistical error and systematic biases in mass modelling. Such offsets are not seen in field galaxies, but are predicted during the long infall to a cluster, if dark matter self-interactions generate an extra drag force.With such a small physical separation, it is difficult to definitively rule out astrophysical effects operating exclusively in dense cluster core environments - but if interpreted solely as evidence for self-interacting dark matter, this offset implies a crosssection $\sigma$DM/m $\sim$ (1.7 ± 0.7) × 10-4 cm2 g-1 × (tinfall/109 yr)-2, where tinfall is the infall duration.}, -archivePrefix = {arXiv}, -arxivId = {1504.03388}, -author = {Massey, Richard and Williams, Liliya and Smit, Renske and Swinbank, Mark and Kitching, Thomas D. and Harvey, David and Jauzac, Mathilde and Israel, Holger and Clowe, Douglas and Edge, Alastair and Hilton, Matt and Jullo, Eric and Leonard, Adrienne and Liesenborgs, Jori and Merten, Julian and Mohammed, Irshad and Nagai, Daisuke and Richard, Johan and Robertson, Andrew and Saha, Prasenjit and Santana, Rebecca and Stott, John and Tittley, Eric}, -doi = {10.1093/mnras/stv467}, -eprint = {1504.03388}, -isbn = {1283712865}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astroparticle physics,Dark matter,Galaxies: clusters: individual: Abell 3827,Gravitational lensing: strong}, -number = {4}, -pages = {3393--3406}, -title = {{The behaviour of dark matter associated with four bright cluster galaxies in the 10 kpc core of Abell 3827}}, -url = {http://arxiv.org/abs/1504.03388}, -volume = {449}, -year = {2015} -} -@article{Kruk2017, -abstract = {We use multiwavelength Sloan Digital Sky Survey (SDSS) images and Galaxy Zoo morphologies to identify a sample of {\$\sim${}}270 late-type galaxies with an off-centre bar. We measure offsets in the range 0.2-2.5 kpc between the photometric centres of the stellar disc and stellar bar. The measured offsets correlate with global asymmetries of the galaxies, with those with largest offsets showing higher lopsidedness. These findings are in good agreement with predictions from simulations of dwarf-dwarf tidal interactions producing off-centre bars. We find that the majority of galaxies with off-centre bars are of Magellanic type, with a median mass of 109.6M⊙, and 91 per cent of them having M⊙ {\textless} 3 × 1010M⊙, the characteristic mass at which galaxies start having higher central concentrations attributed to the presence of bulges. We conduct a search for companions to test the hypothesis of tidal interactions, but find that a similar fraction of galaxies with offset bars have companions within 100 kpc as galaxies with centred bars. Although this may be due to the incompleteness of the SDSS spectroscopic survey at the faint end, alternative scenarios that give rise to offset bars such as interactions with dark companions or the effect of lopsided halo potentials should be considered. Future observations are needed to confirm possible low-mass companion candidates and to determine the shape of the dark matter halo, in order to find the explanation for the off-centre bars in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1705.00007}, -author = {Kruk, Sandor J and Lintott, Chris J and Simmons, Brooke D and Bamford, Steven P and Cardamone, Carolin N and Fortson, Lucy and Hart, Ross E and H{\"{a}}u{\ss}ler, Boris and Masters, Karen L and Nichol, Robert C and Schawinski, Kevin and Smethurst, Rebecca J}, -doi = {10.1093/mnras/stx1026}, -eprint = {1705.00007}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: dwarf,Galaxies: evolution,Galaxies: interactions,Galaxies: irregular,Galaxies: structure}, -number = {3}, -pages = {3363--3373}, -title = {{Galaxy Zoo: Finding offset discs and bars in SDSS galaxies}}, -url = {http://arxiv.org/abs/1705.00007%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1026}, -volume = {469}, -year = {2017} -} -@article{Hopkins2010c, -abstract = {We present a simple estimate of the mass 'deficits' in cored spheroids, as a function of galaxy mass and radius within the galaxy. Previous attempts to measure such deficits depended on fitting some functional form to the profile at large radii extrapolating inwards; this is sensitive to the assumed functional form and does not allow for variation in nuclear profile shapes. For example, we show that literally interpreting the residuals from a single/cored Sersic function fit as implied 'deficit' can be misleading. Instead, we take advantage of larger data sets to directly construct stellar mass profiles of observed systems and measure the stellar mass enclosed in a series of physical radii (M*({\textless} R)), for samples of cusp and core spheroids at the same stellar mass. We show that there is a significant (model-independent) bimodality in this distribution of central structure for this sample at small radii. We non-parametrically measure the median offset between core and cusp populations (the 'deficit'$\Delta$M*({\textless} R)). We can then construct the scoured mass profile as a function of radius, without reference to any assumed functional form. The mass deficit rises in power-law fashion ($\Delta$M*({\textless} R) ∝R1.3-1.8) from a significant but small mass at R≲ 10 pc, to asymptote to a maximum ∼ 0.5-2 MBH at ∼ 100 pc, where MBH is the mass of the central, supermassive black hole (BH) hosted by the spheroid. At larger radii there is no statistically significant separation between populations; the upper limit to the cumulative scoured mass at ∼kpc is ∼ 2-4 MBH. This does not depend strongly on stellar mass. The dispersion in M*({\textless} R) appears larger in the core population, possibly reflecting the fact that core scouring increases the scatter in central profile shapes. We measure this broadening effect as a function of radius. The relatively low mass deficits inferred, and characteristic radii, are in good agreement with models of 'scouring' from BH binary systems. {\textcopyright}2010 The Authors. Journal compilation {\textcopyright}2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1006.0488}, -author = {Hopkins, Philip F and Hernquist, Lars}, -doi = {10.1111/j.1365-2966.2010.16915.x}, -eprint = {1006.0488}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {447--457}, -title = {{A non-parametric estimate of mass 'scoured' in galaxy cores}}, -url = {http://arxiv.org/abs/1006.0488%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1365-2966.2010.16915.x}, -volume = {407}, -year = {2010} -} -@article{Brewer2008, -abstract = {We present a source and lens reconstruction for the optical Einstein ring gravitational lens system RXS J1131-1231. We resolve detail in the source, which is the host galaxy of a z = 0.658 quasar, down to a resolution of 0.045 arcsec (this is the size of the smallest conclusively resolved structures, rather than the pixel scale), using a Bayesian technique with a realistic model for the prior information. The source reconstruction reveals a substantial amount of complex structure in the host galaxy, which is ∼8 kpc in extent and contains several bright compact substructures, with the quasar source residing in one of these bright substructures. Additionally, we recover the mass distribution of the lensing galaxy, assuming a simply parametrized model, using information from both the quasar images and the extended images. This allows a direct comparison of the amount of information about the lens that is provided by the quasar images in comparison to the extended images. In this system, we find that the extended images provide significantly more information about the lens than the quasar images alone, especially if we do not include prior constraints on the central position of the lens. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0807.2145}, -author = {Brewer, B. J. and Lewis, G. F.}, -doi = {10.1111/j.1365-2966.2008.13715.x}, -eprint = {0807.2145}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing,Methods: statistical}, -number = {1}, -pages = {39--48}, -title = {{Unlensing HST observations of the Einstein ring 1RXS J1131-1231: A Bayesian analysis}}, -volume = {390}, -year = {2008} -} -@article{Morishita2018, -abstract = {Observations have revealed massive (logM*/Msun{\textgreater}11) galaxies that were already dead when the universe was only {\$\sim${}}2 Gyr. Given the short time before these galaxies were quenched, their past histories and quenching mechanism(s) are of particular interest. In this paper, we study star formation histories (SFHs) of 24 massive galaxies at 1.6{\textless}z{\textless}2.5. A deep slitless spectroscopy + imaging data set collected from multiple Hubble Space Telescope surveys allows robust determination of their spectral energy distributions and SFHs with no functional assumption on their forms. We find that most of our massive galaxies had formed {\textgreater} 50{\%} of their extant masses by {\$\sim${}}1.5 Gyr before the time of observed redshifts, with a trend where more massive galaxies form earlier. Their stellar-phase metallicities are already compatible with those of local early-type galaxies, with a median value of logZ*/Zsun=0.25 and scatter of {\$\sim${}}0.15dex. In combination with the reconstructed SFHs, we reveal their rapid metallicity evolution from z{\$\sim${}}5.5 to {\$\sim${}}2.2 at a rate of {\$\sim${}}0.2dex/Gyr in log Z*/Zsun. Interestingly, the inferred stellar-phase metallicities are, when compared at half-mass time, {\$\sim${}}0.25dex higher than observed gas-phase metallicities of star forming galaxies. While systematic uncertainties remain, this may imply that these quenched galaxies have continued low-level star formation, rather than abruptly terminating their star formation activity, and kept enhancing their metallicity until recently.}, -archivePrefix = {arXiv}, -arxivId = {1812.06980}, -author = {Morishita, T and Abramson, L E and Treu, T and Brammer, G B and Jones, T and Kelly, P and Stiavelli, M and Trenti, M and Vulcani, B and Wang, X}, -doi = {10.3847/1538-4357/ab1d53}, -eprint = {1812.06980}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cd,elliptical and lentic-,evolution,formation,fundamental parameters,galaxies,stellar content,ular}, -number = {2}, -pages = {141}, -title = {{ Massive Dead Galaxies at z ∼ 2 with HST Grism Spectroscopy. I. Star Formation Histories and Metallicity Enrichment }}, -url = {http://arxiv.org/abs/1812.06980}, -volume = {877}, -year = {2019} -} -@article{Steinmetz2002, -abstract = {We report first results from a series of N-body/gasdynamical simulations designed to study the origin of galaxy morphologies in a cold dark matter-dominated universe. The simulations include star formation and feedback and have numerical resolution sufficiently high to allow for a direct investigation of the morphology of simulated galaxies.We find, in agreement with previous theoretical work, that the presence of the main morphological components of galaxies-disks, spheroids, bars-is regulated by the mode of gas accretion and intimately linked to discrete accretion events. In the case we present, disks arise from the smooth deposition of cooled gas at the center of dark halos, spheroids result from the stirring of preexisting disks during mergers, and bars are triggered by tides generated by satellites. This demonstrates that morphology is a transient phenomenon within the lifetime of a galaxy and that the Hubble sequence reflects the varied accretion histories of galaxies in hierarchical formation scenarios. In particular, we demonstrate directly that disk /bulge systems can be built and rebuilt by the smooth accretion of gas onto the remnant of a major merger and that the present-day remnants of late dissipative mergers between disks are spheroidal stellar systems with structure resembling that of field ellipticals. The perplexing variety of galaxy morphologies is thus highly suggestive of-and may actually even demand-a universe where structures have evolved hierarchically. {\textcopyright}2002 Elsevier Science B.V. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202466}, -author = {Steinmetz, Matthias and Navarro, Julio F}, -doi = {10.1016/S1384-1076(02)00102-1}, -eprint = {0202466}, -isbn = {0161-6420}, -issn = {13841076}, -journal = {New Astronomy}, -keywords = {Cosmology,Dark matter,Formation,Galaxies,Miscellaneous,Structure}, -number = {4}, -pages = {155--160}, -primaryClass = {astro-ph}, -title = {{The hierarchical origin of galaxy morphologies}}, -volume = {7}, -year = {2002} -} -@article{Metcalf2018, -abstract = {Large-scale imaging surveys will increase the number of galaxy-scale strong lensing candidates by maybe three orders of magnitudes beyond the number known today. Finding these rare objects will require picking them out of at least tens of millions of images, and deriving scientific results from them will require quantifying the efficiency and bias of any search method. To achieve these objectives automated methods must be developed. Because gravitational lenses are rare objects, reducing false positives will be particularly important. We present a description and results of an open gravitational lens finding challenge. Participants were asked to classify 100 000 candidate objects as to whether they were gravitational lenses or not with the goal of developing better automated methods for finding lenses in large data sets. A variety of methods were used including visual inspection, arc and ring finders, support vector machines (SVM) and convolutional neural networks (CNN). We find that many of the methods will be easily fast enough to analyse the anticipated data flow. In test data, several methods are able to identify upwards of half the lenses after applying some thresholds on the lens characteristics such as lensed image brightness, size or contrast with the lens galaxy without making a single false-positive identification. This is significantly better than direct inspection by humans was able to do. Having multi-band, ground based data is found to be better for this purpose than single-band space based data with lower noise and higher resolution, suggesting that multi-colour data is crucial. Multi-band space based data will be superior to ground based data. The most difficult challenge for a lens finder is differentiating between rare, irregular and ring-like face-on galaxies and true gravitational lenses. The degree to which the efficiency and biases of lens finders can be quantified largely depends on the realism of the simulated data on which the finders are trained.}, -archivePrefix = {arXiv}, -arxivId = {1802.03609}, -author = {Metcalf, R B and Meneghetti, M and Avestruz, C and Bellagamba, F and Bom, C R and Bertin, E and Cabanac, R and Courbin, F and Davies, A and Decenci{\`{e}}re, E and Flamary, R and Gavazzi, R and Geiger, M and Hartley, P and Huertas-Company, M and Jackson, N and Jacobs, C and Jullo, E and Kneib, J P and Koopmans, L V E and Lanusse, F and Li, C L and Ma, Q and Makler, M and Li, N and Lightman, M and Petrillo, C E and Serjeant, S and Sch{\"{a}}fer, C and Sonnenfeld, A and Tagore, A and Tortora, C and Tuccillo, D and Valent{\'{i}}n, M B and Velasco-Forero, S and {Verdoes Kleijn}, G A and Vernardos, G}, -doi = {10.1051/0004-6361/201832797}, -eprint = {1802.03609}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Gravitational lensing: strong - methods: data anal}, -title = {{The strong gravitational lens finding challenge}}, -url = {http://arxiv.org/abs/1802.03609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1051/0004-6361/201832797}, -volume = {625}, -year = {2019} -} -@article{Weijmans2014, -abstract = {We use the ATLAS3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation $\sigma$q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and $\sigma$q = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrizations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P T and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F and Davies, Roger L and Davis, Timothy A and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular,Galaxies,Structure,cD- galaxies}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{Matthee2024, -abstract = {Characterizing the prevalence and properties of faint active galactic nuclei (AGNs) in the early Universe is key for understanding the formation of supermassive black holes (SMBHs) and determining their role in cosmic reionization. We perform a spectroscopic search for broad H $\alpha$ emitters at z ≈ 4–6 using deep JWST/NIRCam imaging and wide field slitless spectroscopy from the EIGER and FRESCO surveys. We identify 20 H $\alpha$ lines at z = 4.2–5.5 that have broad components with line widths from ∼1200–3700 km s −1 , contributing ∼30%–90% of the total line flux. We interpret these broad components as being powered by accretion onto SMBHs with implied masses ∼10 7–8 M ⊙ . In the UV luminosity range M UV,AGN+host = −21 to −18, we measure number densities of ≈10 −5 cMpc −3 . This is an order of magnitude higher than expected from extrapolating quasar UV luminosity functions (LFs). Yet, such AGN are found in only <1% of star-forming galaxies at z ∼ 5. The number density discrepancy is much lower when compared to the broad H $\alpha$ LF. The SMBH mass function agrees with large cosmological simulations. In two objects, we detect complex H $\alpha$ profiles that we tentatively interpret as caused by absorption signatures from dense gas fueling SMBH growth and outflows. We may be witnessing early AGN feedback that will clear dust-free pathways through which more massive blue quasars are seen. We uncover a strong correlation between reddening and the fraction of total galaxy luminosity arising from faint AGN. This implies that early SMBH growth is highly obscured and that faint AGN are only minor contributors to cosmic reionization.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:2306.05448v3}, -author = {Matthee, Jorryt and Naidu, Rohan P and Brammer, Gabriel and Chisholm, John and Eilers, Anna-christina and Goulding, Andy and Greene, Jenny and Kashino, Daichi and Labbe, Ivo and Lilly, Simon J and Mackenzie, Ruari and Oesch, Pascal A. and Weibel, Andrea and Wuyts, Stijn and Xiao, Mengyuan and Bordoloi, Rongmon and Bouwens, Rychard and van Dokkum, Pieter and Illingworth, Garth and Kramarenko, Ivan and Maseda, Michael V. and Mason, Charlotte and Meyer, Romain A. and Nelson, Erica J. and Reddy, Naveen A. and Shivaei, Irene and Simcoe, Robert A. and Yue, Minghao}, -doi = {10.3847/1538-4357/ad2345}, -eprint = {arXiv:2306.05448v3}, -file = {:C\:/Users/Jammy/Documents/Papers/High_Redshift_galaxies/Matthee2024LittleRedDot.pdf:pdf}, -issn = {0004-637X}, -journal = {ApJ}, -keywords = {active galaxies,early universe,formation,galaxies,high-redshift,ization,quasars,reion-,supermassive black holes}, -number = {2}, -pages = {129}, -title = {{Little Red Dots: An Abundant Population of Faint Active Galactic Nuclei at z ∼ 5 Revealed by the EIGER and FRESCO JWST Surveys}}, -volume = {963}, -year = {2024} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z ∼ 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u - g color profiles for these galaxies and show that most z ∼ 2galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z ∼ 2galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: ($\Delta$(u - g rest)/$\Delta$(log r))median = -0.47, -0.33, and -0.46 for z ∼ 2, z ∼ 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z ∼ 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u - g colors, and lower S{\'{e}}rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch. {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J. and {Van Dokkum}, Pieter G. and Labb{\'{e}}, Ivo and Illingworth, Garth D. and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Szomoru et al. - 2011 - Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging The hubbl.pdf:pdf}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Handley2015, -abstract = {POLYCHORD is a novel nested sampling algorithm tailored for high-dimensional parameter spaces. This paper coincides with the release of POLYCHORD v1.6, and provides an extensive account of the algorithm. POLYCHORD utilizes slice sampling at each iteration to sample within the hard likelihood constraint of nested sampling. It can identify and evolve separate modes of a posterior semi-independently, and is parallelized using OPENMPI. It is capable of exploiting a hierarchy of parameter speeds such as those present in COSMOMC and CAMB, and is now in use in the COSMOCHORD and MODECHORD codes. POLYCHORD is available for download from http://ccpforge.cse.rl.ac.uk/gf/project/polychord/.}, -archivePrefix = {arXiv}, -arxivId = {1506.00171}, -author = {Handley, W J and Hobson, M P and Lasenby, A N}, -doi = {10.1093/mnras/stv1911}, -eprint = {1506.00171}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: data analysis,Methods: statistical}, -number = {4}, -pages = {4384--4398}, -title = {{POLYCHORD: Next-generation nested sampling}}, -volume = {453}, -year = {2015} -} -@article{Genel2017, -abstract = {We analyse scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, star formation rate and redshift are reproduced, and a quantitative comparison of projected r band sizes at 0 ≲ z ≲ 2 shows agreement to much better than 0.25 dex. We follow populations of z = 0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M*, z = 0 ≳ 109.5 M⊙, the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z = 0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M*, M*, z = 0 ≳ 109.5 M⊙ experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies withM*, z = 0 ≳ 1011 M⊙, the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z = 0.}, -archivePrefix = {arXiv}, -arxivId = {1707.05327}, -author = {Genel, Shy and Nelson, Dylan and Pillepich, Annalisa and Springel, Volker and Pakmor, R{\"{u}}diger and Weinberger, Rainer and Hernquist, Lars and Naiman, Jill and Vogelsberger, Mark and Marinacci, Federico and Torrey, Paul}, -doi = {10.1093/mnras/stx3078}, -eprint = {1707.05327}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Galaxies: structure,Methods: numerical}, -number = {3}, -pages = {3976--3996}, -title = {{The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation}}, -url = {http://arxiv.org/abs/1707.05327}, -volume = {474}, -year = {2018} -} -@article{Wang2014a, -abstract = {Charged Coupled Devices (CCDs) have been successfully used in several low energy X-ray astronomical satellites over the past two decades. Their high energy resolution and high spatial resolution make them a perfect tool for low energy astronomy, such as observing the formation of galaxy clusters and the environment around black holes. The Low Energy X-ray Telescope (LE) group is developing a Swept Charge Device (SCD) for the Hard X-ray Modulation Telescope (HXMT) satellite. A SCD is a special low energy X-ray CCD, which can be read out a thousand times faster than traditional CCDs, simultaneously keeping excellent energy resolution. A test method for measuring the charge transfer efficiency (CTE) of a prototype SCD has been set up. Studies of the charge transfer inefficiency (CTI) with a proton-irradiated SCD have been performed at a range of operating temperatures. The SCD is irradiated by 3 × 10 8 cm -2 10 MeV protons. {\textcopyright}2014 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.}, -archivePrefix = {arXiv}, -arxivId = {1308.1698}, -author = {Wang, Yu Sa and Yang, Yan Ji and Chen, Yong and Liu, Xiao Yan and Cui, Wei Wei and Xu, Yu Peng and Li, Cheng Kui and Li, Mao Shun and Han, Da Wei and Chen, Tian Xiang and Huo, Jia and Wang, Juan and Li, Wei and Hu, Wei and Zhang, Yi and Lu, Bo and Yin, Guo He and Zhu, Yue and Zhang, Zi Liang}, -doi = {10.1088/1674-1137/38/6/066001}, -eprint = {1308.1698}, -issn = {16741137}, -journal = {Chinese Physics C}, -keywords = {CCD,CTE,CTI,HXMT,LE,SCD,proton-irradiated}, -number = {6}, -pages = {66001}, -title = {{Measurements of charge transfer efficiency in a proton-irradiated swept charge device}}, -url = {http://stacks.iop.org/1674-1137/38/i=6/a=066001?key=crossref.02a5cb134fd3859a1cfa309d04df9b61}, -volume = {38}, -year = {2014} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified $\sim$17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M <10^9 M*), low-metallicity (Z$\sim$1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He \ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A. and Erb, Dawn K. and Auger, Matthew W. and Pettini, Max and Brammer, Gabriel B.}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Berg et al. - 2018 - A Window on the Earliest Star Formation Extreme Photoionization Conditions of a High-ionization, Low-metallicity(2).pdf:pdf}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {164}, -title = {{ A Window on the Earliest Star Formation: Extreme Photoionization Conditions of a High-ionization, Low-metallicity Lensed Galaxy at z ∼ 2* }}, -url = {http://arxiv.org/abs/1803.02340}, -volume = {859}, -year = {2018} -} -@article{Deason2011, -abstract = {We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the gimic suite of simulations. gimic consists of resimulations of five cosmologically representative regions from the Millennium Simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r∼ 0.1r200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r∼r200). Misalignments of >45° are seen in ∼30 per cent of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20 per cent of the satellite systems with 10 bright galaxies within r200 exhibit a polar spatial alignment with respect to the galaxy - an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction (∼10 per cent) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z= 0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation - the memory of their accretion history can remain intact to z= 0. Understanding the phase-space distribution of the z= 0 satellite population is key for studies that estimate the host halo mass from the line-of-sight velocities and projected positions of satellite galaxies. We quantify the effects of such systematics in estimates of the host halo mass from the satellite population. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A. J. and Mccarthy, I. G. and Font, A. S. and Evans, N. W. and Frenk, C. S. and Belokurov, V. and Libeskind, N. I. and Crain, R. A. and Theuns, T.}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Deason et al. - 2011 - Mismatch and misalignment Dark haloes and satellites of disc galaxies(2).pdf:pdf}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Bower:2016aa, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of {\$\sim${}}1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G and Schaye, Joop and Frenk, Carlos S and Theuns, Tom and Schaller, Matthieu and Crain, Robert A and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an end.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -month = {jul}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Rimoldini2018, -abstract = {Context. More than half a million of the 1.69 billion sources in Gaia Data Release 2 (DR2) are published with photometric time series that exhibit light variations during the 22 months of observation. Aims. An all-sky classification of common high-amplitude pulsators (Cepheids, long-period variables, $\delta$ Scuti/SX Phoenicis, and RR Lyrae stars) is provided for stars with brightness variations greater than 0.1 mag in G band. Methods. A semi-supervised classification approach was employed, firstly training multi-stage random forest classifiers with sources of known types in the literature, followed by a preliminary classification of the Gaia data and a second training phase that included a selection of the first classification results to improve the representation of some classes, before the improved classifiers were applied to the Gaia data. Dedicated validation classifiers were used to reduce the level of contamination in the published results. A relevant fraction of objects were not yet sufficiently sampled for reliable Fourier series decomposition, consequently classifiers were based on features derived from statistics of photometric time series in the G, GBP, and GRP bands, as well as from some astrometric parameters. Results. The published classification results include 195 780 RR Lyrae stars, 150 757 long-period variables, 8550 Cepheids, and 8882 $\delta$ Scuti/SX Phoenicis stars. All of these results represent candidates whose completeness and contamination are described as a function of variability type and classification reliability. Results are expressed in terms of class labels and classification scores, which are available in the varificlassifier-result table of the Gaia archive.}, -archivePrefix = {arXiv}, -arxivId = {1811.03919}, -author = {Rimoldini, L. and Holl, B. and Audard, M. and Mowlavi, N. and Nienartowicz, K. and Evans, D. W. and Guy, L. P. and Lecoeur-Ta{\"{i}}bi, I. and {De Fombelle}, G. J. and Marchal, O. and Roelens, M. and {De Ridder}, J. and Sarro, L. M. and Regibo, S. and Lopez, M. and Clementini, G. and Ripepi, V. and Molinaro, R. and Garofalo, A. and Moln{\'{a}}r, L. and Plachy, E. and Juh{\'{a}}sz and Szabados, L. and Lebzelter, T. and Teyssier, D. and Eyer, L.}, -doi = {10.1051/0004-6361/201834616}, -eprint = {1811.03919}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rimoldini et al. - 2019 - All-sky classification of high-amplitude pulsating stars.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Catalogs,Methods: Data analysis,Stars: Variables: Cepheids,Stars: Variables: Delta Scuti,Stars: Variables: General,Stars: Variables: RR Lyrae}, -number = {34616}, -title = {{All-sky classification of high-amplitude pulsating stars}}, -url = {http://arxiv.org/abs/1811.03919}, -volume = {625}, -year = {2019} -} -@article{Reynolds2015, -abstract = {Compact radio sources sometimes exhibit intervals of large, rapid changes in their flux-density, due to lensing by interstellar plasma crossing the line-of-sight. A novel survey program has made it possible to discover these "Extreme Scattering Events" (ESEs) in real time, resulting in a high-quality dynamic spectrum of an ESE observed in PKS 1939-315. Here we present a method for determining the column-density profile of a plasma lens, given only the dynamic radio spectrum of the lensed source, under the assumption that the lens is either axisymmetric or totally anisotropic. Our technique relies on the known, strong frequency dependence of the plasma refractive index in order to determine how points in the dynamic spectrum map to positions on the lens. We apply our method to high-frequency (4.2-10.8 GHz) data from the Australia Telescope Compact Array of the PKS 1939-315 ESE. The derived electron column-density profiles are very similar for the two geometries we consider, and both yield a good visual match to the data. However, the fit residuals are substantially above the noise level, and deficiencies are evident when we compare the predictions of our model to lower-frequency (1.6-3.1 GHz) data on the same ESE, thus motivating future development of more sophisticated inversion techniques.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1512.03411}, -author = {Tuntsov, Artem V and Walker, Mark A and Koopmans, Leon V E and Bannister, Keith W and Stevens, Jamie and Johnston, Simon and Reynolds, Cormac and Bignall, Hayley E}, -doi = {10.3847/0004-637X/817/2/176}, -eprint = {1512.03411}, -issn = {15384357}, -number = {December}, -title = {{Dynamic spectral mapping of interstellar plasma lenses}}, -url = {http://arxiv.org/abs/1512.03411%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/2/176}, -year = {2015} -} -@article{Einstein1916, -abstract = {Not Available}, -author = {Lorentz, H A and Einstein, A and Minkowski, H and Einstein, A}, -doi = {10.1007/978-3-663-19510-8_7}, -isbn = {1521-3889}, -issn = {15213889}, -journal = {Das Relativit{\"{a}}tsprinzip}, -number = {7}, -pages = {81--124}, -pmid = {168842}, -title = {{Die Grundlage der allgemeinen Relativit{\"{a}}tstheorie}}, -volume = {354}, -year = {2013} -} -@article{Springel2008, -abstract = {We have performed the largest ever particle simulation of a Milky Way sized dark matter halo, and present the most comprehensive convergence study for an individual dark matter halo carried out thus far. We have also simulated a sample of six ultrahighly resolved Milky Way sized haloes, allowing us to estimate the halo-to-halo scatter in substructure statistics. In our largest simulation, we resolve nearly 300 000 gravitationally bound subhaloes within the virialized region of the halo. Simulations of the same object differing in mass resolution by factors of up to 1800 accurately reproduce the largest subhaloes with the same mass, maximum circular velocity and position, and yield good convergence for the abundance and internal properties of dark matter substructures. We detect up to four generations of subhaloes within subhaloes, but contrary to recent claims, we find less substructure in subhaloes than in the main halo when regions of equal mean overdensity are compared. The overall substructure mass fraction is much lower in subhaloes than in the main halo. Extrapolating the main halo's subhalo mass spectrum down to an Earth mass, we predict the mass fraction in substructure to be well below 3 per cent within 100 kpc, and to be below 0.1 per cent within the solar circle. The inner density profiles of subhaloes show no sign of converging to a fixed asymptotic slope and are well fitted by gently curving profiles of Einasto form. The mean concentrations of isolated haloes are accurately described by the fitting formula of Neto et al. down to maximum circular velocities of 1.5 km s -1, an extrapolation over some five orders of magnitude in mass. However, at equal maximum circular velocity, subhaloes are more concentrated than field haloes, with a characteristic density that is typically ∼2.6 times larger and increases with decreasing distance from halo centre. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0809.0898}, -author = {Springel, V. and Wang, J. and Vogelsberger, M. and Ludlow, A. and Jenkins, A. and Helmi, A. and Navarro, J. F. and Frenk, C. S. and White, S. D.M.}, -doi = {10.1111/j.1365-2966.2008.14066.x}, -eprint = {0809.0898}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Dark matter,Methods: numerical}, -month = {dec}, -number = {4}, -pages = {1685--1711}, -title = {{The Aquarius Project: The subhaloes of galactic haloes}}, -volume = {391}, -year = {2008} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kiloparsecs. We use data from the Hyper Suprime-Cam (HSC) survey that is simultaneously wide ({\$\sim${}}100 deg2) and deep ({\textgreater}28.5 mag arcsec-2 in i band) to study the stellar haloes of a sample of {\$\sim${}}7000 massive galaxies at z {\$\sim${}} 0.4. The depth of the HSC data enables us to measure surface mass density profiles to 100 kpc for individual galaxies without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles than smaller galaxies. When this extended light is not properly accounted for (because of shallow imaging and/or inadequate profile modelling), the derived stellar mass function can be significantly underestimated at the high-mass end. Across our sample, the ellipticity of outer light profile increases substantially with radius. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass dependence in outer colour gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at a later time from a series of merging events. We provide surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless} z {\textless} 0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Lapi2011, -abstract = {Exploiting the Herschel Astrophysical Terahertz Large Area Survey Science Demonstration Phase survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 $\mu$m and at several redshifts z ≳ 1, for bright submillimeter galaxies with star formation rates (SFRs) ≳ 100 M ⊙ yr-1. We find that the evolution of the comoving LF is strong up to ≈ z 2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of dust-enshrouded star formation in massive halos (M H ≳ 3 × 1012 M ⊙) amounts to ∼7 × 10 8yr. Given the SFRs, which are in the range of 102-10 3 M ⊙ yr-1, this timescale implies final stellar masses of the order of 1011-1012 M ⊙. The corresponding stellar mass function matches the observed mass function of passively evolving galaxies at z ≳ 1. The comparison of the statistics for submillimeter and UV-selected galaxies suggests that the dust-free, UV bright phase is ≳ 102 times shorter than the submillimeter bright phase, implying that the dust must form soon after the onset of star formation. Using a single reference spectral energy distribution (SED; the one of the z ≈ 2.3 galaxy SMM J2135-0102), our simple physical model is able to reproduce not only the LFs at different redshifts >1 but also the counts at wavelengths ranging from 250 $\mu$m to 1mm. Owing to the steepness of the counts and their relatively broad frequency range, this result suggests that the dispersion of submillimeter SEDs of z > 1 galaxies around the reference one is rather small. {\textcopyright} 2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1108.3911}, -author = {Lapi, A. and Gonz{\'{a}}lez-Nuevo, J. and Fan, L. and Bressan, A. and {De Zotti}, G. and Danese, L. and Negrello, M. and Dunne, L. and Eales, S. and Maddox, S. and Auld, R. and Baes, M. and Bonfield, D. G. and Buttiglione, S. and Cava, A. and Clements, D. L. and Cooray, A. and Dariush, A. and Dye, S. and Fritz, J. and Herranz, D. and Hopwood, R. and Ibar, E. and Ivison, R. and Jarvis, M. J. and Kaviraj, S. and L{\'{o}}pez-Caniego, M. and Massardi, M. and Micha{\l}owski, M. J. and Pascale, E. and Pohlen, M. and Rigby, E. and Rodighiero, G. and Serjeant, S. and Smith, D. J.B. and Temi, P. and Wardlow, J. and {Van Der Werf}, P.}, -doi = {10.1088/0004-637X/742/1/24}, -eprint = {1108.3911}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: evolution,galaxies: formation,galaxies: high-redshift,submillimeter: galaxies}, -number = {1}, -pages = {24}, -title = {{Herschel-atlas galaxy counts and high-redshift luminosity functions: The formation of massive early-type galaxies}}, -url = {http://arxiv.org/abs/1108.3911}, -volume = {742}, -year = {2011} -} -@article{Bluck2015, -abstract = {We derive the dependence of the fraction of passive central galaxies on the mass of their supermassive black holes for a sample of over 400,000 SDSS galaxies at z < 0.2. Our large sample contains galaxies in a wide range of environments, with stellar masses 8 < log(M*/Msun) < 12, spanning the entire morphological spectrum from pure disks to spheroids. We derive estimates for the black hole masses from measured central velocity dispersions and bulge masses, using a variety of published empirical relationships. We find a very strong dependence of the passive fraction on black hole mass, which is largely unaffected by the details of the black hole mass estimate. Moreover, the passive fraction relationship with black hole mass remains strong and tight even at fixed values of galaxy stellar mass (M*), dark matter halo mass (Mhalo), and bulge-to-total stellar mass ratio (B/T). Whereas, the passive fraction dependence on M*, Mhalo and B/T is weak at fixed MBH. These observations show that, for central galaxies, MBH is the strongest correlator with the passive fraction, consistent with quenching from AGN feedback.}, -archivePrefix = {arXiv}, -arxivId = {1412.3862}, -author = {Bluck, Asa F. L. and Ellison, Sara L. and Patton, David R. and Simard, Luc and Mendel, J. Trevor and Teimoorinia, Hossein and Moreno, Jorge and Starkenburg, Else}, -eprint = {1412.3862}, -journal = {arXiv e-prints}, -keywords = {agn,black holes,evolution,formation,galaxies,morphology,star formation}, -month = {dec}, -number = {December 2014}, -pages = {6}, -title = {{Why do galaxies stop forming stars? I. The passive fraction - black hole mass relation for central galaxies}}, -url = {http://arxiv.org/abs/1412.3862}, -volume = {000}, -year = {2014} -} -@article{Gonzalez2009, -abstract = {The huge size and uniformity of the Sloan Digital Sky Survey (SDSS) make possible an exacting test of current models of galaxy formation. We compare the predictions of the galform semi-analytical galaxy formation model for the luminosities, morphologies, colours and scalelengths of local galaxies. galform models the luminosity and size of the disc and bulge components of a galaxy, and so we can compute quantities which can be compared directly with SDSS observations, such as the Petrosian magnitude and the S{\'{e}}rsic index. We test the predictions of two published models set in the cold dark matter cosmology: the Baugh et al. model, which assumes a top-heavy initial mass function (IMF) in starbursts and superwind feedback, and the Bower et al. model, which uses active galactic nucleus feedback and a standard IMF. The Bower et al. model better reproduces the overall shape of the luminosity function, the morphology-luminosity relation and the colour bimodality observed in the SDSS data, but gives a poor match to the size-luminosity relation. The Baugh et al. model successfully predicts the size-luminosity relation for late-type galaxies. Both models fail to reproduce the sizes of bright early-type galaxies. These problems highlight the need to understand better both the role of feedback processes in determining galaxy sizes, in particular the treatment of the angular momentum of gas reheated by supernovae, and the sizes of the stellar spheroids formed by galaxy mergers and disc instabilities. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0812.4399}, -author = {Gonz{\'{a}}lez, Juan E. and Lacey, C. G. and Baugh, C. M. and Frenk, C. S. and Benson, A. J.}, -doi = {10.1111/j.1365-2966.2009.15057.x}, -eprint = {0812.4399}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -month = {aug}, -number = {3}, -pages = {1254--1274}, -title = {{Testing model predictions of the cold dark matter cosmology for the sizes, colours, morphologies and luminosities of galaxies with the SDSS}}, -volume = {397}, -year = {2009} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for $\sim$20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J. and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Coenda, Mart{\'{i}}nez, Muriel - 2018 - Green valley galaxies as a transition population in different environments.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Hickox2012, -abstract = {We present a measurement of the spatial clustering of submillimetre galaxies (SMGs) at z= 1-3. Using data from the 870$\mu$m Large APEX Bolometer Camera (LABOCA) submillimetre survey of the Extended Chandra Deep Field-South, we employ a novel technique to measure the cross-correlation between SMGs and galaxies, accounting for the full probability distributions for photometric redshifts of the galaxies. From the observed projected two-point cross-correlation function we derive the linear bias and characteristic dark matter halo masses for the SMGs. We detect clustering in the cross-correlation between SMGs and galaxies at the >4$\sigma$ level. Accounting for the clustering of galaxies from their autocorrelation function, we estimate an autocorrelation length for SMGs of r o = 7.7 -2.3+1.8 h -1 Mpc assuming a power-law slope $\gamma$= 1.8, and derive a corresponding dark matter halo mass of log(M halo[h -1M ⊙]) = 12.8 -0.5+0.3. Based on the evolution of dark matter haloes derived from simulations, we show that that the z= 0 descendants of SMGs are typically massive ($\sim$2-3L *) elliptical galaxies residing in moderate- to high-mass groups (log(M halo[h -1M ⊙]) = 13.3 -0.5+0.3). From the observed clustering we estimate an SMG lifetime of $\sim$100Myr, consistent with lifetimes derived from gas consumption times and star formation time-scales, although with considerable uncertainties. The clustering of SMGs at z$\sim$ 2 is consistent with measurements for optically selected quasi-stellar objects (QSOs), supporting evolutionary scenarios in which powerful starbursts and QSOs occur in the same systems. Given that SMGs reside in haloes of characteristic mass $\sim$6 × 10 12h -1M ⊙, we demonstrate that the redshift distribution of SMGs can be described remarkably well by the combination of two effects: the cosmological growth of structure and the evolution of the molecular gas fraction in galaxies. We conclude that the powerful starbursts in SMGs likely represent a short-lived but universal phase in massive galaxy evolution, associated with the transition between cold gas-rich, star-forming galaxies and passively evolving systems. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.0321}, -author = {Hickox, Ryan C. and Wardlow, J. L. and Smail, Ian and Myers, A. D. and Alexander, D. M. and Swinbank, A. M. and Danielson, A. L.R. and Stott, J. P. and Chapman, S. C. and Coppin, K. E.K. and Dunlop, J. S. and Gawiser, E. and Lutz, D. and van der Werf, P. and Wei{\ss}, A.}, -doi = {10.1111/j.1365-2966.2011.20303.x}, -eprint = {1112.0321}, -isbn = {00358711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: starburst,Large-scale structure of Universe,Submillimetre: galaxies}, -number = {1}, -pages = {284--295}, -pmid = {23747736}, -title = {{The LABOCA survey of the Extended Chandra Deep Field-South: Clustering of submillimetre galaxies}}, -volume = {421}, -year = {2012} -} -@article{Wang2018a, -abstract = {We explore the isothermal total matter radial density profiles in early-type galaxies (ETGs) selected from the IllustrisTNG simulation. For a sample of 514 ETGs in the stellar mass range of $10^{10.7}\mathrm{M}_{\odot} \leqslant M_{\ast} \leqslant 10^{11.9}\mathrm{M}_{\odot}$ at $z = 0$, the total power-law slope has a mean of $\langle\gamma^{\prime}\rangle = 2.003 \pm 0.008$ and a standard deviation of $\sigma_{\gamma^{\prime}} = 0.175$ over the radial range from 0.4 to 4 times the stellar half mass radius. Several correlations between $\gamma^{\prime}$ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduce correlation trends qualitatively, and $\gamma^{\prime}$ is almost constant with redshift below $z = 2$. The power-law density profile of the ETG dark matter halos is steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. The dark matter inner slopes of the best-fit generalized NFW profile are much steeper than the standard NFW profile and they are anti-correlated (constant) with the halo mass in the FP (DMO) run. The dark matter inner slope is also anti-correlated with the halo concentration parameter $c_{200}$ in both runs. Comparison of the mass-weighted slope/central dark matter fraction correlation, $\gamma_{\mathrm{mw}}^{\prime}-f_{\mathrm{DM}}$, with models and observations indicates contraction of the IllustrisTNG dark matter halos, especially in lower-mass systems.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -eprint = {1811.06545}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2018 - Early-type galaxy density profiles from IllustrisTNG I. Galaxy correlations and the impact of baryons(5).pdf:pdf}, -title = {{Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -year = {2018} -} -@article{Viel2013, -abstract = {We present updated constraints on the free-streaming of warm dark matter (WDM) particles derived from an analysis of the Lyman-$\alpha$ flux power spectrum measured from high-resolution spectra of 25 z>4 quasars obtained with the Keck High Resolution Echelle Spectrometer and the Magellan Inamori Kyocera Echelle spectrograph. We utilize a new suite of high-resolution hydrodynamical simulations that explore WDM masses of 1, 2 and 4 keV (assuming the WDM consists of thermal relics), along with different physically motivated thermal histories. We carefully address different sources of systematic error that may affect our final results and perform an analysis of the Lyman-$\alpha$ flux power with conservative error estimates. By using a method that samples the multidimensional astrophysical and cosmological parameter space, we obtain a lower limit mWDM{\^{a}}‰3.3 keV (2$\sigma$) for warm dark matter particles in the form of early decoupled thermal relics. Adding the Sloan Digital Sky Survey Lyman-$\alpha$ flux power spectrum does not improve this limit. Thermal relics of masses 1, 2 and 2.5 keV are disfavored by the data at about the 9$\sigma$, 4$\sigma$ and 3$\sigma$ C.L., respectively. Our analysis disfavors WDM models where there is a suppression in the linear matter power spectrum at (nonlinear) scales corresponding to k=10h/Mpc which deviates more than 10% from a Lambda cold dark matter model. Given this limit, the corresponding "free-streaming mass" below which the mass function may be suppressed is ∼2×108h-1M {\^{a}}{\v{S}}™. There is thus very little room for a contribution of the free-streaming of WDM to the solution of what has been termed the small scale crisis of cold dark matter. {\textcopyright} 2013 American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {1306.2314}, -author = {Viel, Matteo and Becker, George D. and Bolton, James S. and Haehnelt, Martin G.}, -doi = {10.1103/PhysRevD.88.043502}, -eprint = {1306.2314}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Viel et al. - 2013 - Warm dark matter as a solution to the small scale crisis New constraints from high redshift Lyman-$\alpha$ forest data.pdf:pdf}, -issn = {15507998}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -number = {4}, -pages = {1--20}, -title = {{Warm dark matter as a solution to the small scale crisis: New constraints from high redshift Lyman-$\alpha$ forest data}}, -volume = {88}, -year = {2013} -} -@article{Cole:2000aa, -abstract = {We describe the GALFORM semi-analytic model for calculating the formation and evolution of galaxies in hierarchical clustering cosmologies. It improves upon, and extends, the earlier scheme developed by Cole et al. The model employs a new Monte Carlo algorithm to follow the merging evolution of dark matter haloes with arbitrary mass resolution. It incorporates realistic descriptions of the density profiles of dark matter haloes and the aas they contain; it follows the chemical evolution of gas and stars, and the associated production of dust; and it includes a detailed calculation of the sizes of discs and spheroids. Wherever possible, our prescriptions for modelling individual physical processes are based on results of numerical simulations. They require a number of adjustable parameters, which we fix by reference to a small subset of local galaxy data. This results in a fully specified model of galaxy formation which can be tested against other data. We apply our methods to the ACDM cosmology ($\Omega$0 = 0.3, A0 = 0.7), and find good agreement with a wide range of properties of the local galaxy population: the B- and K-band luminosity functions, the distribution of colours for the population as a whole, the ratio of ellipticals to spirals, the distribution of disc sizes, and the current cold gas content of discs. In spite of the overall success of the model, some interesting discrepancies remain: the colour-magnitude relation for ellipticals in clusters is significantly flatter than observed at bright magnitudes (although the scatter is about right), and the model predicts galaxy circular velocities, at a given luminosity, that are about 30 per cent larger than is observed. It is unclear whether these discrepancies represent fundamental shortcomings of the model, or whether they result from the various approximations and uncertainties inherent in the technique. Our more detailed methods do not change our earlier conclusion that just over half the stars in the Universe are expected to have formed since z ≲ 1.5.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0007281}, -author = {Cole, Shaun and Lacey, Cedric G. and Baugh, Carlton M. and Frenk, Carlos S.}, -doi = {10.1046/j.1365-8711.2000.03879.x}, -eprint = {0007281}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cole et al. - 2000 - Hierarchical galaxy formation(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation}, -month = {nov}, -number = {1}, -pages = {168--204}, -primaryClass = {astro-ph}, -title = {{Hierarchical galaxy formation}}, -url = {http://arxiv.org/abs/astro-ph/0007281%0Ahttp://dx.doi.org/10.1046/j.1365-8711.2000.03879.x}, -volume = {319}, -year = {2000} -} -@article{Pontzen2014, -abstract = {A principal discovery in modern cosmology is that standard model particles comprise only 5 per cent of the mass-energy budget of the Universe. In the $\Lambda$CDM paradigm, the remaining 95 per cent consists of dark energy ($\Lambda$) and cold dark matter. $\Lambda$CDM is being challenged by its apparent inability to explain the low-density 'cores' of dark matter measured at the centre of galaxies, where centrally concentrated high-density 'cusps' were predicted. But before drawing conclusions, it is necessary to include the effect of gas and stars, historically seen as passive components of galaxies. We now understand that these can inject heat energy into the cold dark matter through a coupling based on rapid gravitational potential fluctuations, explaining the observed low central densities. {\textcopyright}2014 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1402.1764}, -author = {Pontzen, Andrew and Governato, Fabio}, -doi = {10.1038/nature12953}, -eprint = {1402.1764}, -isbn = {1476-4687 (Electronic){\$}\backslash{\$}r0028-0836 (Linking)}, -issn = {00280836}, -journal = {Nature}, -number = {7487}, -pages = {171--178}, -pmid = {24522596}, -title = {{Cold dark matter heats up}}, -volume = {506}, -year = {2014} -} -@article{Weijmans2014, -abstract = {We use the ATLAS3D sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation $\sigma$q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and $\sigma$q = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrizations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.}, -archivePrefix = {arXiv}, -arxivId = {1408.1099}, -author = {Weijmans, Anne Marie and {De Zeeuw}, P. T. and Emsellem, Eric and Krajnovi{\'{c}}, Davor and Lablanche, Pierre Yves and Alatalo, Katherine and Blitz, Leo and Bois, Maxime and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, Martin and Cappellari, Michele and Crocker, Alison F. and Davies, Roger L. and Davis, Timothy A. and Duc, Pierre Alain and Khochfar, Sadegh and Kuntschner, Harald and McDermid, Richard M. and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Serra, Paolo and Kleijn, Gijs Verdoes and Young, Lisa M.}, -doi = {10.1093/mnras/stu1603}, -eprint = {1408.1099}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Weijmans et al. - 2014 - The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Elliptical and lenticular, cD- galaxies,Galaxies,Structure}, -number = {4}, -pages = {3340--3356}, -title = {{The ATLAS3D project - XXIV. The intrinsic shape distribution of early-type galaxies}}, -volume = {444}, -year = {2014} -} -@article{He2023, -abstract = {Strong gravitational lensing offers a compelling test of the cold dark matter paradigm, as it allows for subhaloes with masses of ∼109 M⊙ and below to be detected. We test commonly used techniques for detecting subhaloes superposed in images of strongly lensed galaxies. For the lens we take a simulated galaxy in a ∼1013 M⊙ halo grown in a high-resolution cosmological hydrodynamical simulation, which we view from two different directions. Though the resolution is high, we note the simulated galaxy still has an artificial core which adds additional complexity to the baryon dominated region. To remove particle noise, we represent the projected galaxy mass distribution by a series of Gaussian profiles which precisely capture the features of the projected galaxy. We first model the lens mass as a (broken) power-law density profile and then search for small haloes. Of the two projections, one has a regular elliptical shape, while the other has distinct deviations from an elliptical shape. For the former, the broken power-law model gives no false positives and correctly recovers the mass of the superposed small halo; however, for the latter we find false positives and the inferred halo mass is overestimated by ∼4–5 times. We then use a more complex model in which the lens mass is decomposed into stellar and dark matter components. In this case, we show that we can capture the simulated galaxy's complex projected structures and correctly infer the input small halo.}, -archivePrefix = {arXiv}, -arxivId = {2202.10191}, -author = {He, Qiuhan and Nightingale, James and Robertson, Andrew and Amvrosiadis, Aristeidis and Cole, Shaun and Frenk, Carlos S and Massey, Richard and Li, Ran and Amorisco, Nicola C and Metcalf, R Benton and Cao, Xiaoyue and Etherington, Amy}, -doi = {10.1093/mnras/stac2779}, -eprint = {2202.10191}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/He2022Preprint.pdf:pdf}, -issn = {0035-8711}, -journal = {MNRAS}, -keywords = {dark matter,gravitational lensing,strong}, -number = {1}, -pages = {220--239}, -title = {{Testing strong lensing subhalo detection with a cosmological simulation}}, -url = {http://arxiv.org/abs/2202.10191}, -volume = {518}, -year = {2023} -} -@article{Dalal2002, -abstract = {We place limits on the linear power spectrum on small scales (k > 50 h/Mpc) using measurements of substructure in gravitational lens galaxies. We find excellent agreement with the simplest LambdaCDM models, and in conjunction with other cosmological probes, place constraints on the neutrino mass m_nu, tilt of the primordial power spectrum n, and mass of the dark matter particle m. We find n>0.94, and for a Harrison-Zeldovich spectrum, find m_nu<0.74 eV and m>5.2 keV, at 95% confidence.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0202290}, -author = {Dalal, Neal and Kochanek, Christopher S.}, -eprint = {0202290}, -journal = {ArXiv Astrophysics e-prints}, -keywords = {Astrophysics,High Energy Physics - Phenomenology}, -month = {feb}, -pages = {3}, -primaryClass = {astro-ph}, -title = {{Strong Lensing Constraints on Small-Scale Linear Power}}, -url = {http://arxiv.org/abs/astro-ph/0202290}, -year = {2002} -} -@article{Pulsoni2017, -abstract = {Wolbachia is an intracellular endosymbiont that induces a variety of reproductive alterations in diverse arthropods. The almond moth, Cadra cautella, is double infected with two Wolbachia variants, wCauA and wCauB, and expresses complete cytoplasmic incompatibility (CI). The individual contribution of wCauA and wCauB to the expression of CI are unclear, however, because the two variants have not been separated in this host. The effect of wCauA is of particular interest because it induces male killing when transferred into the Mediterranean flour moth, Ephestia kuehniella. In the present study, we generated C. cautella infected with only wCauA by treating double-infected insects with tetracycline. Single-infected C. cautella exhibited strong CI, demonstrating that wCauA induces two distinct reproductive phenotypes in different hosts: CI in C. cautella and male killing in E. kuehniella. CI was also observed in the cross of double-infected males and single-infected females. Comparison of the single- and double-infected insects by real-time quantitative polymerase chain reaction suggested that the wCauA density is not affected much by the presence or absence of wCauB. {\textcopyright}2005 Nature Publishing Group All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {http://www.R-project.org}, -author = {Sasaki, T and Massaki, N and Kubo, T}, -doi = {10.1038/sj.hdy.6800737}, -eprint = {/www.R-project.org}, -isbn = {0018-067X}, -issn = {0018067X}, -journal = {Heredity}, -keywords = {Cadra cautella,Cytoplasmic incompatibility,Double infection,Male killing,Real-time quantitative PCR,Wolbachia}, -number = {5}, -pages = {389--393}, -pmid = {16106260}, -primaryClass = {http:}, -title = {{Wolbachia variant that induces two distinct reproductive phenotypes in different hosts}}, -url = {http://www.ncbi.nlm.nih.gov/pubmed/16106260}, -volume = {95}, -year = {2005} -} -@article{Deason2011, -abstract = {We study the phase-space distribution of satellite galaxies associated with late-type galaxies in the gimic suite of simulations. gimic consists of resimulations of five cosmologically representative regions from the Millennium Simulation, which have higher resolution and incorporate baryonic physics. Whilst the disc of the galaxy is well aligned with the inner regions (r∼ 0.1r200) of the dark matter halo, both in shape and angular momentum, there can be substantial misalignments at larger radii (r∼r200). Misalignments of {\textgreater}45° are seen in ∼30 per cent of our sample. We find that the satellite population aligns with the shape (and angular momentum) of the outer dark matter halo. However, the alignment with the galaxy is weak owing to the mismatch between the disc and dark matter halo. Roughly 20 per cent of the satellite systems with 10 bright galaxies within r200 exhibit a polar spatial alignment with respect to the galaxy - an orientation reminiscent of the classical satellites of the Milky Way. We find that a small fraction (∼10 per cent) of satellite systems show evidence for rotational support which we attribute to group infall. There is a bias towards satellites on prograde orbits relative to the spin of the dark matter halo (and to a lesser extent with the angular momentum of the disc). This preference towards co-rotation is stronger in the inner regions of the halo where the most massive satellites accreted at relatively early times are located. We attribute the anisotropic spatial distribution and angular momentum bias of the satellites at z= 0 to their directional accretion along the major axes of the dark matter halo. The satellite galaxies have been accreted relatively recently compared to the dark matter mass and have experienced less phase-mixing and relaxation - the memory of their accretion history can remain intact to z= 0. Understanding the phase-space distribution of the z= 0 satellite population is key for studies that estimate the host halo mass from the line-of-sight velocities and projected positions of satellite galaxies. We quantify the effects of such systematics in estimates of the host halo mass from the satellite population. {\textcopyright}2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1101.0816}, -author = {Deason, A J and Mccarthy, I G and Font, A S and Evans, N W and Frenk, C S and Belokurov, V and Libeskind, N I and Crain, R A and Theuns, T}, -doi = {10.1111/j.1365-2966.2011.18884.x}, -eprint = {1101.0816}, -isbn = {9781100258300}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: general,Galaxies: haloes,Galaxies: kinematics and dynamics}, -number = {3}, -pages = {2607--2625}, -primaryClass = {astro-ph.CO}, -title = {{Mismatch and misalignment: Dark haloes and satellites of disc galaxies}}, -volume = {415}, -year = {2011} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -month = {aug}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -volume = {370}, -year = {2006} -} -@article{Genel2017, -abstract = {We analyse scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, star formation rate and redshift are reproduced, and a quantitative comparison of projected r band sizes at 0 ≲ z ≲ 2 shows agreement to much better than 0.25 dex. We follow populations of z = 0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M*, z = 0 ≳ 109.5 M⊙, the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z = 0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M*, M*, z = 0 ≳ 109.5 M⊙ experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies withM*, z = 0 ≳ 1011 M⊙, the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z = 0.}, -archivePrefix = {arXiv}, -arxivId = {1707.05327}, -author = {Genel, Shy and Nelson, Dylan and Pillepich, Annalisa and Springel, Volker and Pakmor, R{\"{u}}diger and Weinberger, Rainer and Hernquist, Lars and Naiman, Jill and Vogelsberger, Mark and Marinacci, Federico and Torrey, Paul}, -doi = {10.1093/mnras/stx3078}, -eprint = {1707.05327}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Galaxies: structure,Methods: numerical}, -number = {3}, -pages = {3976--3996}, -title = {{The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation}}, -url = {http://arxiv.org/abs/1707.05327}, -volume = {474}, -year = {2018} -} -@article{Aschwanden2017, -abstract = {Self-organization is a property of dissipative nonlinear processes that are governed by a global driving force and a local positive feedback mechanism, which creates regular geometric and/or temporal patterns, and decreases the entropy locally, in contrast to random processes. Here we investigate for the first time a comprehensive number of (17) self-organization processes that operate in planetary physics, solar physics, stellar physics, galactic physics, and cosmology. Self-organizing systems create spontaneous “order out of randomness”, during the evolution from an initially disordered system to an ordered quasi-stationary system, mostly by quasi-periodic limit-cycle dynamics, but also by harmonic (mechanical or gyromagnetic) resonances. The global driving force can be due to gravity, electromagnetic forces, mechanical forces (e.g., rotation or differential rotation), thermal pressure, or acceleration of nonthermal particles, while the positive feedback mechanism is often an instability, such as the magneto-rotational (Balbus-Hawley) instability, the convective (Rayleigh-B{\'{e}}nard) instability, turbulence, vortex attraction, magnetic reconnection, plasma condensation, or a loss-cone instability. Physical models of astrophysical self-organization processes require hydrodynamic, magneto-hydrodynamic (MHD), plasma, or N-body simulations. Analytical formulations of self-organizing systems generally involve coupled differential equations with limit-cycle solutions of the Lotka-Volterra or Hopf-bifurcation type.}, -archivePrefix = {arXiv}, -arxivId = {1708.03394}, -author = {Aschwanden, Markus J and Scholkmann, Felix and B{\'{e}}thune, William and Schmutz, Werner and Abramenko, Valentina and Cheung, Mark C M and M{\"{u}}ller, Daniel and Benz, Arnold and Chernov, Guennadi and Kritsuk, Alexei G and Scargle, Jeffrey D and Melatos, Andrew and Wagoner, Robert V and Trimble, Virginia and Green, William H}, -doi = {10.1007/s11214-018-0489-2}, -eprint = {1708.03394}, -issn = {15729672}, -journal = {Space Science Reviews}, -keywords = {Astrophysics,Hopf bifurcation,Instabilities,Limit cycle dynamics,Lotka,Organization,Planetary physics,Self,Solar physics,Stellar physics,Volterra systems}, -number = {2}, -pages = {1--41}, -title = {{Order out of Randomness: Self-Organization Processes in Astrophysics}}, -url = {http://arxiv.org/abs/1708.03394}, -volume = {214}, -year = {2018} -} -@article{Greene2017a, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Hodge2019, -abstract = {We present sub-kpc-scale mapping of the 870 $\mu$m ALMA continuum emission in six luminous ($L_{\rm IR}\sim\sim\sim5\sim\times10^{12}$ L$_{\odot}$) submillimeter galaxies (SMGs) from the ALESS survey of the Extended Chandra Deep Field South. Our high-fidelity 0.07$''$-resolution imaging ($\sim$500 pc) reveals robust evidence for structures with deconvolved sizes of $\lesssim$0.5-1 kpc embedded within (dominant) exponential dust disks. The large-scale morphologies of the structures within some of the galaxies show clear curvature and/or clump-like structures bracketing elongated nuclear emission, suggestive of bars, star-forming rings, and spiral arms. In this interpretation, the ratio of the `ring' and `bar' radii (1.9$\pm$0.3) agrees with that measured for such features in local galaxies. These potential spiral/ring/bar structures would be consistent with the idea of tidal disturbances, with their detailed properties implying flat inner rotation curves and Toomre-unstable disks (Q<1). The inferred one-dimensional velocity dispersions ($\sigma_{\rm r}\lesssim$ 70-160 km s$^{-1}$) are marginally consistent with the limits implied if the sizes of the largest structures are comparable to the Jeans length. We create maps of the star formation rate density ($\Sigma_{\rm SFR}$) on $\sim$500 pc scales and show that the SMGs are able to sustain a given (galaxy-averaged) $\Sigma_{\rm SFR}$ over much larger physical scales than local (ultra-)luminous infrared galaxies. However, on 500 pc scales, they do not exceed the Eddington limit set by radiation pressure on dust. If confirmed by kinematics, the potential presence of non-axisymmetric structures would provide a means for net angular momentum loss and efficient star formation, helping to explain the very high star formation rates measured in SMGs.}, -archivePrefix = {arXiv}, -arxivId = {1810.12307}, -author = {Hodge, J. A. and Smail, I. and Walter, F. and da Cunha, E. and Swinbank, A. M. and Rybak, M. and Venemans, B. and Brandt, W. N. and Rivera, G. Calistro and Chapman, S. C. and Chen, Chian-Chou and Cox, P. and Dannerbauer, H. and Decarli, R. and Greve, T. R. and Knudsen, K. K. and Menten, K. M. and Schinnerer, E. and Simpson, J. M. and van der Werf, P. and Wardlow, J. L. and Weiss, A.}, -doi = {10.3847/1538-4357/ab1846}, -eprint = {1810.12307}, -file = {:C\:/Users/Jammy/Documents/Papers/High_Redshift_galaxies/Hodge2019AlmaRevealsS[pirals.pdf:pdf}, -issn = {15384357}, -journal = {The Astrophysical Journal}, -keywords = {evolution,formation,galaxies,galaxies: evolution,galaxies: formation,galaxies:,high-redshift,starburst,submillimeter}, -number = {2}, -pages = {130}, -publisher = {IOP Publishing}, -title = {{ALMA Reveals Potential Evidence for Spiral Arms, Bars, and Rings in High-redshift Submillimeter Galaxies}}, -url = {http://dx.doi.org/10.3847/1538-4357/ab1846}, -volume = {876}, -year = {2019} -} -@article{LaBarbera2010, -abstract = {We present an analysis of stellar population gradients in 4546 early-type galaxies (ETGs) with photometry in grizYHJK along with optical spectroscopy. ETGs were selected as bulge-dominated systems, displaying passive spectra within the SDSS fibers. A new approach is described which utilizes color information to constrain age and metallicity gradients. Defining an effective color gradient, ∇*, which incorporates all of the available color indices, we investigate how ∇* varies with galaxy mass proxies, i.e., velocity dispersion, stellar (M*) and dynamical (Mdyn) masses, as well as age, metallicity, and [$\alpha$/Fe]. ETGs with Mdyn larger than 8.5 × 1010 M⊙ have increasing age gradients and decreasing metallicity gradients with respect to mass, metallicity, and enhancement. We find that velocity dispersion and [$\alpha$/Fe] are the main drivers of these correlations. ETGs with 2.5 × 10 10 Ṁ ≤ Mdyn ≤ 8.5 × 10 10 M⊙ show no correlation of age, metallicity, and color gradients with respect to mass, although color gradients still correlate with stellar population parameters, and these correlations are independent of each other. In both mass regimes, the striking anti-correlation between color gradient and $\alpha$-enhancement is significant at ∼5$\sigma$ and results from the fact that metallicity gradient decreases with [$\alpha$/Fe]. This anti-correlation may reflect the fact that star formation and metallicity enrichment are regulated by the interplay between the energy input from supernovae, and the temperature and pressure of the hot X-ray gas in ETGs. For all mass ranges, positive age gradients are associated with old galaxies (>5-7 Gyr). For galaxies younger than ∼5 Gyr, mostly at low mass, the age gradient tends to be anti-correlated with the Age parameter, with more positive gradients at younger ages.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1006.4056}, -author = {Barbera, F. La and {De Carvalho}, R. R. and {De La Rosa}, I. G. and Gal, R. R. and Swindle, R. and Lopes, P. A.A.}, -doi = {10.1088/0004-6256/140/5/1528}, -eprint = {1006.4056}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {Evolution - Galaxies,Formation - Galaxies,Fundamental parameters,Galaxies}, -month = {nov}, -number = {5}, -pages = {1528--1556}, -primaryClass = {astro-ph.CO}, -title = {{Spider. IV. Optical and near-infrared color gradients in early-type galaxies: New insight into correlations with galaxy properties}}, -url = {http://stacks.iop.org/1538-3881/140/i=5/a=1528?key=crossref.aeafeae7d16ab184d33f1707803b9e32}, -volume = {140}, -year = {2010} -} -@article{Collett2018, -author = {Collett, Thomas E and Oldham, Lindsay J and Smith, Russell J and Auger, Matthew W and Westfall, Kyle B and Bacon, David and Nichol, Robert C and Masters, Karen L}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Collett2018GR.pdf:pdf}, -journal = {Science}, -number = {1395}, -pages = {1342--1346}, -title = {{A precise extragalactic test of General Relativity}}, -volume = {360}, -year = {2018} -} -@article{Tao2012, -abstract = {Astrophysics gives evidence for the existence of Dark Matter and puts constraints on its nature. The Cold Dark Matter model has become "standard" cosmology combined with a cosmological constant. There are indications that "Cold" Dark Matter could be "warmer" than initially discussed. This paper reviews the main information on the Cold/Warm nature of Dark Matter.}, -author = {Tao, C.}, -doi = {10.1051/eas/1253012}, -file = {:C\:/Users/Jammy/Documents/Papers/PartB1_DMIDAS(1).pdf:pdf}, -issn = {1633-4760}, -journal = {EAS Publications Series}, -pages = {97--104}, -title = {{Astrophysical constraints on Dark Matter}}, -volume = {53}, -year = {2012} -} -@article{Greene2017b, -abstract = {The "kinematic" morphology-density relation for early-type galaxies posits that those galaxies with low angular momentum are preferentially found in the highest-density regions of the universe. We use a large sample of galaxy groups with halo masses 10^12.5 < M_halo < 10^14.5 M_sun/h observed with the Mapping Nearby Galaxies at APO (MaNGA) survey to examine whether there is a correlation between local environment and rotational support that is independent of stellar mass. We find no compelling evidence for a relationship between the angular momentum content of early-type galaxies and either local overdensity or radial position within the group at fixed stellar mass.}, -archivePrefix = {arXiv}, -arxivId = {1708.07843}, -author = {Greene, J. E. and Leauthaud, A. and Emsellem, E. and Goddard, D. and Ge, J. and Andrews, B. H. and Brinkman, J. and Brownstein, J. R. and Greco, J. and Law, D. and Lin, Y.-T. and Masters, K. L. and Merrifield, M. and More, S. and Okabe, N. and Schneider, D. P. and Thomas, D. and Wake, D. A. and Yan, R. and Drory, N.}, -doi = {10.3847/2041-8213/aa8ace}, -eprint = {1708.07843}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2017 - SDSS-IV MaNGA Probing the Kinematic Morphology–Density Relation of Early-type Galaxies with MaNGA.pdf:pdf}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L33}, -title = {{SDSS-IV MaNGA: Probing the Kinematic Morphology–Density Relation of Early-type Galaxies with MaNGA}}, -url = {http://arxiv.org/abs/1708.07843%0Ahttp://dx.doi.org/10.3847/2041-8213/aa8ace}, -volume = {851}, -year = {2017} -} -@article{Greco2017, -abstract = {We present a catalog of extended low-surface-brightness galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first ${\sim}$200 deg$^2$ of the survey, we have uncovered 781 LSBGs, spanning red ($g-i\geq0.64$) and blue ($g-i<0.64$) colors and a wide range of morphologies. Since we focus on extended galaxies ($r_\mathrm{eff}=2.5$-$14^{\prime\prime}$), our sample is likely dominated by low-redshift objects. We define LSBGs to have mean surface brightnesses $\bar{\mu}_\mathrm{eff}(g)>24.3$ mag arcsec$^{-2}$, which allows nucleated galaxies into our sample. As a result, the central surface brightness distribution spans a wide range of $\mu_0(g)=18$-$27.4$ mag arcsec$^{-2}$, with 50% and 95% of galaxies fainter than 24.3 and 22 mag arcsec$^{-2}$, respectively. Furthermore, the surface brightness distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well-characterized by single-component S\'{e}rsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We crossmatch our sample with existing optical, HI, and ultraviolet catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, ranging from dwarf spheroidals and ultra-diffuse galaxies in nearby groups to gas-rich irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the LSBG population.}, -archivePrefix = {arXiv}, -arxivId = {1709.04474}, -author = {Greco, Johnny P. and Greene, Jenny E. and Strauss, Michael A. and Macarthur, Lauren A. and Flowers, Xzavier and Goulding, Andy D. and Huang, Song and Kim, Ji Hoon and Komiyama, Yutaka and Leauthaud, Alexie and Leisman, Lukas and Lupton, Robert H. and Sif{\'{o}}n, Crist{\'{o}}bal and Wang, Shiang-Yu}, -doi = {10.3847/1538-4357/aab842}, -eprint = {1709.04474}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greco et al. - 2018 - Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {dwarf,galaxies,general,keywords}, -number = {2}, -pages = {104}, -title = {{Illuminating Low Surface Brightness Galaxies with the Hyper Suprime-Cam Survey}}, -url = {http://arxiv.org/abs/1709.04474%0Ahttp://dx.doi.org/10.3847/1538-4357/aab842}, -volume = {857}, -year = {2018} -} -@article{Hall2014a, -abstract = {Charge-Coupled Devices are the detector of choice for the focal planes of many optical and X-ray space telescopes. In recent years, EM-CCDs, SCDs and CMOS sensors have been used, or baselined, for missions in which the detection of X-ray and visible photons are key to the science goals of the mission. When placed in orbit, silicon-based detectors will suffer radiation damage as a consequence of the harsh space radiation environment, creating traps in the silicon. The radiation-induced traps will capture and release signal electrons, effectively "smearing" the image. Without correction, this smearing of the image would have major consequences on the science goals of the missions. Fitting to observed results, through careful planning of observation strategies while the radiation dose received remains low in the early stages of the mission, has previously been used to correct against the radiation damage effects. As the science goals becoming increasingly demanding, however, the correction algorithms require greater accuracy and a more physical approach is required, removing the effects of the radiation damage by modelling the trap capture and release mechanisms to a high level of detail. The drive for increasingly accurate trap parameters has led to the development of new methods of characterisation of traps in the silicon, measuring the trap properties and their effects to the single-trap level in situ. Here, we summarise the latest developments in trap characterisation techniques for n-channel and p-channel devices. ? 2014 SPIE.}, -author = {Hall, David J. and Murray, Neil and Gow, Jason and Wood, Daniel and Holland, Andrew}, -doi = {10.1117/12.2055906}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hall et al. - 2014 - In situ trap parameter studies in CCDs for space applications.pdf:pdf}, -isbn = {9780819496225}, -issn = {0277-786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VI}, -keywords = {[CCD, CTI, Defect, Euclid, Gaia, HST, N-channel, P}, -number = {0}, -pages = {915408}, -title = {{ In situ trap parameter studies in CCDs for space applications }}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2055906}, -volume = {9154}, -year = {2014} -} -@article{Lovell2018a, -abstract = {We use the IllustrisTNG (TNG) cosmological simulations to provide theoretical expectations for the dark matter mass fractions (DMFs) and circular velocity profiles of galaxies. TNG predicts flat circular velocity curves for z = 0 Milky Way (MW)-like galaxies beyond a few kpc from the galaxy centre, in better agreement with observational constraints than its predecessor, Illustris. TNG also predicts an enhancement of the dark matter mass within the 3D stellar half-mass radius (rhalf; M200c = 1010-1013M⊙, z ≤ 2) compared to its dark matter only and Illustris counterparts. This enhancement leads TNG present-day galaxies to be dominated by dark matter within their inner regions, with fDM(< rhalf) ≳ 0.5 at all masses and with a minimum for MW-mass galaxies. The 1$\sigma$ scatter is ≲10 per cent at all apertures, which is smaller than that inferred by some observational data sets, e.g. 40 per cent from the SLUGGS survey. TNG agrees with the majority of the observationally inferred values for elliptical galaxies once a consistent initial mass function is adopted (Chabrier) and the DMFs are measured within the same apertures. The DMFs measured within rhalf increase towards lower redshifts: this evolution is dominated by the increase in galaxy size with time. At z $\sim$ 2, the DMF in disc-like TNG galaxies decreases with increasing galaxy mass, with fDM(< rhalf) $\sim$ 0.10-0.65 for 1010 ≲ Mstars/M⊙ ≲ 1012, and are two times higher than if TNG galaxies resided in Navarro-Frenk-White dark matter haloes unaffected by baryonic physics. It remains to be properly assessed whether recent observational estimates of the DMFs at z $\sim$2 rule out the contraction of the dark matter haloes predicted by the TNG model.}, -archivePrefix = {arXiv}, -arxivId = {1801.10170}, -author = {Lovell, Mark R. and Pillepich, Annalisa and Genel, Shy and Nelson, Dylan and Springel, Volker and Pakmor, R{\"{u}}diger and Marinacci, Federico and Weinberger, Rainer and Torrey, Paul and Vogelsberger, Mark and Alabi, Adebusola and Hernquist, Lars}, -doi = {10.1093/MNRAS/STY2339}, -eprint = {1801.10170}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lovell et al. - 2018 - The fraction of dark matter within galaxies from the IllustrisTNG simulations.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {(cosmology:) dark matter,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1950--1975}, -title = {{The fraction of dark matter within galaxies from the IllustrisTNG simulations}}, -volume = {481}, -year = {2018} -} -@article{Hall2014, -abstract = {The science goals of space missions from the Hubble Space Telescope through to Gaia and Euclid require ultraprecise positional, photometric, and shape measurement information. However, in the radiation environment of the space telescopes, damage to the focal plane detectors through high-energy protons leads to the creation of traps, a loss of charge transfer efficiency, and a consequent deterioration in measurement accuracy. An understanding of the traps produced and their properties in the CCD during operation is essential to allow optimization of the devices and suitable modeling to correct the effect of the damage through the postprocessing of images. The technique of 'pumping single traps' has allowed the study of individual traps in high detail that cannot be achieved with other techniques, such as deep level transient spectroscopy, whilst also locating each trap to the subpixel level in the device. Outlining the principles used, we have demonstrated the technique for the A-center, the most influential trap in serial readout, giving results consistent with the more general theoretical values, but here showing new results indicating the spread in the emission times achieved and the variation in capture probability of individual traps with increasing signal levels. This technique can now be applied to other time and temperature regimes in the CCD to characterize individual traps in situ under standard operating conditions such that dramatic improvements can be made to optimization processes and modeling techniques. {\textcopyright}2013 IEEE.}, -author = {Hall, David J and Murray, Neil J and Holland, Andrew D and Gow, Jason and Clarke, Andrew and Burt, David}, -doi = {10.1109/TNS.2013.2295941}, -isbn = {9781467350570}, -issn = {00189499}, -journal = {IEEE Transactions on Nuclear Science}, -keywords = {A-centre,CCD image sensors,Euclid,Si-A,defect,pocket pumping,radiation damage,trap pumping}, -number = {4}, -pages = {1826--1833}, -title = {{Determination of in situ trap properties in CCDs using a "single-trap pumping" technique}}, -volume = {61}, -year = {2014} -} -@article{Kremer2017, -abstract = {Astrophysics and cosmology are rich with data. The advent of wide-area digital cameras on large aperture telescopes has led to ever more ambitious surveys of the sky. Data volumes of entire surveys a decade ago can now be acquired in a single night, and real-time analysis is often desired. Thus, modern astronomy requires big data know-how, in particular, highly efficient machine learning and image analysis algorithms. But scalability isn't the only challenge: astronomy applications touch several current machine learning research questions, such as learning from biased data and dealing with label and measurement noise. The authors argue that this makes astronomy a great domain for computer science research, as it pushes the boundaries of data analysis. They focus here on exemplary results, discuss main challenges, and highlight some recent methodological advancements in machine learning and image analysis triggered by astronomical applications.}, -archivePrefix = {arXiv}, -arxivId = {1704.04650}, -author = {Kremer, Jan and Stensbo-Smidt, Kristoffer and Gieseke, Fabian and Pedersen, Kim Steenstrup and Igel, Christian}, -doi = {10.1109/MIS.2017.40}, -eprint = {1704.04650}, -issn = {15411672}, -journal = {IEEE Intelligent Systems}, -keywords = {astronomy,big data,computer vision,intelligent systems,machine learning}, -number = {2}, -pages = {16--22}, -title = {{Big Universe, Big Data: Machine Learning and Image Analysis for Astronomy}}, -volume = {32}, -year = {2017} -} -@article{Cautun2015, -abstract = {The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model ({\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of the MW and M31 planes in {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high resolution cosmological simulations. We find that planar structures are very common, and that {\$\sim${}}10{\%} of {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM predictions. In fact, {\$\sim${}}10{\%} of {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1506.04151}, -author = {Cautun, Marius and Bose, Sownak and Frenk, Carlos S and Guo, Qi and Han, Jiaxin and Hellwing, Wojciech A and Sawala, Till and Wang, Wenting}, -doi = {10.1093/mnras/stv1557}, -eprint = {1506.04151}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {4}, -pages = {3838--3852}, -title = {{Planes of satellite galaxies: When exceptions are the rule}}, -volume = {452}, -year = {2015} -} -@article{Rawle2010, -abstract = {We present the stellar population and velocity dispersion gradients for a sample of 24 brightest cluster galaxies (BCGs) in the nearby Universe for which we have obtained high-quality long-slit spectra at the Gemini telescopes. With the aim of studying the possible connection between the formation of the BCGs and their host clusters, we explore the relations between the stellar population gradients and properties of the host clusters, as well as the possible connections between the stellar population gradients and other properties of the galaxies. We find mean stellar population gradients (negative $\Delta$[Z/H]/logr gradient of -0.285 ± 0.064, small positive $\Delta$log (age)/logr gradient of 0.069 ± 0.049 and null $\Delta$[E/Fe]/logr gradient of -0.008 ± 0.032) that are consistent with those of normal massive elliptical galaxies. However, we find a trend between metallicity gradients and velocity dispersion (with a negative slope of -1.616 ± 0.539) that is not found for the most massive ellipticals. Furthermore, we find trends between the metallicity gradients and K-band luminosities (with a slope of 0.173 ± 0.081) as well as the distance from the BCG to the X-ray peak of the host cluster (with a slope of -7.546 ± 2.752). The latter indicates a possible relation between the formation of the cluster and that of the central galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1204.3601}, -author = {Loubser, S. I. and S{\'{a}}nchez-Bl{\'{a}}zquez, P.}, -doi = {10.1111/j.1365-2966.2012.21079.x}, -eprint = {1204.3601}, -isbn = {00358711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: evolution,Galaxies: stellar content}, -number = {2}, -pages = {841--861}, -title = {{Stellar population gradients in brightest cluster galaxies}}, -volume = {425}, -year = {2012} -} -@article{Rest2001, -abstract = {We present high-resolution R -band images of the central regions of 67 early-type galaxies obtained with the Wide Field and Planetary Camera 2 (WFPC2) aboard the Hubble Space Telescope ( HST ). This homogeneously selected sample roughly doubles the number of early-type galaxies that have now been imaged at HST resolution and complements similar data on the central regions of radio galaxies and the bulges of spiral galaxies. Our sample strikingly confirms the complex morphologies of the central regions of early-type galaxies which have become apparent from previous studies with HST . In particular, we detect dust, either in the form of nuclear disks or with a filamentary distribution, in 43% of all galaxies, in good agreement with previous estimates. In addition, we find evidence for embedded stellar disks in a remarkably large fraction of 51%. In 14 of those galaxies the disklike structures are misaligned with the main galaxy, suggesting that they correspond to stellar bars in S0 galaxies. We analyze the luminosity profiles of the galaxies in our sample and classify galaxies according to their central cusp slope. To a large extent we confirm the results from previous HST surveys in that early-type galaxies reveal a clear dichotomy: the bright ellipticals ( M B ##IMG## [http://ej.iop.org/icons/Entities/lesssim.gif] {lesssim} -20.5) are generally boxy and have luminosity profiles that break from steep outer power laws to shallow inner cusps (referred to as "core" galaxies). The fainter ellipticals, on the other hand, typically have disky isophotes and luminosity profiles that lack a clear break and have a steep central cusp (referred to as "power-law" galaxies). The advantages and shortcomings of classification schemes utilizing the extrapolated central cusp slope $\gamma$ are discussed, and it is shown that $\gamma$ might be an inadequate representation for galaxies whose luminosity profile slope changes smoothly with radius rather than resembling a broken power law. Thus, we introduce a new, alternative parameter and show how this affects the classification. In fact, we find evidence for an "intermediate" class of galaxies that cannot unambiguously be classified as either core or power-law galaxies and that have central cusp slopes and absolute magnitudes intermediate between those of core and power-law galaxies. It is unclear at present, however, whether these galaxies make up a physically distinct class or whether distance and/or resolution effects cause them to lose their distinct core or power-law characteristics.}, -author = {Rest, Armin and van den Bosch, Frank C. and Jaffe, Walter and Tran, Hien and Tsvetanov, Zlatan and Ford, Holland C. and Davies, James and Schafer, Joanna}, -doi = {10.1086/320370}, -issn = {00046256}, -journal = {The Astronomical Journal}, -keywords = {cd {\`{e}} galaxies,elliptical and lenticular,galaxies,nuclei {\`{e}} galaxies,structure}, -number = {5}, -pages = {2431--2482}, -title = {{WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data}}, -volume = {121}, -year = {2001} -} -@article{Mukherjee2021, -abstract = {We use nine different galaxy formation scenarios in ten cosmological simulation boxes from the EAGLE (Evolution and Assembly of GaLaxies and their Environments) suite of Lambda cold dark matter hydrodynamical simulations to assess the impact of feedback mechanisms in galaxy formation and compare these to observed strong gravitational lenses. To compare observations with simulations, we create strong lenses with M∗ > 1011 M with the appropriate resolution and noise level, and model them with an elliptical power-law mass model to constrain their total mass density slope. We also obtain the mass-size relation of the simulated lens-galaxy sample. We find significant variation in the total mass density slope at the Einstein radius and in the projected stellar mass-size relation, mainly due to different implementations of stellar and active galactic nucleus (AGN) feedback. We find that for lens-selected galaxies, models with either too weak or too strong stellar and/or AGN feedback fail to explain the distribution of observed mass density slopes, with the counter-intuitive trend that increasing the feedback steepens the mass density slope around the Einstein radius (≈3-10 kpc). Models in which stellar feedback becomes inefficient at high gas densities, or weaker AGN feedback with a higher duty cycle, produce strong lenses with total mass density slopes close to isothermal [i.e. -dlog ($\rho$)/dlog (r) ≈ 2.0] and slope distributions statistically agreeing with observed strong-lens galaxies in Sloan Lens ACS Survey and BOSS (Baryon Oscillation Spectroscopic Survey) Emission-Line Lens Survey. Agreement is only slightly worse with the more heterogeneous Strong Lensing Legacy Survey lens-galaxy sample. Observations of strong-lens-selected galaxies thus appear to favour models with relatively weak feedback in massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1901.01095}, -author = {Mukherjee, Sampath and Koopmans, L{\'{e}}on V.E. and Metcalf, R. Benton and Tortora, Cresenzo and Schaller, Matthieu and Schaye, Joop and Vernardos, Georgios and Bellagamba, Fabio}, -doi = {10.1093/mnras/stab693}, -eprint = {1901.01095}, -file = {:C\:/Users/Jammy/Documents/Papers/Simulation/Mukherjee2019SEGLE2.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: structure,galaxy formation,gravitational lensing: strong,methods: numerical}, -number = {3}, -pages = {3455--3477}, -title = {{SEAGLE - II. Constraints on feedback models in galaxy formation from massive early-type strong-lens galaxies}}, -volume = {504}, -year = {2021} -} -@article{Bruce2014, -abstract = {We present the results of a new and improved study of the morphological and spectral evolution of massive galaxies over the redshift range 1{\textless}z{\textless}3. Our analysis is based on a bulge-disk decomposition of 396 galaxies with Mstar{\textgreater}10{\^{}}11 Msolar from the CANDELS WFC3/IR imaging within the COSMOS and UKIDSS UDS survey fields. We find that, by modelling the H(160) image of each galaxy with a combination of a de Vaucouleurs bulge (Sersic index n=4) and an exponential disk (n=1), we can then lock all derived morphological parameters for the bulge and disk components, and successfully reproduce the shorter-wavelength J(125), i(814), v(606) HST images simply by floating the magnitudes of the two components. This then yields sub-divided 4-band HST photometry for the bulge and disk components which, with no additional priors, is well described by spectrophotometric models of galaxy evolution. Armed with this information we are able to properly determine the masses and star-formation rates for the bulge and disk components, and find that: i) from z=3 to z=1 the galaxies move from disk-dominated to increasingly bulge-dominated, but very few galaxies are pure bulges/ellipticals by z=1; ii) while most passive galaxies are bulge-dominated, and most star-forming galaxies disk-dominated, 18+/-5{\%} of passive galaxies are disk-dominated, and 11+/-3{\%} of star-forming galaxies are bulge-dominated, a result which needs to be explained by any model purporting to connect star-formation quenching with morphological transformations; iii) there exists a small but significant population of pure passive disks, which are generally flatter than their star-forming counterparts (whose axial ratio distribution peaks at b/a{\$\sim${}}0.7); iv) flatter/larger disks re-emerge at the highest star-formation rates, consistent with recent studies of sub-mm galaxies, and with the concept of a maximum surface-density for star-formation activity.}, -archivePrefix = {arXiv}, -arxivId = {1405.1736}, -author = {Bruce, V A and Dunlop, J S and McLure, R J and Cirasuolo, M and Buitrago, F and Bowler, R A A and Targett, T A and Bell, E F and McIntosh, D H and Dekel, A and Faber, S M and Ferguson, H C and Grogin, N A and Hartley, W and Kocevski, D D and Koekemoer, A M and Koo, D C and McGrath, E J}, -doi = {10.1093/mnras/stu1478}, -eprint = {1405.1736}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: Elliptical and lenticular,Galaxies: Evolution,Galaxies: Highredshift,Galaxies: Spiral,Galaxies: Structure,cD}, -month = {oct}, -number = {2}, -pages = {1001--1033}, -title = {{The bulge-disc decomposed evolution of massive galaxies at 1 {\textless} z {\textless} 3 in CANDELS}}, -volume = {444}, -year = {2014} -} -@article{Dye2005, -abstract = {We measure the mass density profile of the lens galaxy in the Einstein ring system 0047-2808 using our semi-linear inversion method developed in an earlier paper. By introducing an adaptively gridded source plane, we are able to eliminate the need for regularisation of the inversion. This removes the problem of a poorly defined number of degrees of freedom, encountered by inversion methods that employ regularisation, and so allows a proper statistical comparison between models. We confirm the results of Wayth et al. (2004), that the source is double, and that a power-law model gives a significantly better fit that the singular isothermal ellipsoid model. We measure a slope alpha=2.11+/-0.04. We find, further, that a dual-component constant M/L baryonic + dark halo model gives a significantly better fit than the power-law model, at the 99.7% confidence level. The inner logarithmic slope of the dark halo profile is found to be 0.87^{+0.69}_{-0.61} (95% CL), consistent with the predictions of CDM simulations of structure formation. We determine an unevolved B-band mass to light ratio for the baryons (only) of 3.05^{+0.53}_{-0.90} h_65 M_sol/L_Bsol (95% CL). This is the first measurement of the baryonic M/L of a single galaxy by purely gravitational lens methods. The baryons account for 65^{+10}_{-18}% (95% CL) of the total projected mass, or, assuming spherical symmetry, 84^{+12}_{-24}% (95% CL) of the total three-dimensional mass within the mean radius of 1.16'' (7.5 h_65^{-1} kpc) traced by the ring. Finally, at the level of >3sigma, we find that the halo mass is rounder than the baryonic distribution and that the two components are offset in orientation from one another.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0411452}, -author = {Dye, S. and Warren, S. J.}, -doi = {10.1086/428340}, -eprint = {0411452}, -issn = {0004-637X}, -journal = {ApJ}, -number = {1}, -pages = {31--41}, -primaryClass = {astro-ph}, -title = {{Decomposition of the Visible and Dark Matter in the Einstein Ring 0047−2808 by Semilinear Inversion}}, -url = {http://stacks.iop.org/0004-637X/623/i=1/a=31}, -volume = {623}, -year = {2005} -} -@article{Tinker2016, -abstract = {We present measurements of the clustering of galaxies as a function of their stellar mass in the Baryon Oscillation Spectroscopic Survey. We compare the clustering of samples using 12 different methods for estimating stellar mass, isolating the method that has the smallest scatter at fixed halo mass. In this test, the stellar mass estimate with the smallest errors yields the highest amplitude of clustering at fixed number density. We find that the PCA stellar masses of Chen etal (2012) clearly have the tightest correlation with halo mass. The PCA masses use the full galaxy spectrum, differentiating them from other estimates that only use optical photometric information. Using the PCA masses, we measure the large-scale bias as a function of Mgal for galaxies with logMgal{\textgreater}=11.4, correcting for incompleteness at the low-mass end of our measurements. Using the abundance-matching ansatz to connect dark matter halo mass to stellar mass, we construct theoretical models of b(Mgal) that match the same stellar mass function but have different amounts of scatter in stellar mass at fixed halo mass, sigma{\_}logM. Using this approach, we find sigma{\_}logM=0.18{\^{}}{\{}+0.01{\}}{\_}{\{}-0.02{\}}. This value includes both intrinsic scatter as well as random errors in the stellar masses. To partially remove the latter, we use repeated spectra to estimate statistical errors on the stellar masses, yielding an upper limit to the intrinsic scatter of 0.16 dex.}, -archivePrefix = {arXiv}, -arxivId = {1607.04678}, -author = {Tinker, Jeremy L and Brownstein, Joel R and Guo, Hong and Leauthaud, Alexie and Maraston, Claudia and Masters, Karen and Montero-Dorta, Antonio D and Thomas, Daniel and Tojeiro, Rita and Weiner, Benjamin and Zehavi, Idit and Olmstead, Matthew D}, -doi = {10.3847/1538-4357/aa6845}, -eprint = {1607.04678}, -issn = {1538-4357}, -title = {{The Correlation Between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe}}, -url = {http://arxiv.org/abs/1607.04678%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa6845}, -year = {2016} -} -@article{Machanek1993, -author = {MACHACEK, MARIE E. and CARLSON, ERIC D. and HALL, LAWRENCE J.}, -doi = {10.1111/j.1749-6632.1993.tb43955.x}, -issn = {17496632}, -journal = {Annals of the New York Academy of Sciences}, -number = {1}, -pages = {681--685}, -title = {{Self‐Interacting Dark Matter: An Alternative Scenario?}}, -volume = {688}, -year = {1993} -} -@article{Pontzen2015a, -abstract = {Galaxies and the dark matter haloes that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealized calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter core-creation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are 'maximally stable', i.e. that do not evolve at first order when external potentials (which arise from baryons, large-scale tidal fields or infalling substructure) are applied. We show that a spherically symmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for near-isotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealized spherically symmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter haloes (formed in collisionless cosmological simulations) nearly attain our maximally stable limit, but their evolution freezes out before reaching it.}, -archivePrefix = {arXiv}, -arxivId = {1502.07356}, -author = {Pontzen, Andrew and Read, Justin I and Teyssier, Romain and Governato, Fabio and Gualandris, Alessia and Roth, Nina and Devriendt, Julien}, -doi = {10.1093/mnras/stv1032}, -eprint = {1502.07356}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {1366--1379}, -title = {{Milking the spherical cow - on aspherical dynamics in spherical coordinates}}, -volume = {451}, -year = {2015} -} -@article{Goobar2016, -abstract = {We report the discovery of a multiply imaged, gravitationally lensed type Ia supernova, iPTF16geu (SN 2016geu), at redshift z = 0.409. This phenomenon was identified because the light from the stellar explosion was magnified more than 50 times by the curvature of space around matter in an intervening galaxy.We used high-spatial-resolution observations to resolve four images of the lensed supernova, approximately 0.3 arc seconds from the center of the foreground galaxy. The observations probe a physical scale of {\$\sim${}}1 kiloparsec, smaller than is typical in other studies of extragalactic gravitational lensing. The large magnification and symmetric image configuration imply close alignment between the lines of sight to the supernova and to the lens. The relative magnifications of the four images provide evidence for substructures in the lensing galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1611.00014}, -author = {Goobar, A and Amanullah, R and Kulkarni, S R and Nugent, P E and Johansson, J and Steidel, C and Law, D and M{\"{o}}rtsell, E and Quimby, R and Blagorodnova, N and Brandeker, A and Cao, Y and Cooray, A and Ferretti, R and Fremling, C and Hangard, L and Kasliwal, M and Kupfer, T and Lunnan, R and Masci, F and Miller, A A and Nayyeri, H and Neill, J D and Ofek, E O and Papadogiannakis, S and Petrushevska, T and Ravi, V and Sollerman, J and Sullivan, M and Taddia, F and Walters, R and Wilson, D and Yan, L and Yaron, O}, -doi = {10.1126/science.aal2729}, -eprint = {1611.00014}, -isbn = {1095-9203 (Electronic) 0036-8075 (Linking)}, -issn = {10959203}, -journal = {Science}, -number = {6335}, -pages = {291--295}, -pmid = {28428419}, -title = {{IPTF16geu: A multiply imaged, gravitationally lensed type ia supernova}}, -url = {http://arxiv.org/abs/1611.00014}, -volume = {356}, -year = {2017} -} -@article{Lackner2012, -abstract = {We present a set of bulge-disc decompositions for a sample of 71 825 Sloan Digital Sky Survey (SDSS) main-sample galaxies in the redshift range 0.003 {\textless} z {\textless} 0.05. We have fitted each galaxy with either a de Vaucouleurs ('classical') or an exponential ('pseudo-') bulge and an exponential disc. Two-dimensional S{\'{e}}rsic fits are performed when the two-component fits are not statistically significant or when the fits are poor, even in the presence of high signal-to-noise ratio (S/N). We study the robustness of our two-component fits by studying a bright subsample of galaxies and we study the systematics of these fits with decreasing resolution and S/N. Only 30 per cent of our sample have been fitted with two-component fits in which both components are non-zero. The g-r and g-i colours of each component for the two-component models are determined using linear templates derived from the r-band model. We attempt a physical classification of types of fits into disc galaxies, pseudo-bulges, classical bulges and ellipticals. Our classification of galaxies agrees well with previous large bulge plus disc (B+D) decomposed samples. Using our galaxy classifications, we find that Petrosian concentration is a good indicator of bulge-to-total ratio, while overall S{\'{e}}rsic index is not. Additionally, we find that the majority of green valley galaxies are bulge+disc galaxies. Furthermore, in the transition from green to red B+D galaxies, the total galaxy colour is most strongly correlated with the disc colour.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph.CO/1201.0763}, -author = {Lackner, C N and Gunn, J E}, -doi = {10.1111/j.1365-2966.2012.20450.x}, -eprint = {1201.0763}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: photometry,Galaxies: structure}, -number = {3}, -pages = {2277--2302}, -primaryClass = {astro-ph.CO}, -title = {{Astrophysically motivated bulge-disc decompositions of Sloan Digital Sky Survey galaxies}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data%7B%5C_%7Dquery?bibcode=2012arXiv1201.0763L%7B%5C&%7Dlink%7B%5C_%7Dtype=ABSTRACT%7B%5C%25%7D5Cnpapers2://publication/uuid/85C0F4F3-26D1-423F-8472-7E24A25541A6}, -volume = {421}, -year = {2012} -} -@article{Gadotti2011, -abstract = {I present results from the modeling of stellar bars in nearly 300 barred galaxies in the local universe through parametric multi-component multi-band image fitting. The surface brightness radial profile of bars is described using a Sersic function, and parameters such as bar effective radius, ellipticity, boxiness, length and mass, and bar-to-total luminosity and mass ratios, are determined, which is unprecedented for a sample of this size. The properties of bars in galaxies with classical bulges and pseudo-bulges are compared. For a fixed bar-to-total mass ratio, pseudo-bulges are on average significantly less massive than classical bulges, indicating that, if pseudo-bulges are formed through bars, further processes are necessary to build a classical bulge. I find a correlation between bar ellipticity and boxiness, and define a new parameter as the product of these two quantities. I also find correlations between this product and normalised bar size, between the sizes of bars and bulges, and between normalised bar size and bulge-to-total ratio. Bars with different ellipticities follow parallel lines in the latter two correlations. These correlations can arise if, starting off with different normalised sizes and ellipticities, bars grow longer and stronger with dynamical age, as a result of angular momentum exchange from the inner to the outer parts of galaxies, consistent with previous theoretical predictions. A plausible consequence is that bar pattern speeds should become lower with bar dynamical age, and towards galaxies with more prominent bulges.}, -archivePrefix = {arXiv}, -arxivId = {1003.1719}, -author = {Gadotti, Dimitri A}, -doi = {10.1111/j.1365-2966.2011.18945.x}, -eprint = {1003.1719}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: photometry,Galaxies: structure}, -number = {4}, -pages = {3308--3318}, -title = {{Secular evolution and structural properties of stellar bars in galaxies}}, -volume = {415}, -year = {2011} -} -@article{Hopkins2011, -abstract = {We present analytic calculations of angular momentum transport and gas inflow in galaxies, from scales of {\$\sim${}}kpc to deep in the potential of a central black hole (BH). We compare these analytic calculations to numerical simulations and use them to develop a sub-grid model of BH growth that can be incorporated into semi-analytic models or cosmological simulations. Both analytic calculations and simulations argue that the strongest torque on gas arises when non-axisymmetric perturbations to the stellar gravitational potential produces orbit crossings and shocks in the gas. This is true both at large radii {\$\sim${}}0.01-1 kpc, where bar-like modes dominate the non-axisymmetric potential, and at smaller radii {\textless}10 pc, where a lopsided/eccentric disk dominates. The traditional orbit crossing criterion is not always adequate to predict the locations of, and inflow due to, shocks in gas+stellar disks with finite sound speeds. We derive a modified criterion that predicts the presence of shocks in stellar dominated systems even absent formal orbit crossing. We then derive analytic expressions for the loss of angular momentum and the resulting gas inflow rates in the presence of such shocks. We test our analytic predictions using hydrodynamic simulations at a range of galactic scales, and show that they successfully predict the mass inflow rates and quasi-steady gas surface densities with small scatter (0.3 dex). We use our analytic results to construct a new estimate of the BH accretion rate given galaxy properties at larger radii. This captures the key scalings in the numerical simulations. Alternate estimates such as the local viscous accretion rate or the spherical Bondi rate fail systematically to reproduce the simulations.}, -archivePrefix = {arXiv}, -arxivId = {1007.2647}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1365-2966.2011.18542.x}, -eprint = {1007.2647}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Quasars: general}, -number = {2}, -pages = {1027--1050}, -title = {{An analytic model of angular momentum transport by gravitational torques: From galaxies to massive black holes}}, -volume = {415}, -year = {2011} -} -@article{Xie2015, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -volume = {447}, -year = {2015} -} -@article{Cautun2015, -abstract = {The detection of planar structures within the satellite systems of both the Milky Way (MW) and Andromeda (M31) has been reported as being in stark contradiction to the predictions of the standard cosmological model ($\Lambda$ cold dark matter - $\Lambda$CDM). Given the ambiguity in defining a planar configuration, it is unclear how to interpret the low incidence of theMWand M31 planes in $\Lambda$CDM. We investigate the prevalence of satellite planes around galactic mass haloes identified in high-resolution cosmological simulations. We find that planar structures are very common, and that {\$\sim${}}10 per cent of $\Lambda$CDM haloes have even more prominent planes than those present in the Local Group. While ubiquitous, the planes of satellite galaxies show a large diversity in their properties. This precludes using one or two systems as small-scale probes of cosmology, since a large sample of satellite systems is needed to obtain a good measure of the object-to-object variation. This very diversity has been misinterpreted as a discrepancy between the satellite planes observed in the Local Group and $\Lambda$CDM predictions. In fact, {\$\sim${}}10 per cent of $\Lambda$CDM galactic haloes have planes of satellites that are as infrequent as the MW and M31 planes. The look-elsewhere effect plays an important role in assessing the detection significance of satellite planes and accounting for it leads to overestimating the significance level by a factor of 30 and 100 for the MW and M31 systems, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1506.04151}, -author = {Cautun, Marius and Bose, Sownak and Frenk, Carlos S and Guo, Qi and Han, Jiaxin and Hellwing, Wojciech A and Sawala, Till and Wang, Wenting}, -doi = {10.1093/mnras/stv1557}, -eprint = {1506.04151}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: abundances,Galaxies: haloes,Galaxies: statistics}, -number = {4}, -pages = {3838--3852}, -title = {{Planes of satellite galaxies: When exceptions are the rule}}, -volume = {452}, -year = {2015} -} -@article{Grillo2018, -abstract = {Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" ({\$}z = 1.489{\$}), which were obtained thanks to Hubble Space Telescope (HST) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5{\$}+{\$}2223 ({\$}z = 0.542{\$}), published by Grillo et al. (2016), and explore different {\$}\backslashLambda{\$}CDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of {\$}H{\_}{\{}0{\}}{\$} and {\$}\backslashOmega{\_}{\{}\backslashrm m{\}}{\$} with relative (1{\$}\backslashsigma{\$}) statistical errors of, respectively, 6{\%} (7{\%}) and 31{\%} (26{\%}) in flat (general) cosmological models, assuming a conservative 3{\%} uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of {\$}H{\_}{\{}0{\}}{\$}, based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.}, -archivePrefix = {arXiv}, -arxivId = {1802.01584}, -author = {Grillo, C and Rosati, P and Suyu, S H and Balestra, I and Caminha, G B and Halkola, A and Kelly, P L and Lombardi, M and Mercurio, A and Rodney, S A and Treu, T}, -doi = {10.3847/1538-4357/aac2c9}, -eprint = {1802.01584}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {2223,5,claudio,claudio grillo,clusters,corresponding author,cosmological parameters,dark energy,dark matter,distance scale,galaxies,gravitational lensing,grillo,individuals,it,macs j1149,strong,unimi}, -number = {2}, -pages = {94}, -title = {{Measuring the Value of the Hubble Constant “{\`{a}} la Refsdal”}}, -url = {http://arxiv.org/abs/1802.01584}, -volume = {860}, -year = {2018} -} -@article{Brooks2015, -abstract = {The latest generation of cosmological simulations are on the verge of being able to resolve the structure of bulges for the first time. Hence, we review the current state of bulge formation in cosmological simulations, and discuss open questions that can be addressed in the near future by simulators, with a particular focus on merger-driven bulge growth. Galaxy mergers have long been assumed to produce classical bulges in disc galaxies. Under this bulge-formationmodel, though, the high rates of mergers in Cold Dark Matter (CDM) galaxy formation theory predict many more classical bulges than are observed. Furthermore, simulations of galaxy formation continue to generally produce too massive of bulges. Feedback offers a promising avenue for reducing merger-driven bulge growth by maintaining high gas fractions in galaxies and ejecting low-angular momentum gas driven to the centers of galaxies. After reviewing the results of relevant research that has been published to date, we use cosmological simulations to explore the ability of feedback to reduce or even prevent bulge growth during mergers. In dwarf galaxies, mergers actually reduce the central concentration of galaxies as the induced burst of star formation drives out low-angular momentum material. This result shows the potential for feedback to reduce central mass growth. However, we also demonstrate that it is very difficult for current stellar feedback models to reproduce the small bulges observed in more massive disc galaxies like the Milky Way. We argue that feedback models need to be improved, or an additional source of feedback such as AGN is necessary to generate the required outflows.}, -archivePrefix = {arXiv}, -arxivId = {1511.04095}, -author = {Brooks, Alyson and Christensen, Charlotte}, -doi = {10.1007/978-3-319-19378-6_12}, -eprint = {1511.04095}, -isbn = {9783319193786}, -journal = {Galactic Bulges}, -pages = {317--353}, -title = {{Bulge formation via mergers in cosmological simulations}}, -volume = {418}, -year = {2015} -} -@article{Bullock2005a, -abstract = {If the favored hierarchical cosmological model is correct, then the Milky Way system should have accreted {\$\sim${}}100-200 luminous satellite galaxies in the past $\backslash${\$\sim${}}12 Gyr. We model this process using a hybrid semi-analytic plus N-body approach which distinguishes explicitly between the evolution of light and dark matter in accreted satellites. This distinction is essential to our ability to produce a realistic stellar halo, with mass and density profile much like that of our own Galaxy, and a surviving satellite population that matches the observed number counts and structural parameter distributions of the satellite galaxies of the Milky Way. Our model stellar halos have density profiles which typically drop off with radius faster than those of the dark matter. They are assembled from the inside out, with the majority of mass ({\$\sim${}}80{\%}) coming from the $\backslash${\$\sim${}}15 most massive accretion events. The satellites that contribute to the stellar halo have median accretion times of {\$\sim${}}9 Gyr in the past, while surviving satellite systems have median accretion times of {\$\sim${}}5 Gyr in the past. This implies that stars associated with the inner halo should be quite different chemically from stars in surviving satellites and also from stars in the outer halo or those liberated in recent disruption events. We briefly discuss the expected spatial structure and phase space structure for halos formed in this manner. Searches for this type of structure offer a direct test of whether cosmology is indeed hierarchical on small scales.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0506467}, -author = {Bullock, James S and Johnston, Kathryn V}, -doi = {10.1086/497422}, -eprint = {0506467}, -isbn = {0272-9490 (Print)$\backslash$r0272-9490 (Linking)}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {931--949}, -pmid = {10886430}, -primaryClass = {astro-ph}, -title = {{Tracing Galaxy Formation with Stellar Halos I: Methods}}, -url = {http://arxiv.org/abs/astro-ph/0506467%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/497422}, -volume = {635}, -year = {2005} -} -@article{Bristow2003, -author = {Bristow, Paul}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bristow - 2003 - Application of Model Derived Charge Transfer Inefficiency Corrections to STIS Photometric CCD Data(2).pdf:pdf}, -journal = {preprint (astro-ph/0310714)}, -keywords = {annotate,community,discipline,institutional,knowledge,patent,publication,read,science,share,source}, -month = {oct}, -title = {{Application of Model Derived Charge Transfer Inefficiency Corrections to STIS Photometric CCD Data}}, -year = {2003} -} -@article{Swinbank2006, -abstract = {We present two-dimensional spectroscopy covering the rest-frame wavelengths of strong optical emission lines in six luminous submillimetre galaxies (SMGs) at z = 1.3-2.5. Using this near-infrared integral field spectroscopy together with Hubble Space Telescope ACS and NICMOS imaging, we map the dynamics and morphologies of these systems on scales from 4-11 kpc. Four of the systems show multiple components in their spatially resolved spectra with average velocity offsets of ∼ 180 kms -1 across 8 kpc in projection. From the ensemble properties of eight galaxies, from our survey and the literature, we estimate the typical dynamical masses of bright SMGs as 5 ± 3 × 10 11 M ⊙. This is similar to recent estimates of their stellar masses - suggesting that the dynamics of the central regions of these galaxies are baryon dominated, with a substantial fraction of those baryons in stars by the epoch of observation. Combining our dynamical mass estimates with stellar luminosities for this population, we investigate whether SMGs can evolve on to the Faber-Jackson (FJ) relation for local ellipticals. Adopting a typical lifetime of $\tau$ burst ∼ 300 Myr for the submillimetre-luminous phase - using the latest estimates of gas masses, star formation rates and active galactic nucleus contribution to the bolometric luminosities - we find that the stellar populations of SMGs should fade to place them on the FJ relation, at M K ∼ -25.1. Furthermore, using the same starburst lifetime we correct the observed space density of SMGs for the duty cycle to derive a volume density of the progenitors of ∼1 × 10 -4 Mpc -3. This is consistent with the space density of local luminous early-type galaxies with M K ∼ -25.1, indicating that SMGs can evolve on to the scaling relations observed for local early-type galaxies, and the observed population at z ∼ 2 is then sufficient to account for the formation of the whole population of ≳3 L* K ellipticals seen at z ∼ 0. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0606372}, -author = {Swinbank, A. M. and Chapman, S. C. and Smail, Ian and Lindner, C. and Borys, C. and Blain, A. W. and Ivison, R. J. and Lewis, G. F.}, -doi = {10.1111/j.1365-2966.2006.10673.x}, -eprint = {0606372}, -isbn = {0102-0935}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: high-redshift,Galaxies: individual,Submillimetre}, -number = {1}, -pages = {465--476}, -primaryClass = {astro-ph}, -title = {{The link between submillimetre galaxies and luminous ellipticals: Near-infrared IFU spectroscopy of submillimetre galaxies}}, -volume = {371}, -year = {2006} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637x/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {21}, -title = {{ Supermassive Black Holes and Their Host Spheroids. Ii. the Red and Blue Sequence in the M Bh – M *,Sph Diagram }}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -volume = {817}, -year = {2016} -} -@article{DiazRivero2020, -abstract = {Strong gravitational lensing is a promising way of uncovering the nature of dark matter, by finding perturbations to images that cannot be accounted for well by modeling the lens galaxy without additional structure, be it subhalos (smaller halos within the smooth lens) or line-of-sight (LOS) halos. We present results attempting to infer the presence of substructure from images without requiring an intermediate step in which a smooth model has to be subtracted, using a simple convolutional neural network (CNN). We find that the network is only able to infer the presence of subhalos with greater than 75% accuracy when they have masses of greater than or equal to 5×109M if they lie within the main lens galaxy. Since less massive foreground LOS halos can have the same effect as higher-mass subhalos, the CNN can probe lower masses in the halo mass function. The accuracy does not improve significantly if we add a population of less massive subhalos. With the expectation of experiments such as Hubble Space Telescope and Euclid yielding thousands of high-quality strong lensing images in the next years, having a way of analyzing images quickly to identify candidates that merit further analysis to determine individual subhalo properties while preventing extensive resources being used for images that would yield null detections could be very useful. By understanding the sensitivity as a function of substructure mass, nondetections could be combined with the information from images with substructure to constrain the cold dark matter scenario, in particular if the sensitivity can be pushed to lower masses.}, -archivePrefix = {arXiv}, -arxivId = {1910.00015}, -author = {{Diaz Rivero}, Ana and Dvorkin, Cora}, -doi = {10.1103/PhysRevD.101.023515}, -eprint = {1910.00015}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Diaz Rivero, Dvorkin - 2020 - Direct detection of dark matter substructure in strong lens images with convolutional neural networks.pdf:pdf}, -issn = {24700029}, -journal = {Physical Review D}, -number = {2}, -pages = {1--17}, -title = {{Direct detection of dark matter substructure in strong lens images with convolutional neural networks}}, -volume = {101}, -year = {2020} -} -@article{Arcetri2018, -abstract = {We quantify the importance of mass accretion during active galactic nuclei (AGN) phases in the growth of supermassive black holes (BHs) by comparing the mass function of black holes in the Local Universe with that expected from AGN relics, which are black holes grown entirely with mass accretion during AGN phases. The local BH mass function (BHMF) is estimated by applying the well-known correlations between BH mass, bulge luminosity and stellar velocity dispersion to galaxy luminosity and velocity functions. We find that different correlations provide the same BHMF only if they have the same intrinsic dispersion. The density of supermassive black holes in the Local Universe that we estimate is $\rho$BH = 4.6-1.4+1.9h0.72 × 105 M⊙ Mpc-3. The relic BHMF is derived from the continuity equation with the only assumption that AGN activity is due to accretion on to massive BHs and that merging is not important. We find that the relic BHMF at z = 0 is generated mainly at z < 3 where the major part of the growth of a BH takes place. Moreover, BH growth is antihierarchical in the sense that smaller BHs (MBH < 10 7 M⊙) grow at lower redshifts (z < 1) with respect to more massive ones (z ∼ 1-3). Unlike previous work, we find that the BHMF of AGN relics is perfectly consistent with the local BHMF, indicating that local BHs were mainly grown during AGN activity. This agreement is obtained while satisfying, at the same time, the constraints imposed from the X-ray background (XRB). The comparison between the local and relic BHMFs also suggests that the merging process is not important in shaping the relic BHMF, at least at low redshifts (z < 3), and allows us to estimate the average radiative efficiency (e), the ratio between emitted and Eddington luminosity (A.) and the average lifetime of active BHs. Our analysis thus suggests the following scenario: local BHs grew during AGN phases in which accreting matter was converted into radiation with efficiencies $\epsilon$ = 0.04-0.16 and emitted at a fraction $\Lambda$ = 0.1-1.7 of the Eddington luminosity. The average total lifetime of these active phases ranges from ≃ 4.5 × 108 yr for MBH < 108 M⊙ to ≃ 1.5 × 108 yr for MBH > 109 M⊙, but can become as large as ∼109 yr for the lowest acceptable $\epsilon$ and $\lambda$values.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0311619}, -author = {Marconi, A. and Risaliti, G. and Gilli, R. and Hunt, L. K. and Maiolino, R. and Salvati, M.}, -doi = {10.1111/j.1365-2966.2004.07765.x}, -eprint = {0311619}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Marconi et al. - 2004 - Local supermassive black holes, relics of active galactic nuclei and the X-ray background.pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Cosmology: miscellaneous,Galaxies: active,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -pages = {169--185}, -primaryClass = {astro-ph}, -title = {{Local supermassive black holes, relics of active galactic nuclei and the X-ray background}}, -volume = {351}, -year = {2004} -} -@article{Numpy2011, -author = {van der Walt, S and Colbert, S C and Varoquaux, G}, -journal = {Computing in Science Engineering}, -number = {2}, -pages = {22--30}, -title = {{The NumPy Array: A Structure for Efficient Numerical Computation}}, -volume = {13}, -year = {2011} -} -@article{Gaitskell2004, -abstract = {This article is a brief overview of the status of direct detection experiments of the dark matter, especially searching for WIMPs (Weakly Interacting Massive Particles) at deep underground laboratory, when it was discussed at 37th international conference on high energy physics (ICHEP2018) in Seoul, Korea.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:1410.0601v1}, -author = {Lee, Hyun Su}, -doi = {10.1201/b17323-11}, -eprint = {arXiv:1410.0601v1}, -isbn = {}, -issn = {18248039}, -journal = {Proceedings of Science}, -keywords = {95.30.Cq,95.35.+d,98.62.Gq,SUSY,WIMPs,axions,cold dark matter,dark matter halo}, -month = {dec}, -number = {1}, -pages = {159--178}, -title = {{Direct detection of dark matter}}, -url = {http://www.annualreviews.org/doi/10.1146/annurev.nucl.54.070103.181244}, -volume = {340}, -year = {2019} -} -@article{Shi2017, -abstract = {We investigate the origin, the shape, the scatter, and the cosmic evolution in the observed relationship between specific angular momentum {\$}j{\_}\backslashstar{\$} and the stellar mass {\$}M{\_}\backslashstar{\$} in early-type (ETGs) and late-type galaxies (LTGs). Specifically, we exploit the observed star-formation efficiency and chemical abundance to infer the fraction {\$}f{\_}{\{}\backslashrm inf{\}}{\$} of baryons that infall toward the central regions of galaxies where star formation can occur. We find {\$}f{\_}{\{}\backslashrm inf{\}}\backslashapprox 1{\$} for LTGs and {\$}\backslashapprox 0.4{\$} for ETGs with an uncertainty of about {\$}0.25{\$} dex, consistent with a biased collapse. By comparing with the locally observed {\$}j{\_}\backslashstar{\$} vs. {\$}M{\_}\backslashstar{\$} relations for LTGs and ETGs we estimate the fraction {\$}f{\_}j{\$} of the initial specific angular momentum associated to the infalling gas that is retained in the stellar component: for LTGs we find {\$}f{\_}j\backslashapprox 1.11{\^{}}{\{}+0.75{\}}{\_}{\{}-0.44{\}}{\$}, in line with the classic disc formation picture; for ETGs we infer {\$}f{\_}j\backslashapprox 0.64{\^{}}{\{}+0.20{\}}{\_}{\{}-0.16{\}}{\$}, that can be traced back to a {\$}z{\textless}1{\$} evolution via dry mergers. We also show that the observed scatter in the {\$}j{\_}{\{}\backslashstar{\}}{\$} vs. {\$}M{\_}{\{}\backslashstar{\}}{\$} relation for both galaxy types is mainly contributed by the intrinsic dispersion in the spin parameters of the host dark matter halo. The biased collapse plus mergers scenario implies that the specific angular momentum in the stellar components of ETG progenitors at {\$}z\backslashsim 2{\$} is already close to the local values, in pleasing agreement with observations. All in all, we argue such a behavior to be imprinted by nature and not nurtured substantially by the environment.}, -archivePrefix = {arXiv}, -arxivId = {1706.02165}, -author = {Shi, J and Lapi, A and Mancuso, C and Wang, H and Danese, L}, -doi = {10.3847/1538-4357/aa7893}, -eprint = {1706.02165}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {elliptical - galaxies,evolution - galaxies,formation - galaxies,fundamental,galaxies}, -number = {2}, -pages = {105}, -title = {{Angular Momentum of Early- and Late-type Galaxies: Nature or Nurture?}}, -url = {http://arxiv.org/abs/1706.02165%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa7893}, -volume = {843}, -year = {2017} -} -@article{Yamamoto2019, -abstract = {Despite recent progress in diagnostic and multimodal treatment approaches, most cancer deaths are still caused by metastatic spread and the subsequent growth of tumor cells in sites distant from the primary organ. So far, few quantitative studies are available that allow for the estimation of metastatic parameters and the evaluation of alternative treatment strategies. Most computational studies have focused on situations in which the tumor cell population expands exponentially over time; however, tumors may eventually be subject to resource and space limitations so that their growth patterns deviate from exponential growth to adhere to density-dependent growth models. In this study, we developed a stochastic evolutionary model of cancer progression that considers alterations in metastasis-related genes and intercellular growth competition leading to density effects described by logistic growth. Using this stochastic model, we derived analytical approximations for the time between the initiation of tumorigenesis and diagnosis, the expected number of metastatic sites, the total number of metastatic cells, the size of the primary tumor, and survival. Furthermore, we investigated the effects of drug administration and surgical resection on these quantities and predicted outcomes for different treatment regimens. Parameter values used in the analysis were estimated from data obtained from a pancreatic cancer rapid autopsy program. Our theoretical approach allows for flexible modeling of metastatic progression dynamics.}, -author = {Yamamoto, Kimiyo N and Liu, Lin L and Nakamura, Akira and Haeno, Hiroshi and Michor, Franziska}, -doi = {10.1200/CCI.18.00079}, -issn = {2473-4276}, -journal = {JCO Clinical Cancer Informatics}, -month = {mar}, -number = {3}, -pages = {1--11}, -title = {{Stochastic Evolution of Pancreatic Cancer Metastases During Logistic Clonal Expansion}}, -url = {http://ascopubs.org/doi/10.1200/CCI.18.00079}, -year = {2019} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/9602085v1}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085v1}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {arXiv:astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{Regier2015, -abstract = {We present a new, fully generative model of optical telescope image sets, along with a variational procedure for inference. Each pixel intensity is treated as a Poisson random variable, with a rate parameter dependent on latent properties of stars and galaxies. Key latent properties are themselves random, with scientific prior distributions constructed from large ancillary data sets. We check our approach on synthetic images. We also run it on images from a major sky survey, where it exceeds the performance of the current state-of-the-art method for locating celestial bodies and measuring their colors.}, -archivePrefix = {arXiv}, -arxivId = {1506.01351}, -author = {Regier, Jeffrey and Miller, Andrew and McAuliffe, Jon and Adams, Ryan and Hoffman, Matt and Lang, Dustin and Schlegel, David and Prabhat}, -eprint = {1506.01351}, -isbn = {9781510810587}, -journal = {32nd International Conference on Machine Learning, ICML 2015}, -pages = {2095--2103}, -title = {{Celeste: Variational inference for a generative model of astronomical images}}, -volume = {3}, -year = {2015} -} -@article{2001ew, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Kung2017, -abstract = {We report modelling follow-up of recently discovered gravitational-lens candidates in the Canada France Hawaii Telescope Legacy Survey. Lens modelling was done by a small group of specially interested volunteers from the SpaceWarps citizen-science community who originally found the candidate lenses. Models are categorized according to seven diagnostics indicating (a) the image morphology and how clear or indistinct it is, (b) whether the mass map and synthetic lensed image appear to be plausible, and (c) how the lens-model mass compares with the stellar mass and the abundance-matched halo mass. The lensing masses range from {\$\sim${}}1011 to {\textgreater} 1013M⊙. Preliminary estimates of the stellar masses show a smaller spread in stellar mass (except for two lenses): a factor of a few below or above {\$\sim${}}1011M⊙. Therefore, we expect the stellar-to-total mass fraction to decline sharply as lensing mass increases. The most massive system with a convincing model is J1434+522 (SW 05). The two low-mass outliers are J0206-095 (SW 19) and J2217+015 (SW 42); if these two are indeed lenses, they probe an interesting regime of very low star formation efficiency. Some improvements to the modelling software (SpaghettiLens), and discussion of strategies regarding scaling to future surveys with more and frequent discoveries, are included.}, -archivePrefix = {arXiv}, -arxivId = {1711.07297}, -author = {K{\"{u}}ng, Rafael and Saha, Prasenjit and Ferreras, Ignacio and Baeten, Elisabeth and Coles, Jonathan and Cornen, Claude and Macmillan, Christine and Marshall, Phil and More, Anupreeta and Oswald, Lucy and Verma, Aprajita and Wilcox, Julianne K}, -doi = {10.1093/mnras/stx3012}, -eprint = {1711.07297}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: general,Galaxies: stellar content,Gravitational lensing: strong}, -number = {3}, -pages = {3700--3713}, -title = {{Models of gravitational lens candidates from SpaceWarps CFHTLS}}, -url = {http://arxiv.org/abs/1711.07297}, -volume = {474}, -year = {2018} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes posses a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a {\$}\backslashLambda{\$}CDM universe.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R and Eke, Vincent R and Frenk, Carlos S and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{Genel2017, -abstract = {We analyze scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, star-formation rate and redshift are reproduced, and a quantitative comparison of projected r-band sizes at 0{\$\sim${}}{\textless}z{\textless}{\$\sim${}}2 shows agreement to much better than 0.25dex. We follow populations of z=0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M{\_}{\{}*,z=0{\}}{\textgreater}{\$\sim${}}10{\^{}}{\{}9.5{\}}Msun, the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z=0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M{\_}{\{}*,z=0{\}}{\textgreater}{\$\sim${}}10{\^{}}{\{}9.5{\}}Msun experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies with M{\_}{\{}*,z=0{\}}{\textgreater}{\$\sim${}}10{\^{}}{\{}11{\}}Msun, the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main-sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z=0.}, -archivePrefix = {arXiv}, -arxivId = {1707.05327}, -author = {Genel, Shy and Nelson, Dylan and Pillepich, Annalisa and Springel, Volker and Pakmor, R{\"{u}}diger and Weinberger, Rainer and Hernquist, Lars and Naiman, Jill and Vogelsberger, Mark and Marinacci, Federico and Torrey, Paul}, -doi = {10.1093/mnras/stx3078}, -eprint = {1707.05327}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: evolution,Galaxies: formation,Galaxies: structure,Methods: numerical}, -number = {3}, -pages = {3976--3996}, -title = {{The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation}}, -url = {http://arxiv.org/abs/1707.05327}, -volume = {474}, -year = {2018} -} -@article{Buitrago2017a, -abstract = {Using the exquisite depth of the Hubble Ultra Deep Field (HUDF12 programme) dataset, we explore the ongoing assembly of the outermost regions of the most massive galaxies (M{\_}{\{}stellar{\}} {\textgreater}5x10{\^{}}{\{}10{\}} M{\_}{\{}Sun{\}}) at z {\textless}1. The outskirts of massive objects, particularly Early-Types Galaxies (ETGs), are expected to suffer a dramatic transformation across cosmic time due to continuous accretion of small galaxies. HUDF imaging allows us to study this process at intermediate redshifts in 6 massive galaxies, exploring the individual surface brightness profiles out to 25 effective radii. We find that 10-30{\%} of the total stellar mass for the galaxies in our sample is contained within 10 {\textless}R {\textless}50 kpc. These values are in close agreement with numerical simulations, and at least 2-3 times higher than those reported for late-type galaxies. The fraction of stellar mass stored in the outer envelopes/haloes of Massive Early-Type Galaxies increases with decreasing redshift, being 28.7{\%} at {\textless}z {\textgreater}= 0.1, 22.6{\%} at {\textless}z {\textgreater}= 0.65 and 3.5{\%} at {\textless}z {\textgreater}= 2. The fraction of mass in diffuse features linked with ongoing minor merger events is {\textgreater}1-3{\%}, very similar to predictions based on observed close pair counts. Therefore, our results suggest that the size and mass growth of the most massive galaxies have been solely driven by minor and major merging from z = 1 to today.}, -archivePrefix = {arXiv}, -arxivId = {1602.01846}, -author = {Buitrago, Fernando and Trujillo, Ignacio and Curtis-Lake, Emma and Montes, Mireia and Cooper, Andrew P and Bruce, Victoria A and P{\'{e}}rez-Gonz{\'{a}}lez, Pablo G and Cirasuolo, Michele}, -doi = {10.1093/mnras/stw3382}, -eprint = {1602.01846}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cd,elliptical and lenticular,evolution,galaxies,haloes,high-redshift,morphology,structure}, -number = {January}, -pages = {stw3382}, -title = {{The cosmic assembly of stellar haloes in massive Early-Type Galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw3382}, -volume = {000}, -year = {2017} -} -@article{corner2016, -author = {Foreman-Mackey, Daniel}, -doi = {10.21105/joss.00024}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Foreman-Mackey - 2016 - corner.py Scatterplot matrices in Python(2).pdf:pdf}, -journal = {J. Open Source Softw}, -month = {jun}, -number = {2}, -pages = {24}, -publisher = {The Open Journal}, -title = {{corner.py: Scatterplot matrices in Python}}, -url = {https://doi.org/10.21105/joss.00024}, -volume = {1}, -year = {2016} -} -@article{Dekel2009b, -abstract = {Massive galaxies in the young Universe, ten billion years ago, formed stars at surprising intensities. Although this is commonly attributed to violent mergers, the properties of many of these galaxies are incompatible with such events, showing gas-rich, clumpy, extended rotating disks not dominated by spheroids. Cosmological simulations and clustering theory are used to explore how these galaxies acquired their gas. Here we report that they are 'stream-fed galaxies', formed from steady, narrow, cold gas streams that penetrate the shock-heated media of massive dark matter haloes. A comparison with the observed abundance of star-forming galaxies implies that most of the input gas must rapidly convert to stars. One-third of the stream mass is in gas clumps leading to mergers of mass ratio greater than 1:10, and the rest is in smoother flows. With a merger duty cycle of 0.1, three-quarters of the galaxies forming stars at a given rate are fed by smooth streams. The rarer, submillimetre galaxies that form stars even more intensely are largely merger-induced starbursts. Unlike destructive mergers, the streams are likely to keep the rotating disk configuration intact, although turbulent and broken into giant star-forming clumps that merge into a central spheroid. This stream-driven scenario for the formation of discs and spheroids is an alternative to the merger picture. {\textcopyright}2009 Macmillan Publishers Limited. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0808.0553}, -author = {Dekel, A. and Birnboim, Y. and Engel, G. and Freundlich, J. and Goerdt, T. and Mumcuoglu, M. and Neistein, E. and Pichon, C. and Teyssier, R. and Zinger, E.}, -doi = {10.1038/nature07648}, -eprint = {0808.0553}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dekel et al. - 2009 - Cold streams in early massive hot haloes as the main mode of galaxy formation.pdf:pdf}, -issn = {00280836}, -journal = {Nature}, -month = {jan}, -number = {7228}, -pages = {451--454}, -pmid = {19158792}, -title = {{Cold streams in early massive hot haloes as the main mode of galaxy formation}}, -url = {https://ui.adsabs.harvard.edu/#abs/2009Natur.457..451D/abstract}, -volume = {457}, -year = {2009} -} -@article{Harvey2015, -abstract = {Collisions between galaxy clusters provide a test of the nongravitational forces acting on dark matter. Dark matter's lack of deceleration in the "bullet cluster" collision constrained its self-interaction cross section $\sigma$DM/m < 1.25 square centimeters per gram (cm2/g) [68% confidence limit (CL)] ($\sigma$DM, self-interaction cross section; m, unit mass of dark matter) for long-ranged forces. Using the Chandra and Hubble Space Telescopes, we have now observed 72 collisions, including both major and minor mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6s significance. The position of the dark mass has remained closely aligned within 5.8 T 8.2 kiloparsecs of associated stars, implying a self-interaction cross section $\sigma$DM/m < 0.47 cm2/g (95% CL) and disfavoring some proposed extensions to the standard model.}, -archivePrefix = {arXiv}, -arxivId = {1503.07675}, -author = {Harvey, David and Massey, Richard and Kitching, Thomas and Taylor, Andy and Tittley, Eric}, -doi = {10.1126/science.1261381}, -eprint = {1503.07675}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Harvey et al. - 2015 - The nongravitational interactions of dark matter in colliding galaxy clusters.pdf:pdf}, -issn = {10959203}, -journal = {Science}, -number = {6229}, -pages = {1462--1465}, -pmid = {25814581}, -title = {{The nongravitational interactions of dark matter in colliding galaxy clusters}}, -volume = {347}, -year = {2015} -} -@article{Greene2015a, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 < $\sigma$∗ < 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E. and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J. and Blakeslee, John P. and Thomas, Jens and Murphy, Jeremy D.}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Greene et al. - 2015 - the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies(3).pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: elliptical and lenticular, cD,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Hewitt1988, -abstract = {We report the discovery of extremely unusual structure in the radio source MG1131 + 0456. In a radio map with sub∼arc$econd resolution the object appears as an elliptical ring of emission accompanied by a pair of more compact sources, nearly diametrically opposed and offset ∼0.3 arc s to the south-west of the ring. There is a faint, slightly extended, optical counterpart. In its spectrum we detect a continuum but no emission lines; therefore the redshift of the counterpart is unknown. The radio morphology suggests that this source may be an example of an 'Einstein ring'1, a highly symmetric case of grayitational lensing in which the source is imaged into a ring. Other explanations that we consider are excluded by the data. Another possibility is that MG1131 +0456 represents a new type of (unlensed) astronomical object. {\textcopyright} 1988 Nature Publishing Group.}, -author = {Hewitt, J. N. and Turner, E. L. and Schneider, D. P. and Burke, B. F. and Langston, G. I. and Lawrence, C. R.}, -doi = {10.1038/333537a0}, -issn = {00280836}, -journal = {Nature}, -keywords = {Extragalactic Radio Sources,Gravitational Fields,Gravitational Lenses,Infrared Sources (Astronomy),Radio Galaxies,Very Large Array (Vla)}, -month = {jun}, -number = {6173}, -pages = {537--540}, -title = {{Unusual radio source MG1131+0456: A possible Einstein ring}}, -url = {http://www.nature.com/doifinder/10.1038/333537a0}, -volume = {333}, -year = {1988} -} -@article{Agustsson2006a, -abstract = {We compute the locations of satellite galaxies with respect to their hosts using the Lambda-CDM GIF simulation. If the major axes of the hosts' images are perfectly aligned with the major axes of their projected mass, the satellites are located preferentially close to the hosts' major axes. In this case, the degree of anisotropy in the satellite locations is a good tracer of the flattening of the hosts' halos. If all hosts have luminous circular disks, the symmetry axes of the projected mass and light are not perfectly aligned, and the locations of the satellites depend upon how the hosts' disks are placed within their halos. If the disk angular momentum vectors are aligned with the major axes of the halos, the satellites show a pronounced "Holmberg effect". If the disk angular momentum vectors are aligned with the intermediate axes of the local large scale structure, the distribution of satellite locations is essentially isotropic. If the disk angular momentum vectors are aligned with either the minor axes or with the net angular momentum vectors of the halos, the satellites are distributed anisotropically about their hosts, with a preference for being found nearby the hosts' major axes. This agrees well with the observation that satellite galaxies in the Sloan Digital Sky Survey tend to be found nearby the major axes of their hosts, and suggests that the mass and light of SDSS host galaxies must be fairly well aligned in projection on the sky.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0505272}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G.}, -doi = {10.1086/507084}, -eprint = {0505272}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Agustsson, Brainerd - 2006 - The Locations of Satellite Galaxies in a $\Lambda$CDM Universe(2).pdf:pdf}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Dwarf,Galaxies: Fundamental Parameters,Galaxies: Halos,Galaxies: Structure}, -number = {2}, -pages = {550--559}, -primaryClass = {astro-ph}, -title = {{The Locations of Satellite Galaxies in a $\Lambda$CDM Universe}}, -url = {http://arxiv.org/abs/astro-ph/0505272%0Ahttp://dx.doi.org/10.1086/507084}, -volume = {650}, -year = {2006} -} -@article{Anderson2014, -abstract = {We present a one per cent measurement of the cosmic distance scale from the detections of the baryon acoustic oscillations (BAO) in the clustering of galaxies from the Baryon Oscillation Spectroscopic Survey, which is part of the Sloan Digital Sky Survey III. Our results come from the Data Release 11 (DR11) sample, containing nearly one million galaxies and covering approximately 8500 square degrees and the redshift range 0.2 < z < 0.7. We also compare these results with those from the publicly released DR9 and DR10 samples. Assuming a concordance $\Lambda$ cold dark matter ($\Lambda$CDM) cosmological model, the DR11 sample covers a volume of 13 Gpc3 and is the largest region of the Universe ever surveyed at this density. We measure the correlation function and power spectrum, including density-field reconstruction of the BAO feature. The acoustic features are detected at a significance of over 7$\sigma$ in both the correlation function and power spectrum. Fitting for the position of the acoustic features measures the distance relative to the sound horizon at the drag epoch, rd, which has a value of rd,fid = 149.28 Mpc in our fiducial cosmology. We find DV = (1264 ± 25 Mpc)(rd/rd,fid) at z = 0.32 and DV = (2056 ± 20 Mpc)(rd/rd,fid) at z = 0.57. At 1.0 per cent, this latter measure is the most precise distance constraint ever obtained from a galaxy survey. Separating the clustering along and transverse to the line of sight yields measurements at z = 0.57 of DA = (1421 ± 20 Mpc)(rd/rd,fid) and H = (96.8 ± 3.4 kms-1 Mpc-1)(rd,fid/rd). Our measurements of the distance scale are in good agreement with previous BAO measurements and with the predictions from cosmic microwave background data for a spatially flat CDM model with a cosmological constant. {\textcopyright} 2014 The Author Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1312.4877}, -author = {Anderson, Lauren and Aubourg, {\'{E}}lric and Bailey, Stephen and Beutler, Florian and Bhardwaj, Vaishali and Blanton, Michael and Bolton, Adam S. and Brinkmann, J. and Brownstein, Joel R. and Burden, Angela and Chuang, Chia Hsun and Cuesta, Antonio J. and Dawson, Kyle S. and Eisenstein, Daniel J. and Escoffier, Stephanie and Gunn, James E. and Guo, Hong and Ho, Shirley and Honscheid, Klaus and Howlett, Cullan and Kirkby, David and Lupton, Robert H. and Manera, Marc and Maraston, Claudia and McBride, Cameron K. and Mena, Olga and Montesano, Francesco and Nichol, Robert C. and Nuza, Sebasti{\'{a}}n E. and Olmstead, Matthew D. and Padmanabhan, Nikhil and Palanque-Delabrouille, Nathalie and Parejko, John and Percival, Will J. and Petitjean, Patrick and Prada, Francisco and Price-Whelan, Adrian M. and Reid, Beth and Roe, Natalie A. and Ross, Ashley J. and Ross, Nicholas P. and Sabiu, Cristiano G. and Saito, Shun and Samushia, Lado and S{\'{a}}nchez, Ariel G. and Schlegel, David J. and Schneider, Donald P. and Scoccola, Claudia G. and Seo, Hee Jong and Skibba, Ramin A. and Strauss, Michael A. and Molly, Molly E. and Thomas, Daniel and Tinker, Jeremy L. and Tojeiro, Rita and Maga{\~{n}}a, Mariana Vargas and Verde, Licia and Wake, David A. and Weaver, Benjamin A. and Weinberg, David H. and White, Martin and Xu, Xiaoying and Y{\`{e}}che, Christophe and Zehavi, Idit and Zhao, Gong Bo}, -doi = {10.1093/mnras/stu523}, -eprint = {1312.4877}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Anderson et al. - 2014 - The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey Baryon acoustic oscillations.pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Anderson et al. - 2014 - The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey Baryon acoustic oscillati(2).pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Cosmology: observations,Dark energy,Distance scale,Large-scale structure of Universe}, -number = {1}, -pages = {24--62}, -title = {{The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey: Baryon acoustic oscillations in the data releases 10 and 11 galaxy samples}}, -volume = {441}, -year = {2014} -} -@article{Gow2016, -abstract = {{\textcopyright} 2016 SPIE. A major concern when using Charge-Coupled Devices in hostile radiation environments is radiation induced Charge Transfer Inefficiency. The displacement damage from non-ionising radiation incident on the detector creates defects within the silicon lattice, these defects can capture and hold charge for a period of time dependent on the operating temperature and the type of defect, or "trap species". The location and type of defect can be determined to a high degree of precision using the trap-pumping technique, whereby background charges are input and then shuffled forwards and backwards between pixels many times and repeated using different transfer timings to promote resonant charge-pumping at particular defect sites. Where the charge transfer timings used in the trap-pumping process are equivalent to the nominal CCD readout modes, a simple "trap-map" of the defects that will most likely contribute to charge transfer inefficiency in the CCD array can be quickly generated. This paper describes a concept for how such a "trap-map" can be used to correct images subject to non-ionising radiation damage and provides initial results from an analytical algorithm and our recommendations for future developments.}, -author = {Gow, Jason P. D. and Murray, Neil J.}, -doi = {10.1117/12.2232706}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Gow, Murray - 2016 - Simplified charge transfer inefficiency correction in CCDs by trap-pumping(2).pdf:pdf}, -isbn = {9781510602090}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VII}, -keywords = {ccd,charge recovery,charge transfer efficiency,proton radiation damage,trap-pumping}, -number = {0}, -pages = {99152A}, -title = {{Simplified charge transfer inefficiency correction in CCDs by trap-pumping}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2232706}, -volume = {9915}, -year = {2016} -} -@article{Ding2016, -abstract = {The empirical correlation between the mass of a super-massive black hole (MBH) and its host galaxy properties is widely considered to be evidence of their co-evolution. A powerful way to test the co-evolution scenario and learn about the feedback processes linking galaxies and nuclear activity is to measure these correlations as a function of redshift. Unfortunately, currently MBH can only be estimated in active galaxies at cosmological distances. At these distances, bright active galactic nuclei (AGN) can outshine the host galaxy, making it extremely difficult to measure the host's luminosity. Strongly lensed AGNs provide in principle a great opportunity to improve the sensitivity and accuracy of the host galaxy luminosity measurements as the host galaxy is magnified and more easily separated from the point source, provided the lens model is sufficiently accurate. In order to measure the MBH-L correlation with strong lensing, it is necessary to ensure that the lens modelling is accurate, and that the host galaxy luminosity can be recovered to at least a precision and accuracy better than that of the typical MBH measurement. We carry out extensive and realistic simulations of deep Hubble Space Telescope observations of lensed AGNs obtained by our collaboration. We show that the host galaxy luminosity can be recovered with better accuracy and precision than the typical uncertainty on MBH({\$\sim${}} 0.5 dex) for hosts as faint as 2-4 magnitudes dimmer than the AGN itself. Our simulations will be used to estimate bias and uncertainties on the actual measurements to be presented in a future paper.}, -archivePrefix = {arXiv}, -arxivId = {1610.08504}, -author = {Ding, Xuheng and Liao, Kai and Treu, Tommaso and Suyu, Sherry H and Chen, Geoff C F and Auger, Matthew W and Marshall, Philip J and Agnello, Adriano and Courbin, Frederic and Nierenberg, Anna M and Rusu, Cristian E and Sluse, Dominique and Sonnenfeld, Alessandro and Wong, Kenneth C}, -doi = {10.1093/mnras/stw3078}, -eprint = {1610.08504}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: evolution}, -number = {4}, -pages = {4634--4649}, -title = {{H0LiCOW. VI. Testing the fidelity of lensed quasar host galaxy reconstruction}}, -url = {http://arxiv.org/abs/1610.08504}, -volume = {465}, -year = {2017} -} -@article{Schaller2015b, -abstract = {We use the 'Evolution and Assembly of GaLaxies and their Environments' (eagle) suite of hydrodynamical cosmological simulations to measure offsets between the centres of stellar and dark matter components of galaxies. We find that the vast majority (>95 per cent) of the simulated galaxies display an offset smaller than the gravitational softening length of the simulations (Plummer-equivalent $\epsilon$= 700 pc), both for field galaxies and satellites in clusters and groups. We also find no systematic trailing or leading of the dark matter along a galaxy's direction of motion. The offsets are consistent with being randomly drawn from a Maxwellian distribution with $\sigma$≤ 196pc. Since astrophysical effects produce no feasible analogues for the 1.62+0.47-0.49kpc offset recently observed in Abell 3827, the observational result is in tension with the collisionless cold dark matter model assumed in our simulations.}, -archivePrefix = {arXiv}, -arxivId = {1505.05470}, -author = {Schaller, Matthieu and Robertson, Andrew and Massey, Richard and Bower, Richard G. and Eke, Vincent R.}, -doi = {10.1093/mnrasl/slv104}, -eprint = {1505.05470}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Astroparticle physics,Cosmology: theory,Dark matter}, -month = {oct}, -number = {1}, -pages = {L58--L62}, -title = {{The offsets between galaxies and their dark matter in $\Lambda$ cold dark matter}}, -url = {http://arxiv.org/abs/1505.05470}, -volume = {453}, -year = {2015} -} -@article{Rasmussen2016, -author = {Rasmussen, Carl Edward}, -pages = {1--13}, -title = {{Factor Graphs and message passing Key concepts}}, -year = {2016} -} -@article{Goobar2016, -abstract = {We report the discovery of a multiply-imaged gravitationally lensed Type Ia supernova, iPTF16geu (SN 2016geu), at redshift {\$}z=0.409{\$}. This phenomenon could be identified because the light from the stellar explosion was magnified more than fifty times by the curvature of space around matter in an intervening galaxy. We used high spatial resolution observations to resolve four images of the lensed supernova, approximately 0.3" from the center of the foreground galaxy. The observations probe a physical scale of {\$}\backslashsim{\$}1 kiloparsec, smaller than what is typical in other studies of extragalactic gravitational lensing. The large magnification and symmetric image configuration implies close alignment between the line-of-sight to the supernova and the lens. The relative magnifications of the four images provide evidence for sub-structures in the lensing galaxy.}, -archivePrefix = {arXiv}, -arxivId = {1611.00014}, -author = {Goobar, A and Amanullah, R and Kulkarni, S R and Nugent, P E and Johansson, J and Steidel, C and Law, D and M{\"{o}}rtsell, E and Quimby, R and Blagorodnova, N and Brandeker, A and Cao, Y and Cooray, A and Ferretti, R and Fremling, C and Hangard, L and Kasliwal, M and Kupfer, T and Lunnan, R and Masci, F and Miller, A A and Nayyeri, H and Neill, J D and Ofek, E O and Papadogiannakis, S and Petrushevska, T and Ravi, V and Sollerman, J and Sullivan, M and Taddia, F and Walters, R and Wilson, D and Yan, L and Yaron, O}, -doi = {10.1126/science.aal2729}, -eprint = {1611.00014}, -isbn = {1095-9203 (Electronic) 0036-8075 (Linking)}, -issn = {10959203}, -journal = {Science}, -number = {6335}, -pages = {291--295}, -pmid = {28428419}, -title = {{IPTF16geu: A multiply imaged, gravitationally lensed type ia supernova}}, -url = {http://arxiv.org/abs/1611.00014}, -volume = {356}, -year = {2017} -} -@article{Lovell2018a, -abstract = {We use the IllustrisTNG (TNG) cosmological simulations to provide theoretical expectations for the dark matter mass fractions (DMFs) and circular velocity profiles of galaxies. TNG predicts flat circular velocity curves for z = 0 Milky Way (MW)-like galaxies beyond a few kpc from the galaxy centre, in better agreement with observational constraints than its predecessor, Illustris. TNG also predicts an enhancement of the dark matter mass within the 3D stellar half-mass radius (rhalf; M200c = 1010-1013M⊙, z ≤ 2) compared to its dark matter only and Illustris counterparts. This enhancement leads TNG present-day galaxies to be dominated by dark matter within their inner regions, with fDM({\textless} rhalf) ≳ 0.5 at all masses and with a minimum for MW-mass galaxies. The 1$\sigma$ scatter is ≲10 per cent at all apertures, which is smaller than that inferred by some observational data sets, e.g. 40 per cent from the SLUGGS survey. TNG agrees with the majority of the observationally inferred values for elliptical galaxies once a consistent initial mass function is adopted (Chabrier) and the DMFs are measured within the same apertures. The DMFs measured within rhalf increase towards lower redshifts: this evolution is dominated by the increase in galaxy size with time. At z {\$\sim${}} 2, the DMF in disc-like TNG galaxies decreases with increasing galaxy mass, with fDM({\textless} rhalf) {\$\sim${}} 0.10-0.65 for 1010 ≲ Mstars/M⊙ ≲ 1012, and are two times higher than if TNG galaxies resided in Navarro-Frenk-White dark matter haloes unaffected by baryonic physics. It remains to be properly assessed whether recent observational estimates of the DMFs at z {\$\sim${}}2 rule out the contraction of the dark matter haloes predicted by the TNG model.}, -archivePrefix = {arXiv}, -arxivId = {1801.10170}, -author = {Lovell, Mark R and Pillepich, Annalisa and Genel, Shy and Nelson, Dylan and Springel, Volker and Pakmor, R{\"{u}}diger and Marinacci, Federico and Weinberger, Rainer and Torrey, Paul and Vogelsberger, Mark and Alabi, Adebusola and Hernquist, Lars}, -doi = {10.1093/MNRAS/STY2339}, -eprint = {1801.10170}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {(cosmology:) dark matter,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1950--1975}, -title = {{The fraction of dark matter within galaxies from the IllustrisTNG simulations}}, -volume = {481}, -year = {2018} -} -@article{Foreman-Mackey2013, -abstract = {We introduce a stable, well tested Python implementation of the affine-invariant ensemble sampler for Markov chain Monte Carlo (MCMC) proposed by Goodman & Weare (2010). The code is open source and has already been used in several published projects in the astrophysics literature. The algorithm behind emcee has several advantages over traditional MCMC sampling methods and it has excellent performance as measured by the autocorrelation time (or function calls per independent sample). One major advantage of the algorithm is that it requires hand-tuning of only 1 or 2 parameters compared to $\sim N^2$ for a traditional algorithm in an N-dimensional parameter space. In this document, we describe the algorithm and the details of our implementation and API. Exploiting the parallelism of the ensemble method, emcee permits any user to take advantage of multiple CPU cores without extra effort. The code is available online at http://dan.iel.fm/emcee under the MIT License.}, -archivePrefix = {arXiv}, -arxivId = {1202.3665}, -author = {Foreman-Mackey, Daniel and Hogg, David W. and Lang, Dustin and Goodman, Jonathan}, -doi = {10.1086/670067}, -eprint = {1202.3665}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Foreman-Mackey et al. - 2013 - emcee The MCMC Hammer.pdf:pdf}, -issn = {00046280}, -journal = {Publ. Astron. Soc. Pac.}, -number = {925}, -pages = {306--312}, -title = {{emcee : The MCMC Hammer}}, -volume = {125}, -year = {2013} -} -@article{Regier2015, -abstract = {We present a new, fully generative model of optical telescope image sets, along with a variational procedure for inference. Each pixel intensity is treated as a Poisson random variable, with a rate parameter dependent on latent properties of stars and galaxies. Key latent properties are themselves random, with scientific prior distributions constructed from large ancillary data sets. We check our approach on synthetic images. We also run it on images from a major sky survey, where it exceeds the performance of the current state-of-the-art method for locating celestial bodies and measuring their colors.}, -archivePrefix = {arXiv}, -arxivId = {1506.01351}, -author = {Regier, Jeffrey and Miller, Andrew and McAuliffe, Jon and Adams, Ryan and Hoffman, Matt and Lang, Dustin and Schlegel, David and Prabhat}, -eprint = {1506.01351}, -isbn = {9781510810587}, -journal = {32nd International Conference on Machine Learning, ICML 2015}, -pages = {2095--2103}, -title = {{Celeste: Variational inference for a generative model of astronomical images}}, -volume = {3}, -year = {2015} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashbackslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless}10{\^{}}7{\\sim{}}M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashbackslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashbackslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashbackslashepsilon = 0.43 \backslashbackslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashbackslashpm 0.04\backslashbackslash{\{}\backslash{\%}{\}}{\$}, i.e.{\$\sim${}}a {\$}\backslashbackslashpm 2\backslashbackslashsigma{\{}\backslash{\$}{\}} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashbackslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637X/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -title = {{Supermassive black holes and their host spheroids II. The red and blue sequence in the {\$}M{\_}{\{}\backslashbackslashrm BH{\}} - M{\_}{\{}\backslashbackslashrm *,sph{\}}{\$} diagram}}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -year = {2015} -} -@article{Lee2016, -abstract = {We study how properties of discrete dark matter halos depend on halo environment, characterized by the mass density around the halos on scales from 0.5 to 16 {\$}h{\^{}}{\{}-1{\}}{\{}\backslashbackslashrm Mpc{\}}{\$}. We find that low mass halos (those less massive than the characteristic mass {\$}M{\_}{\{}\backslashbackslashrm C{\}}{\$} of halos collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations, and rounder shapes than halos in median density environments. Halos in median and low-density environments have similar accretion rates and concentrations, but halos in low density environments have lower spins and are more elongated. Halos of a given mass in high-density regions accrete material earlier than halos of the same mass in lower-density regions. All but the most massive halos in high-density regions are losing mass (i.e., being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low mass halos in high density regions at low redshifts {\$}z {\textless}1{\$}, by preferentially removing higher angular momentum material from halos. Halos in low-density regions have lower than average spins because they lack nearby halos whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an Extreme Value Distribution, and that the density distribution becomes broader with cosmic time.}, -archivePrefix = {arXiv}, -arxivId = {1610.02108}, -author = {Lee, Christoph T and Primack, Joel R and Behroozi, Peter and Rodriguez-Puebla, Aldo and Hellinger, Doug and Dekel, Avishai}, -doi = {10.1093/mnras/stw3348}, -eprint = {1610.02108}, -issn = {0035-8711}, -journal = {Mon. Not. R. Astron. Soc}, -keywords = {Cosmology,Halos -Methods,Large Scale Structure -Dark Matter -Galaxies,Numerical}, -number = {October}, -pages = {1--20}, -title = {{Properties of Dark Matter Halos as a Function of Local Environment Density}}, -url = {http://arxiv.org/abs/1610.02108%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3348}, -volume = {000}, -year = {2016} -} -@article{Houghton2006, -abstract = {ABSTRACT We present near-infrared (NIR) adaptive optics-assisted spectroscopic observations of the CO ($\Delta$$\mu$= 2) absorption bands towards the centre of the giant elliptical galaxy NGC 1399. The observations were made with NAOS-CONICA (on the European Southern Observatory's Very Large Telescope) and have a full width at half-maximum resolution of 0.15 arcsec (14 pc). Kinematic analysis of the observations reveals a decoupled core and strongly non-Gaussian line-of-sight velocity profiles in the central 0.2 arcsec (19 pc). NIR imaging also indicates an asymmetric elongation of the central isophotes in the same region. We use spherical orbit-superposition models to interpret the kinematics, using a set of orthogonal 'eigen-velocity profiles' that allow us to fit models directly to spectra. The models require a central black hole of mass 1.2 +0.5-0.6× 10 9 M ⊙, with a strongly tangentially biased orbit distribution in the inner 40 pc. {\textcopyright} 2006 RAS.}, -author = {Houghton, R. C.W. and Magorrian, J. and Sarzi, M. and Thatte, N. and Davies, R. L. and Krajnovi{\'{c}}, D.}, -doi = {10.1111/j.1365-2966.2005.09713.x}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: individual: NGC 1399,Galaxies: kinematics and dynamics,Instrumentation: adaptive optics}, -month = {mar}, -number = {1}, -pages = {2--18}, -title = {{The central kinematics of NGC 1399 measured with 14 pc resolution}}, -volume = {367}, -year = {2006} -} -@article{Goulding2016a, -abstract = {Studies of the physical properties of local elliptical galaxies (e.g., gas temperatures, halo masses, stellar kinematics) are shedding new light on galaxy formation. Here we present the hot X-ray gas properties of 33 early-type systems within the MASSIVE galaxy survey sample that have archival Chandra X-ray observations. Through careful X-ray spectral modeling, we derive X-ray luminosities (L{\_}X) and plasma temperatures (T{\_}gas) for the diffuse gas components in these galaxies. We combine the MASSIVE sample with 41 galaxies from the ATLAS{\^{}}3D survey to investigate the X-ray and optical properties of a statistically significant sample of nearby early-type galaxies across a wide-range of environments. We deduce that all early-type galaxies (independent of galaxy mass and rotational support) follow a universal scaling law such that L{\_}X{\$\sim${}}T{\_}gas{\^{}}4.5. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, the wide-scale environment does not contribute to the intrinsic scatter ({\$\sim${}}0.5dex) within the scaling relation. We further demonstrate that the scatter in L{\_}X around both K-band luminosity (L{\_}K) and the galaxy stellar velocity dispersion is primarily driven by T{\_}gas, with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the origin of the gas directly to either the stellar mass or the galaxy potential. Indeed, our data require a steeper relation between L{\_}X, L{\_}K, and sigma{\_}e than predicted by standard mass-loss models. Finally, we find a statistically significant correlation between sigma{\_}e and T{\_}gas, suggesting that T{\_}gas is set by the galaxy potential inside the optical effective radius. We conclude that within the inner-most 10-30kpc region, early-types maintain pressure-supported hot gas, with a minimum T{\_}gas set by the virial temperature, but the majority show evidence for some additional heating.}, -archivePrefix = {arXiv}, -arxivId = {1604.01764}, -author = {Goulding, Andy D and Greene, Jenny E and Ma, Chung-Pei and Veale, Melanie and Bogdan, Akos and Nyland, Kristina and Blakeslee, John P and McConnell, Nicholas J and Thomas, Jens}, -doi = {10.3847/0004-637x/826/2/167}, -eprint = {1604.01764}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {167}, -title = {{the Massive Survey. Iv. the X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe}}, -url = {http://arxiv.org/abs/1604.01764%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/826/2/167}, -volume = {826}, -year = {2016} -} -@article{Hopkins2012, -abstract = {Feedback from massive stars is believed to play a critical role in driving galactic super-winds that enrich the intergalactic medium and shape the galaxy mass function, mass-metallicity relation and other global galaxy properties. In previous papers, we have introduced new numerical methods for implementing stellar feedback on sub-giant molecular cloud (sub-GMC) through galactic scales in numerical simulations of galaxies; the key physical processes include radiation pressure in the ultraviolet through infrared, supernovae (Type I and Type II), stellar winds ('fast' O star through 'slow' asymptotic giant branch winds), and Hii photoionization. Here, we show that these feedback mechanisms drive galactic winds with outflow rates as high as ∼10-20 times the galaxy star formation rate. The mass-loading efficiency (wind mass-loss rate divided by the star formation rate) scales roughly as M wind/M* ∞ V c-1 (where V c is the galaxy circular velocity), consistent with simple momentum-conservation expectations. We use our suite of simulations to study the relative contribution of each feedback mechanism to the generation of galactic winds in a range of galaxy models, from Small Magellanic Cloud like dwarfs and Milky Way (MW) analogues to z∼ 2 clumpy discs. In massive, gas-rich systems (local starbursts and high-z galaxies), radiation pressure dominates the wind generation. By contrast, for MW-like spirals and dwarf galaxies the gas densities are much lower and sources of shock-heated gas such as supernovae and stellar winds dominate the production of large-scale outflows. In all of our models, however, the winds have a complex multiphase structure that depends on the interaction between multiple feedback mechanisms operating on different spatial scales and time-scales: any single feedback mechanism fails to reproduce the winds observed. We use our simulations to provide fitting functions to the wind mass loading and velocities as a function of galaxy properties, for use in cosmological simulations and semi-analytic models. These differ from typically adopted formulae with an explicit dependence on the gas surface density that can be very important in both low-density dwarf galaxies and high-density gas-rich galaxies. {\textcopyright}2012 The Author Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.4638}, -author = {Hopkins, Philip F and Quataert, Eliot and Murray, Norman}, -doi = {10.1111/j.1365-2966.2012.20593.x}, -eprint = {1110.4638}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Stars: formation}, -number = {4}, -pages = {3522--3537}, -title = {{Stellar feedback in galaxies and the origin of galaxy-scale winds}}, -volume = {421}, -year = {2012} -} -@article{Enia2018, -abstract = {We perform lens modelling and source reconstruction of Sub-millimetre Array (SMA) data for a sample of 12 strongly lensed galaxies selected at 500$\mu$m in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). A previous analysis of the same data set used a single S{\'{e}}rsic profile to model the light distribution of each background galaxy. Here we model the source brightness distribution with an adaptive pixel scale scheme, extended to work in the Fourier visibility space of interferometry. We also present new SMA observations for seven other candidate lensed galaxies from theH-ATLAS sample. Our derived lens model parameters are in general consistent with previous findings. However, our estimated magnification factors, ranging from 3 to 10, are lower. The discrepancies are observed in particular where the reconstructed source hints at the presence of multiple knots of emission.We define an effective radius of the reconstructed sources based on the area in the source plane where emission is detected above 5s. We also fit the reconstructed source surface brightness with an elliptical Gaussian model. We derive a median value reff {\$\sim${}} 1.77 kpc and a median Gaussian full width at half-maximum {\$\sim${}}1.47 kpc. After correction for magnification, our sources have intrinsic star formation rates (SFR) {\$\sim${}} 900-3500M⊙ yr-1, resulting in a median SFR surface density $\Sigma$SFR {\$\sim${}} 132M⊙ yr-1 kpc-2 (or {\$\sim${}}218M⊙ yr-1 kpc-2 for the Gaussian fit). This is consistent with that observed for other star-forming galaxies at similar redshifts, and is significantly below the Eddington limit for a radiation pressure regulated starburst.}, -archivePrefix = {arXiv}, -arxivId = {1801.01831}, -author = {Enia, A and Negrello, M and Gurwell, M and Dye, S and Rodighiero, G and Massardi, M and {De Zotti}, G and Franceschini, A and Cooray, A and van der Werf, P and Birkinshaw, M and Michalowski, M J and Oteo, I}, -doi = {10.1093/mnras/sty021}, -eprint = {1801.01831}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: structure,Gravitational lensing: strong,Instrumentation: interferometers}, -number = {3}, -pages = {3467--3484}, -title = {{The Herschel-ATLAS: Magnifications and physical sizes of 500-$\mu$m-selected strongly lensed galaxies}}, -url = {http://arxiv.org/abs/1801.01831}, -volume = {475}, -year = {2018} -} -@article{Lee2016, -abstract = {We study how properties of discrete dark matter haloes depend on halo environment, characterized by the mass density around the haloes on scales from 0.5 to 16 h−1 Mpc. We find that low-mass haloes (those less massive than the characteristic mass MC of haloes collapsing at a given epoch) in high-density environments have lower accretion rates, lower spins, higher concentrations and rounder shapes than haloes in median density environments. Haloes in median- and low-density environments have similar accretion rates and concentrations, but haloes in low-density environments have lower spins and are more elongated. Haloes of a given mass in high-density regions accrete material earlier than haloes of the same mass in lower density regions. All but the most massive haloes in high-density regions are losing mass (i.e. being stripped) at low redshifts, which causes artificially lowered NFW scale radii and increased concentrations. Tidal effects are also responsible for the decreasing spins of low-mass haloes in high-density regions at low redshifts z {\textless} 1, by preferentially removing higher angular momentum material from haloes. Haloes in low-density regions have lower than average spins because they lack nearby haloes whose tidal fields can spin them up. We also show that the simulation density distribution is well fit by an extreme value distribution, and that the density distribution becomes broader with cosmic time.}, -archivePrefix = {arXiv}, -arxivId = {1610.02108}, -author = {Lee, Christoph T and Primack, Joel R and Behroozi, Peter and Rodr{\'{i}}guez-Puebla, Aldo and Hellinger, Doug and Dekel, Avishai}, -doi = {10.1093/mnras/stw3348}, -eprint = {1610.02108}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: haloes,Large-scale structure of Universe,Methods: numerical}, -number = {4}, -pages = {3834--3858}, -title = {{Properties of dark matter haloes as a function of local environment density}}, -url = {http://arxiv.org/abs/1610.02108%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3348}, -volume = {466}, -year = {2017} -} -@article{Kocevski2017, -abstract = {We examine the fraction of massive ({\$}M{\_}{\{}*{\}}{\textgreater}10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}), compact star-forming galaxies (cSFGs) that host an active galactic nucleus (AGN) at {\$}z\backslashsim2{\$}. These cSFGs are likely the direct progenitors of the compact quiescent galaxies observed at this epoch, which are the first population of passive galaxies to appear in large numbers in the early Universe. We identify cSFGs that host an AGN using a combination of Hubble WFC3 imaging and Chandra X-ray observations in four fields: the Chandra Deep Fields, the Extended Groth Strip, and the UKIDSS Ultra Deep Survey field. We find that {\$}39.2{\^{}}{\{}+3.9{\}}{\_}{\{}-3.6{\}}{\$}$\backslash${\%} (65/166) of cSFGs at {\$}1.4{\textless}z{\textless}3.0{\$} host an X-ray detected AGN. This fraction is 3.2 times higher than the incidence of AGN in extended star-forming galaxies with similar masses at these redshifts. This difference is significant at the {\$}6.2\backslashsigma{\$} level. Our results are consistent with models in which cSFGs are formed through a dissipative contraction that triggers a compact starburst and concurrent growth of the central black hole. We also discuss our findings in the context of cosmological galaxy evolution simulations that require feedback energy to rapidly quench cSFGs. We show that the AGN fraction peaks precisely where energy injection is needed to reproduce the decline in the number density of cSFGs with redshift. Our results suggest that the first abundant population of massive, quenched galaxies emerged directly following a phase of elevated supermassive black hole growth and further hints at a possible connection between AGN and the rapid quenching of star formation in these galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1710.05921}, -author = {Kocevski, Dale D and Barro, Guillermo and Faber, S M and Dekel, Avishai and Somerville, Rachel S and Young, Joshua A and Williams, Christina C and McIntosh, Daniel H and Georgakakis, Antonis and Hasinger, Guenther and Nandra, Kirpal and Civano, Francesca and Alexander, David M and Almaini, Omar and Conselice, Christopher J and Donley, Jennifer L and Ferguson, Harry C and Giavalisco, Mauro and Grogin, Norman A and Hathi, Nimish and Hawkins, Matthew and Koekemoer, Anton M and Koo, David C and McGrath, Elizabeth J and Mobasher, Bahram and {P{\'{e}}rez Gonz{\'{a}}lez}, Pablo G and Pforr, Janine and Primack, Joel R and Santini, Paola and Stefanon, Mauro and Trump, Jonathan R and van der Wel, Arjen and Wuyts, Stijn and Yan, Haojing}, -doi = {10.3847/1538-4357/aa8566}, -eprint = {1710.05921}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {112}, -title = {{ CANDELS: Elevated Black Hole Growth in the Progenitors of Compact Quiescent Galaxies at z ∼ 2 }}, -url = {http://arxiv.org/abs/1710.05921%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa8566}, -volume = {846}, -year = {2017} -} -@inproceedings{Prodhomme2010, -abstract = {ESA's Gaia mission aims to create a complete and highly accurate stereoscopic map of the Milky Way. The stellar parallaxes will be determined at the micro-arcsecond level, as a consequence the measurement of the stellar image location on the CCD must be highly accurate. The solar wind protons will create charge traps in the CCDs of Gaia, which will induce large charge loss and distort the stellar images causing a degradation of the location measurement accuracy. Accurate modelling of the stellar image distortion induced by radiation is required to mitigate these effects. We assess the capability of a fast physical analytical model of radiation damage effects called the charge distortion model (CDM) to reproduce experimental data. To realize this assessment we developed a rigorous procedure that compares at the sub-pixel level the model outcomes to damaged images extracted from the experimental tests. We show that CDM can reproduce accurately up to a certain level the test data acquired on a highly irradiated device operated in time delay integration mode for different signal levels and different illumination histories. We discuss the potential internal and external factors that contributed to limit the agreement between the data and the charge distortion model. To investigate these limiting factors further, we plan to apply our comparison procedure on a synthetic dataset generated through detailed Monte-Carlo simulations at the CCD electrode level. © 2010 SPIE.
}, -author = {Prod'homme, Thibaut and Weiler, Michael and Brown, Scott W. and Short, Alexander D. T. and Brown, Anthony G. A.}, -booktitle = {High Energy, Optical, and Infrared Detectors for Astronomy IV}, -doi = {10.1117/12.855883}, -isbn = {9780819482327}, -issn = {0277-786X}, -keywords = {Analytical model,Astronomy,CCD,Charge loss,Charge trap,Computer simulation,Data sets,Detectors,Distortion model,Experimental data,Experimental test,Gaia,Gaia mission,Geometrical optics,High energy physics,Image processing,Infrared detectors,Internal and external factors,Irradiated devices,Limiting factors,Mathematical models,Measurement accuracy,Micro-arcsecond,Milky ways,Models,Monte Carlo Simulation,Radiation damage,Radiation damage effects,Signal level,Solar wind,Stellar images,Sub pixels,Test data,Time delay integration,astrometry,astronomy,radiation damage}, -month = {jul}, -pages = {774213}, -series = {\procspie}, -title = {{Comparison of a fast analytical model of radiation damage effects in CCDs with experimental tests}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.855883}, -volume = {7742}, -year = {2010} -} -@article{Murray2012, -abstract = {The charge transfer efficiency of a CCD is based on the average level of signal lost per pixel over a number of transfers. This value can be used to directly compare the relative performances of different structures, increases in radiation damage or to quantify improvements in operating parameters. This number does not however give sufficient detail to mitigate for the actual signal loss/deference in either of the transfer directions that may be critical to measuring shapes to high accuracy, such as those required in astronomy applications (e.g. for Gaia's astrometry or the galaxy distortion measurements for Euclid) based in the radiation environment of space. Pocket-pumping is an established technique for finding the location and activation levels of traps; however, a number of parameters in the process can also be explored to identify the trap species and location to sub-pixel accuracy. This information can be used in two ways to increase the sensitivity of a camera. Firstly, the clocking process can be optimised for the time constant of the majority of traps in each of the transfer directions, reducing deferred charge during read out. Secondly, a correction algorithm can be developed and employed during the post-processing of individual frames to move most of any deferred signal back into the charge packet it originated from. Here we present the trap-pumping techniques used to optimise the charge transfer efficiency of p- and n-channel e2v CCD204s and describe the use of trap-pumped images for on-orbit calibration and ground based image correction algorithms.}, -author = {Murray, N J and Holland, A D and Gow, J P D and Hall, D J and Tutt, James H and Burt, D and Endicott, J}, -doi = {10.1117/12.926804}, -isbn = {9780819491541}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy V}, -keywords = {ccd,cte,cti,p-channel,pocket pumping,transfer,traps}, -pages = {845317}, -title = {{Mitigating radiation-induced charge transfer inefficiency in full-frame CCD applications by 'pumping' traps}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.926804}, -volume = {8453}, -year = {2013} -} -@article{Bruce2012, -abstract = {The Wide-field Infrared Survey Explorer (WISE) has scanned the entire sky with unprecedented sensitivity in four infrared bands, at 3.4, 4.6, 12, and 22 $\mu$m. The WISE Point Source Catalog contains more than 560 million objects, among them hundreds of thousands of galaxies with Active Nuclei (AGN). While type 1 AGN, owing to their bright and unobscured nature, are easy to detect and constitute a rather complete and unbiased sample, their type 2 counterparts, postulated by AGN unification, are not as straightforward to identify. Matching the WISE catalog with known QSOs in the Sloan Digital Sky Survey we confirm previous identification of the type 1 locus in the WISE color space. Using a very large database of the popular Clumpy torus models, we find the colors of the putative type 2 counterparts, and also, for the first time, predict their number vs. flux relation that can be expected to be observed in any given WISE color range. This will allow us to put statistically very significant constraints on the torus parameters. Our results are a successful test of the AGN unification scheme. Copyright {\textcopyright} International Astronomical Union 2014.}, -archivePrefix = {arXiv}, -arxivId = {1312.5380}, -author = {Nikutta, Robert and Nenkova, Maia and Ivezi{\'{c}}, {\v{Z}}eljko and Hunt-Walker, Nicholas and Elitzur, Moshe}, -doi = {10.1017/S1743921314003317}, -eprint = {1312.5380}, -isbn = {9781107045248}, -issn = {17439221}, -journal = {Proceedings of the International Astronomical Union}, -keywords = {catalogs,galaxies: Seyfert,galaxies: active,infrared: galaxies,methods: data analysis,methods: statistical,radiative transfer}, -number = {S304}, -pages = {56--60}, -pmid = {9185952}, -title = {{AGN torus properties with WISE}}, -url = {http://arxiv.org/abs/1301.6373}, -volume = {9}, -year = {2014} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {2041-8213}, -journal = {The Astrophysical Journal}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -number = {2}, -pages = {L14}, -title = {{ Spatially Resolved Patchy Ly $\alpha$ Emission within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8 }}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -volume = {845}, -year = {2017} -} -@article{Sales2012a, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright} 2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V. and Navarro, Julio F. and Theuns, Tom and Schaye, Joop and White, Simon D.M. and Frenk, Carlos S. and Crain, Robert A. and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sales et al. - 2012 - The origin of discs and spheroids in simulated galaxies(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, $\sigma$(R), for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude MK {\textless} -25.3mag, or stellar mass M* ≳ 4 × 1011M⊙, within 108 Mpc. Our wide-field 107 arcsec × 107 arcsec IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes $\gamma$ inner and $\gamma$ outer of s(R). While $\gamma$ inner is mostly negative, of the 56 galaxies with sufficient radial coverage to determine $\gamma$ outer we find 36 per cent to have rising outer dispersion profiles, 30 per cent to be flat within the uncertainties and 34 per cent to be falling. The fraction of galaxies with rising outer profiles increases with M* and in denser galaxy environment, with 10 of the 11 most massive galaxies in our sample having flat or rising dispersion profiles. The strongest environmental correlations are with local density and halo mass, but a weaker correlation with large-scale density also exists. The average $\gamma$ outer is similar for brightest group galaxies, satellites and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis h4. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E and Thomas, Jens and Blakeslee, John P and Walsh, Jonelle L and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{Hoekstra2004, -abstract = {We present the results of a study of weak lensing by galaxies based on 45.5 deg{\$}{\^{}}2{\$} of {\$}R{\_}C{\$} band imaging data from the Red-Sequence Cluster Survey (RCS). We present the first weak lensing detection of the flattening of galaxy dark matter halos. We use a simple model in which the ellipticity of the halo is {\$}f{\$} times the observed ellipticity of the lens. We find a best fit value of {\$}f=0.77{\^{}}{\{}+0.18{\}}{\_}{\{}-0.21{\}}{\$}, suggesting that the dark matter halos are somewhat rounder than the light distribution. The fact that we detect a significant flattening implies that the halos are well aligned with the light distribution. Given the average ellipticity of the lenses, this implies a halo ellipticity of {\$}{\textless}e{\_}{\{}\backslashbackslashrm halo{\}} {\textgreater}=0.33{\^{}}{\{}+0.07{\}}{\_}{\{}-0.09{\}}{\$}, in fair agreement with results from numerical simulations of CDM. This result provides strong support for the existence of dark matter, as an isotropic lensing signal is excluded with 99.5{\%} confidence. We also study the average mass profile around the lenses, using a maximum likelihood analysis. We consider two models for the halo mass profile: a truncated isothermal sphere (TIS) and an NFW profile. We adopt observationally motivated scaling relations between the lens luminosity and the velocity dispersion and the extent of the halo. The best fit NFW model yields a mass {\$}M{\_}{\{}200{\}}=(8.4\backslashbackslashpm0.7\backslashbackslashpm0.4)\backslashbackslashtimes 10{\^{}}{\{}11{\}} h{\^{}}{\{}-1{\}} M{\_}\backslashbackslashodot{\{}\backslash{\$}{\}} and a scale radius {\$}r{\_}s=16.2{\^{}}{\{}+3.6{\}}{\_}{\{}-2.9{\}} h{\^{}}{\{}-1{\}}{\$} kpc. This value for the scale radius is in excellent agreement with predictions from numerical simulations for a halo of this mass.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0306515}, -author = {Hoekstra, Henk and Yee, Howard K C and Gladders, Michael D}, -doi = {10.1086/382726}, -eprint = {0306515}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {67--77}, -primaryClass = {astro-ph}, -title = {{Properties of galaxy dark matter halos from weak lensing}}, -url = {http://arxiv.org/abs/astro-ph/0306515%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/382726}, -volume = {606}, -year = {2003} -} -@article{Cropper2013, -abstract = {This paper describes the definition of a typical next-generation space-based weak gravitational lensing experiment. We first adopt a set of top-level science requirements from the literature, based on the scale and depth of the galaxy sample, and the avoidance of systematic effects in the measurements which would bias the derived shear values. We then identify and categorize the contributing factors to the systematic effects, combining them with the correct weighting, in such a way as to fit within the top-level requirements. We present techniques which permit the performance to be evaluated and explore the limits at which the contributing factors can be managed. Besides the modelling biases resulting from the use of weighted moments, the main contributing factors are the reconstruction of the instrument point spread function, which is derived from the stellar images on the image, and the correction of the charge transfer inefficiency in the CCD detectors caused by radiation damage. {\textcopyright} 2013 The Authors.}, -author = {Cropper, Mark and Hoekstra, Henk and Kitching, Thomas and Massey, Richard and Amiaux, J{\'{e}}r{\^{o}}me and Miller, Lance and Mellier, Yannick and Rhodes, Jason and Rowe, Barnaby and Pires, Sandrine and Saxton, Curtis and Scaramella, Roberto}, -doi = {10.1093/mnras/stt384}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Cropper et al. - 2013 - Defining a weak lensing experiment in space.pdf:pdf}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Cosmological parameters,Cosmology: observations,Gravitational lensing: weak,Methods: statistical,Space vehicles: instruments}, -number = {4}, -pages = {3103--3126}, -title = {{Defining a weak lensing experiment in space}}, -volume = {431}, -year = {2013} -} -@article{Metcalf2012, -abstract = {We investigate the statistics of flux anomalies in gravitationally lensed quasi-stellar objects as a function of dark matter halo properties such as substructure content and halo ellipticity. We do this by creating a very large number of simulated lenses with finite source sizes to compare with the data. After analysing these simulations, we conclude the following. (1) The finite size of the source is important. The point source approximation commonly used can cause biased results. (2) The widely used R cusp statistic is sensitive to halo ellipticity as well as the lens' substructure content. (3) For compact substructure, we find new upper bounds on the amount of substructure from the fact that no simple single-galaxy lenses have been observed with a single source having more than four well separated images. (4) The frequency of image flux anomalies is largely dependent on the total surface mass density in substructures and the size-mass relation for the substructures, and not on the range of substructure masses. (5) Substructure models with the same size-mass relation produce similar numbers of flux anomalies even when their internal mass profiles are different. (6) The lack of high image multiplicity lenses puts a limit on a combination of the substructures' size-mass relation, surface density and mass. (7) Substructures with shallower mass profiles and/or larger sizes produce less extra images. (8) The constraints that we are able to measure here with current data are roughly consistent with $\Lambda$ cold dark matter ($\Lambda$CDM) N-body simulations. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1007.1599}, -author = {Metcalf, R. Benton and Amara, Adam}, -doi = {10.1111/j.1365-2966.2011.19982.x}, -eprint = {1007.1599}, -isbn = {9781479989751}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Gravitational lensing: strong}, -month = {feb}, -number = {4}, -pages = {3414--3425}, -title = {{Small-scale structures of dark matter and flux anomalies in quasar gravitational lenses}}, -volume = {419}, -year = {2012} -} -@article{Bailin2005, -abstract = {(Abridged) We investigate how the shapes and angular momenta of galaxy and group mass dark matter halos in a LCDM N-body simulation are correlated internally, and how they are aligned with respect to the location and properties of surrounding halos. We explore these relationships down to halos of much lower mass (10^11/h Msun) than previous studies. The halos are triaxial, with c/a ratios of 0.6+-0.1. More massive halos are more flattened. The principal axes are very well aligned within 0.6 r_vir. The angular momentum vectors are also reasonably well aligned except between the very outermost and very innermost regions of the halo. The angular momentum vectors tend to align with the minor axes, with a mean misalignment of $\sim$25 degrees, and lie perpendicular to the major and intermediate axes. The properties of a halo at 0.4 r_vir are quite characteristic of the properties at most other radii within the halo. There is a very strong tendency for the minor axes of halos to lie perpendicular to large scale filaments. This alignment extends to much larger separations for group and cluster mass halos than for galaxy mass halos. As a consequence, the intrinsic alignments of galaxies are likely weaker than previous predictions, which were based on the shapes of cluster mass halos. The angular momenta of the highest concentration halos tend to point toward other halos. The angular momenta of galaxy mass halos point parallel to filaments, while those of group and cluster mass halos show a very strong tendency to point perpendicular to the filaments. This suggests that group and cluster mass halos acquire most of their angular momentum from major mergers along filaments, while the accretion history of mass and angular momentum onto galaxy mass halos has been smoother.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0408163}, -author = {Bailin, Jeremy and Steinmetz, Matthias}, -doi = {10.1086/430397}, -eprint = {0408163}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bailin, Steinmetz - 2005 - Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos(2).pdf:pdf}, -isbn = {0309072808}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Clusters: General,Galaxies: Formation,Galaxies: Halos,Galaxies: Structure,Methods: n-Body Simulations}, -number = {2}, -pages = {647--665}, -pmid = {25057539}, -primaryClass = {astro-ph}, -title = {{Internal and External Alignment of the Shapes and Angular Momenta of $\Lambda$CDM Halos}}, -url = {http://arxiv.org/abs/astro-ph/0408163%0Ahttp://dx.doi.org/10.1086/430397}, -volume = {627}, -year = {2005} -} -@article{Ma2014, -abstract = {Massive early-type galaxies represent the modern day remnants of the earliest major star formation episodes in the history of the universe. These galaxies are central to our understanding of the evolution of cosmic structure, stellar populations, and supermassive black holes, but the details of their complex formation histories remain uncertain. To address this situation, we have initiated the MASSIVE Survey, a volume-limited, multi-wavelength, integral-field spectroscopic (IFS) and photometric survey of the structure and dynamics of the ∼100 most massive early-type galaxies within a distance of 108 Mpc. This survey probes a stellar mass range M∗ ≳ 1011.5 M⊙ and diverse galaxy environments that have not been systematically studied to date. Our wide-field IFS data cover about two effective radii of individual galaxies, and for a subset of them, we are acquiring additional IFS observations on sub-arcsecond scales with adaptive optics. We are also acquiring deep K-band imaging to trace the extended halos of the galaxies and measure accurate total magnitudes. Dynamical orbit modeling of the combined data will allow us to simultaneously determine the stellar, black hole, and dark matter halo masses. The primary goals of the project are to constrain the black hole scaling relations at high masses, investigate systematically the stellar initial mass function and dark matter distribution in massive galaxies, and probe the late-time assembly of ellipticals through stellar population and kinematical gradients. In this paper, we describe the MASSIVE sample selection, discuss the distinct demographics and structural and environmental properties of the selected galaxies, and provide an overview of our basic observational program, science goals and early survey results.}, -archivePrefix = {arXiv}, -arxivId = {1407.1054}, -author = {Ma, Chung Pei and Greene, Jenny E and McConnell, Nicholas and Janish, Ryan and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/795/2/158}, -eprint = {1407.1054}, -isbn = {0000000000}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,dark matter,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content,galaxies: structure}, -number = {2}, -pages = {158}, -pmid = {28562576}, -title = {{The massive survey. I. A volume-limited integral-field spectroscopic study of the most massive early-type galaxies within 108 Mpc}}, -url = {http://adsabs.harvard.edu/abs/2014ApJ...795..158M}, -volume = {795}, -year = {2014} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M * = 1010.2 to 1012.0 M . We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority (≳75{\%}) of elliptical galaxies is not well described by a single S{\'{e}}rsic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (Re ∼ 1 kpc) inner component with luminosity fraction f 0.1-0.15; an intermediate-scale (Re 2.5 kpc) middle component with f 0.2-0.25; and a dominant (f = 0.6), extended (Re 10 kpc) outer envelope. All subcomponents have average S{\'{e}}rsic indices n 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies. {\textcopyright}2013. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C and Peng, Chien Y and Li, Zhao Yu and Barth, Aaron J}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{Lin2017, -abstract = {This paper reports the development of a Python Non-Uniform Fast Fourier Transform (PyNUFFT) package, which accelerates non-Cartesian image reconstruction on heterogeneous platforms. Scientific computing with Python encompasses a mature and integrated environment. The NUFFT algorithm has been extensively used for non-Cartesian image reconstruction but previously there was no native Python NUFFT library. The current PyNUFFT software enables multi-dimensional NUFFT on heterogeneous platforms. The PyNUFFT also provides several solvers, including the conjugate gradient method, ℓ1 total-variation regularized ordinary least square (L1TV-OLS) and ℓ1 total-variation regularized least absolute deviation (L1TV-LAD). Metaprogramming libraries were employed to accelerate PyNUFFT. The PyNUFFT package has been tested on multi-core CPU and GPU, with acceleration factors of 6.3 - 9.5× on a 32 thread CPU platform and 5.4 - 13× on the GPU.}, -archivePrefix = {arXiv}, -arxivId = {1710.03197}, -author = {Lin, Jyh Miin}, -eprint = {1710.03197}, -file = {:C\:/Users/Jammy/Documents/Papers/PYNUFFT.pdf:pdf}, -issn = {23318422}, -journal = {arXiv}, -keywords = {Graphic processing unit (GPU),Heterogeneous system architecture (HSA),Metaprogramming,Multi-core system,ℓ1 total variation regularized reconstruction}, -pages = {1--22}, -title = {{Python Non-Uniform Fast Fourier Transform (PyNUFFT): multi-dimensional non-Cartesian image reconstruction package for heterogeneous platforms and applications to MRI}}, -year = {2017} -} -@article{Guo2016, -abstract = {Deep learning algorithms are a subset of the machine learning algorithms, which aim at discovering multiple levels of distributed representations. Recently, numerous deep learning algorithms have been proposed to solve traditional artificial intelligence problems. This work aims to review the state-of-the-art in deep learning algorithms in computer vision by highlighting the contributions and challenges from over 210 recent research papers. It first gives an overview of various deep learning approaches and their recent developments, and then briefly describes their applications in diverse vision tasks, such as image classification, object detection, image retrieval, semantic segmentation and human pose estimation. Finally, the paper summarizes the future trends and challenges in designing and training deep neural networks.}, -archivePrefix = {arXiv}, -arxivId = {1508.01887}, -author = {Guo, Yanming and Liu, Yu and Oerlemans, Ard and Lao, Songyang and Wu, Song and Lew, Michael S}, -doi = {10.1016/j.neucom.2015.09.116}, -eprint = {1508.01887}, -isbn = {0925-2312}, -issn = {18728286}, -journal = {Neurocomputing}, -keywords = {Applications,Challenges,Computer vision,Deep learning,Developments,Trends}, -pages = {27--48}, -pmid = {25462632}, -title = {{Deep learning for visual understanding: A review}}, -volume = {187}, -year = {2016} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ({\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashgamma{\}}{\$}), we find that, although the zero cosmic curvature is still included within {\$}2 \backslashsigma{\$} confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile {\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashalpha{\}}{\$} to be different from that of the total-mass density profile {\$}\backslashnu\backslashsim r{\^{}}{\{}-\backslashdelta{\}}{\$}, a weaker constraint on the curvature ({\$}\backslashOmega{\_}k{\textless}0.197{\$} at 68$\backslash${\%} confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of {\$}\backslashDelta \backslashOmega{\_}k\backslashsimeq 10{\^{}}{\{}-3{\}}{\$}, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{Tenneti2014, -abstract = {The intrinsic alignment of galaxy shapes with the large-scale density field is a contaminant to weak lensing measurements, as well as being an interesting signature of galaxy formation and evolution (albeit one that is difficult to predict theoretically). Here we investigate the shapes and relative orientations of the stars and dark matter of haloes and subhaloes (central and satellite) extracted from the MassiveBlack-II simulation, a state-of-the-art high-resolution hydrodynamical cosmological simulation which includes stellar and active galactic nucleus feedback in a volume of (100 h-1 Mpc)3. We consider redshift evolution from z = 1 to 0.06 and mass evolution within the range of subhalo masses, 1010-6.0 × 1014.0 h-1 M⊙. The shapes of the dark matter distributions are generally more round than the shapes defined by stellar matter. The projected root-mean-square ellipticity per component for stellar matter is measured to be erms = 0.28 at z = 0.3 for Msubhalo {\textgreater} 1012.0 h-1 M⊙, which compares favourably with observational measurements. We find that the shapes of stellar and dark matter are more round for less massive subhaloes and at lower redshifts. By directly measuring the relative orientation of the stellar matter and dark matter of subgroups, we find that, on average, the misalignment between the two components is larger for less massive subhaloes. The mean misalignment angle varies from {\$\sim${}}30° to 10° for M {\$\sim${}} 1010-1014 h-1 M⊙ and shows a weak dependence on redshift. We also compare the misalignment angles in central and satellite subhaloes at fixed subhalo mass, and find that centrals are more misaligned than satellites. We present fitting formulae for the shapes of dark and stellar matter in subhaloes and also the probability distributions of misalignment angles. {\textcopyright}2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1403.4215}, -author = {Tenneti, Ananth and Mandelbaum, Rachel and {Di Matteo}, Tiziana and Feng, Yu and Khandai, Nishikanta}, -doi = {10.1093/mnras/stu586}, -eprint = {1403.4215}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: star formation,Gravitational lensing: weak,Hydrodynamics,Methods: numerical}, -number = {1}, -pages = {470--485}, -title = {{Galaxy shapes and intrinsic alignments in the MassiveBlack-II simulation}}, -volume = {441}, -year = {2014} -} -@article{Geometryen, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Hall2014a, -abstract = {Charge-Coupled Devices are the detector of choice for the focal planes of many optical and X-ray space telescopes. In recent years, EM-CCDs, SCDs and CMOS sensors have been used, or baselined, for missions in which the detection of X-ray and visible photons are key to the science goals of the mission. When placed in orbit, silicon-based detectors will suffer radiation damage as a consequence of the harsh space radiation environment, creating traps in the silicon. The radiation-induced traps will capture and release signal electrons, effectively "smearing" the image. Without correction, this smearing of the image would have major consequences on the science goals of the missions. Fitting to observed results, through careful planning of observation strategies while the radiation dose received remains low in the early stages of the mission, has previously been used to correct against the radiation damage effects. As the science goals becoming increasingly demanding, however, the correction algorithms require greater accuracy and a more physical approach is required, removing the effects of the radiation damage by modelling the trap capture and release mechanisms to a high level of detail. The drive for increasingly accurate trap parameters has led to the development of new methods of characterisation of traps in the silicon, measuring the trap properties and their effects to the single-trap level in situ. Here, we summarise the latest developments in trap characterisation techniques for n-channel and p-channel devices. ? 2014 SPIE.}, -author = {Hall, David J and Murray, Neil and Gow, Jason and Wood, Daniel and Holland, Andrew}, -doi = {10.1117/12.2055906}, -isbn = {9780819496225}, -issn = {1996756X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VI}, -keywords = {CTI,Defect,Euclid,Gaia,HST,N-channel,P,[CCD}, -number = {0}, -pages = {915408}, -title = {{ In situ trap parameter studies in CCDs for space applications }}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2055906}, -volume = {9154}, -year = {2014} -} -@article{Sonnenfeld2022, -abstract = {Context. Existing samples of strong lenses have been assembled by giving priority to sample size, but this is often at the cost of a complex selection function. However, with the advent of the next generation of wide-field photometric surveys, it might become possible to identify subsets of the lens population with well-defined selection criteria, trading sample size for completeness. Aims. There are two main advantages of working with a complete sample of lenses. First, such completeness makes possible to recover the properties of the general population of galaxies, of which strong lenses are a biased subset. Second, the relative number of lenses and non-detections can be used to further constrain models of galaxy structure. The present work illustrates how to carry out a statistical strong lensing analysis that takes advantage of these features. Methods. I introduce a general formalism for the statistical analysis of a sample of strong lenses with known selection function, and then test it on simulated data. The simulation consists of a population of 105 galaxies with an axisymmetric power-law density profile, a population of background point sources, and a subset of $\sim$103 strong lenses, which form a complete sample above an observational cut. Results. The method allows the user to recover the distribution of the galaxy population in Einstein radius and mass density slope in an unbiased way. The number of non-lenses helps to constrain the model when magnification data are not available. Conclusions. Complete samples of lenses are a powerful asset with which to turn precise strong lensing measurements into accurate statements on the properties of the general galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {2109.13246}, -author = {Sonnenfeld, Alessandro}, -doi = {10.1051/0004-6361/202142301}, -eprint = {2109.13246}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Sonnenfeld2022Stats.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Galaxies: fundamental parameters,Gravitational lensing: strong}, -pages = {1--11}, -title = {{Statistical strong lensing: III. Inferences with complete samples of lenses}}, -volume = {659}, -year = {2022} -} -@article{Wang2018, -abstract = {We explore the isothermal total density profiles of early-type galaxies (ETGs) in the IllustrisTNG simulation. For the selected 559 ETGs at z = 0 with stellar masses {\$}10{\^{}}{\{}10.7{\}}\backslash, \backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot {\}} \backslashleqslant M{\_}{\{}\backslashast {\}} \backslashleqslant 10{\^{}}{\{}11.9{\}}\backslash, \backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot {\}}{\$}, the total power-law slope has a mean of 〈$\gamma$′〉 = 2.011 ± 0.007 and a scatter of {\$}\backslashsigma {\_}{\{}\backslashgamma {\^{}}{\{}\backslashprime {\}}{\}} = 0.171{\$} over the radial range 0.4–4 times the stellar half-mass radius. Several correlations between $\gamma$′ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction, and in situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduces many correlation trends, and in particular, $\gamma$′ is almost constant with redshift below z = 2. Through analysing IllustrisTNG model variations, we show that black hole kinetic winds are crucial to lowering $\gamma$′ and matching observed galaxy correlations. The effects of stellar winds on $\gamma$′ are subdominant compared to active galactic nucleus (AGN) feedback, and differ due to the presence of AGN feedback from previous works. The density profiles of the ETG dark matter haloes are well described by steeper than NFW profiles, and they are steeper in the full physics (FP) run than their counterparts in the dark matter-only (DMO) run. Their inner density slopes anticorrelate (remain constant) with the halo mass in the FP (DMO) run, and anticorrelate with the halo concentration parameter c200 in both the types of runs. The dark matter haloes of low-mass ETGs are contracted whereas high-mass ETGs are expanded, suggesting that variations in the total density profile occur through the different halo responses to baryons.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -doi = {10.1093/mnras/stz3348}, -eprint = {1811.06545}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology,dark,formation,galaxies,matter,methods,numerical,structure,theory}, -number = {4}, -pages = {5188--5215}, -title = {{Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {491}, -year = {2020} -} -@article{Spavone2017, -abstract = {Observations of diffuse starlight in the outskirts of galaxies are thought to be a fundamental source of constraint on the cosmological context of galaxy assembly in the $\Lambda$CDM model. Such observations are not trivial because of the extreme faintness of such regions. In this work, we investigated the photometric properties of six massive early-type galaxies (ETGs) in the VEGAS sample (NGC 1399, NGC 3923, NGC 4365, NGC 4472, NGC 5044, and NGC 5846) out to extremely low surface brightness levels with the goal of characterizing the global structure of their light profiles for comparison to state-of-the-art galaxy formation models. We carried out deep and detailed photometric mapping of our ETG sample taking advantage of deep imaging with VST/OmegaCAM in the g and i bands. By fitting the light profiles, and comparing the results to simulations of elliptical galaxy assembly, we have identified signatures of a transition between relaxed and unrelaxed accreted components and can constrain the balance between in situ and accreted stars. The very good agreement of our results with predictions from theoretical simulations demonstrates that the full VEGAS sample of {\$\sim${}}100 ETGs will allow us to use the distribution of diffuse light as a robust statistical probe of the hierarchical assembly of massive galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1703.10835}, -author = {Spavone, Marilena and Capaccioli, Massimo and Napolitano, Nicola R and Iodice, Enrichetta and Grado, Aniello and Limatola, Luca and Cooper, Andrew P and Cantiello, Michele and Forbes, Duncan A and Paolillo, Maurizio and Schipani, Pietro}, -doi = {10.1051/0004-6361/201629111}, -eprint = {1703.10835}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: formation,Galaxies: fundamental parameters,Galaxies: halos,Techniques: image processing,cD}, -number = {3}, -pages = {A38}, -title = {{VEGAS: A VST Early-type GAlaxy Survey: II. Photometric study of giant ellipticals and their stellar halos}}, -url = {http://www.aanda.org/10.1051/0004-6361/201629111}, -volume = {603}, -year = {2017} -} -@article{Dekel2009, -abstract = {We present a simple theoretical framework for massive galaxies at high redshift, where the main assembly and star formation occurred, and report on the first cosmological simulations that reveal clumpy disks consistent with our analysis. The evolution is governed by the interplay between smooth and clumpy cold streams, disk instability, and bulge formation. Intense, relatively smooth streams maintain an unstable dense gas-rich disk. Instability with high turbulence and giant clumps, each a few percent of the disk mass, is self-regulated by gravitational interactions within the disk. The clumps migrate into a bulge in {\$\sim${}}10 dynamical times, or {\$\sim${}}0.5Gyr. The cosmological streams replenish the draining disk and prolong the clumpy phase to several Gigayears in a steady state, with comparable masses in disk, bulge, and dark matter within the disk radius. The clumps form stars in dense subclumps following the overall accretion rate, {\$\sim${}}100 Msun/yr, and each clump converts into stars in {\$\sim${}}0.5 Gyr. While the clumps coalesce dissipatively to a compact bulge, the star-forming disk is extended because the incoming streams keep the outer disk dense and susceptible to instability and because of angular momentum transport. Passive spheroid-dominated galaxies form when the streams are more clumpy: the external clumps merge into a massive bulge and stir up disk turbulence that stabilize the disk and suppress in situ clump and star formation. We predict a bimodality in galaxy type by z{\$\sim${}}3, involving giant-clump star-forming disks and spheroid-dominated galaxies of suppressed star formation. After z{\$\sim${}}1, the disks tend to be stabilized by the dominant stellar disks and bulges. Most of the high-z massive disks are likely to end up as today's early-type galaxies.}, -archivePrefix = {arXiv}, -arxivId = {0901.2458}, -author = {Dekel, Avishai and Sari, Re'Em and Ceverino, Daniel}, -doi = {10.1088/0004-637X/703/1/785}, -eprint = {0901.2458}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: halos,Galaxies: spiral,cD}, -month = {sep}, -number = {1}, -pages = {785--801}, -title = {{Formation of massive galaxies at high redshift: Cold streams, clumpy disks, and compact spheroids}}, -url = {http://stacks.iop.org/0004-637X/703/i=1/a=785?key=crossref.6c2d6916539a875e58937153ad6e9204}, -volume = {703}, -year = {2009} -} -@article{Szomoru2013, -abstract = {We present stellar mass surface density profiles of a mass-selected sample of 177 galaxies at 0.5 < z < 2.5, obtained using very deep Hubble Space Telescope optical and near-infrared data over the GOODS-South field, including recent CANDELS data. Accurate stellar mass surface density profiles have been measured for the first time for a complete sample of high-redshift galaxies more massive than 1010.7 M⊙. The key advantage of this study compared to previous work is that the surface brightness profiles are deconvolved for point-spread function smoothing, allowing accurate measurements of the structure of the galaxies. The surface brightness profiles account for contributions from complex galaxy structures such as rings and faint outer disks. Mass profiles are derived using radial rest-frame ug color profiles and a well-established empirical relation between these colors and the stellar mass-to-light ratio. We derive stellar half-mass radii from the mass profiles, and find that these are on average ∼25% smaller than rest-frame g-band half-light radii. This average size difference of 25% is the same at all redshifts, and does not correlate with stellar mass, specific star formation rate, effective surface density, S{\'{e}}rsic index, or galaxy size. Although on average the difference between half-mass size and half-light size is modest, for approximately 10% of massive galaxies this difference is more than a factor of two. These extreme galaxies are mostly extended, disk-like systems with large central bulges. These results are robust, but could be impacted if the central dust extinction becomes high. ALMA observations can be used to explore this possibility. These results provide added support for galaxy growth scenarios wherein massive galaxies at these epochs grow by accretion onto their outer regions. {\textcopyright} 2013. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1208.4363}, -author = {Szomoru, Daniel and Franx, Marijn and {Van Dokkum}, Pieter G. and Trenti, Michele and Illingworth, Garth D. and Labb{\'{e}}, Ivo and Oesch, Pascal}, -doi = {10.1088/0004-637X/763/2/73}, -eprint = {1208.4363}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -month = {feb}, -number = {2}, -pages = {73}, -title = {{The stellar mass structure of massive galaxies from z = 0 to z = 2.5: Surface density profiles and half-mass radii}}, -url = {http://stacks.iop.org/0004-637X/763/i=2/a=73?key=crossref.a6cbae626684f362d401becc1e688d16%5Cnpapers2://publication/doi/10.1088/0004-637X/763/2/73}, -volume = {763}, -year = {2013} -} -@article{Huang2017, -abstract = {Massive galaxies display extended light profiles that can reach several hundreds of kilo parsecs. These stellar halos provide a fossil record of galaxy assembly histories. Using data that is both wide ({\$\sim${}}100 square degree) and deep (i{\textgreater}28.5 mag/arcsec{\^{}}2 in i-band), we present a systematic study of the stellar halos of a sample of more than 3000 galaxies at 0.3 {\textless}z {\textless}0.5 with {\$}\backslashbackslashlog M{\_}{\{}\backslashbackslashstar{\{}\backslash{\}}{\}}/M{\_}{\{}\backslashbackslashodot{\{}\backslash{\}}{\}} {\textgreater}11.4{\$}. Our study is based on high-quality (0.6 arcsec seeing) imaging data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP), which enables us to individually estimate surface mass density profiles to 100 kpc without stacking. As in previous work, we find that more massive galaxies exhibit more extended outer profiles. When this extended light is not properly accounted for as a result of shallow imaging or inadequate profile modeling, the derived stellar mass function can be significantly underestimated at the highest masses. Across our sample, the ellipticity of outer light profiles increases substantially as we probe larger radii. We show for the first time that these ellipticity gradients steepen dramatically as a function of galaxy mass, but we detect no mass-dependence in outer color gradients. Our results support the two-phase formation scenario for massive galaxies in which outer envelopes are built up at late times from a series of merging events. We provide surface mass surface mass density profiles in a convenient tabulated format to facilitate comparisons with predictions from numerical simulations of galaxy formation.}, -archivePrefix = {arXiv}, -arxivId = {1707.01904}, -author = {Huang, Song and Leauthaud, Alexie and Greene, Jenny E and Bundy, Kevin and Lin, Yen Ting and Tanaka, Masayuki and Miyazaki, Satoshi and Komiyama, Yutaka}, -doi = {10.1093/mnras/stx3200}, -eprint = {1707.01904}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD- galaxies: formation,Galaxies: elliptical and lenticular,Galaxies: photometry,Galaxies: structure,Surveys}, -number = {3}, -pages = {3348--3368}, -title = {{Individual stellar haloes of massive galaxies measured to 100 kpc at 0.3 {\textless}z {\textless}0.5 using Hyper Suprime-Cam}}, -url = {http://arxiv.org/abs/1707.01904}, -volume = {475}, -year = {2018} -} -@article{Lanusse2017a, -abstract = {Galaxy-scale strong gravitational lensing can not only provide a valuable probe of the dark matter distribution of massive galaxies, but also provide valuable cosmological constraints, either by studying the population of strong lenses or by measuring time delays in lensed quasars. Due to the rarity of galaxy-scale strongly lensed systems, fast and reliable automated lens finding methods will be essential in the era of large surveys such as Large Synoptic Survey Telescope, Euclid and Wide-Field Infrared Survey Telescope. To tackle this challenge, we introduce CMU DeepLens, a new fully automated galaxy-galaxy lens finding method based on deep learning. This supervised machine learning approach does not require any tuning after the training step which only requires realistic image simulations of strongly lensed systems. We train and validate our model on a set of 20 000 LSST-like mock observations including a range of lensed systems of various sizes and signal-to-noise ratios (S/N).We find on our simulated data set that for a rejection rate of non-lenses of 99 per cent, a completeness of 90 per cent can be achieved for lenses with Einstein radii larger than 1.4 arcsec and S/N larger than 20 on individual g-band LSST exposures. Finally, we emphasize the importance of realistically complex simulations for training such machine learning methods by demonstrating that the performance of models of significantly different complexities cannot be distinguished on simpler simulations.}, -archivePrefix = {arXiv}, -arxivId = {1703.02642}, -author = {Lanusse, Fran{\c{c}}ois and Ma, Quanbin and Li, Nan and Collett, Thomas E. and Li, Chun Liang and Ravanbakhsh, Siamak and Mandelbaum, Rachel and P{\'{o}}czos, Barnab{\'{a}}s}, -doi = {10.1093/mnras/stx1665}, -eprint = {1703.02642}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Lanusse et al. - 2018 - CMU DeepLens Deep learning for automatic image-based galaxy-galaxy strong lens finding(2).pdf:pdf}, -isbn = {0021-9258 (Print)\r0021-9258 (Linking)}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Methods: statistical,gravitational lensing: strong}, -number = {3}, -pages = {3895--3906}, -pmid = {10913147}, -title = {{CMU DeepLens: Deep learning for automatic image-based galaxy-galaxy strong lens finding}}, -url = {http://arxiv.org/abs/1703.02642}, -volume = {473}, -year = {2018} -} -@article{Momcheva2015, -abstract = {We present the spectroscopic redshift catalog from a wide-field survey of the fields of 28 galaxy-mass strong gravitational lenses. We discuss the acquisition and reduction of the survey data, collected over 40 nights of 6.5 m MMT and Magellan time, employing four different multiobject spectrographs. We determine that no biases are introduced by combining data sets obtained with different telescope and spectrograph combinations. Special care is taken to determine redshift uncertainties using repeat observations. The redshift catalog consists of 9,768 new and unique galaxy redshifts. 82.4% of the catalog redshifts are between z = 0.1 and z = 0.7, and the catalog median redshift. The data from this survey will be used to study the lens environments and line-of-sight structures to gain a better understanding of the effects of large-scale structure on lens statistics and lens-derived parameters.}, -archivePrefix = {arXiv}, -arxivId = {1503.02074}, -author = {Momcheva, Ivelina G. and Williams, Kurtis A. and Cool, Richard J. and Keeton, Charles R. and Zabludoff, Ann I.}, -doi = {10.1088/0067-0049/219/2/29}, -eprint = {1503.02074}, -isbn = {1091-4269}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: distances and redshifts,galaxies: general,gravitational lensing: strong,surveys}, -number = {2}, -pages = {29}, -title = {{A SPECTROSCOPIC SURVEY of the FIELDS of 28 STRONG GRAVITATIONAL LENSES}}, -url = {http://stacks.iop.org/0067-0049/219/i=2/a=29?key=crossref.a5471e69f1ffb2b3fc0f578df7cf09b5}, -volume = {219}, -year = {2015} -} -@article{Governato2015, -abstract = {We use high-resolution Hydro+N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass $\sim$106-7 M⊙, total mass 1010 M⊙) in $\Lambda$-dominated cold dark matter (CDM) and 2 keV warm dark matter (WDM) cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the dark matter (DM) model, but proportionally to the SF efficiency, gas outflows lower the central mass density through 'dynamical heating', such that all realizations have circular velocities < 20 km s-1 at 500 pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial colour- magnitude diagrams and star formation histories (SFHs) in order to directly compare to available observations. The simulated galaxies formed most of their stars in many $\sim$10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including 'baryon physics' in simulations when (1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and (2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F. and Weisz, D. and Pontzen, A. and Loebman, S. and Reed, D. and Brooks, A. M. and Behroozi, P. and Christensen, C. and Madau, P. and Mayer, L. and Shen, S. and Walker, M. and Quinn, T. and Keller, B. W. and Wadsley, J.}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Governato et al. - 2015 - Faint dwarfs as a test of DM models WDM versus CDM.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Tagore2016, -abstract = {Lens modelling of resolved image data has advanced rapidly over the past two decades. More recently pixel-based approaches, wherein the source is reconstructed on an irregular or adaptive grid, have become popular. Generally, the source reconstruction takes place in a Bayesian framework and is guided by a set of sensible priors. We discuss the integration of a shapelets-based method into a Bayesian framework and quantify the required regularization. In such approaches, the source is reconstructed analytically, using a subset of a complete and orthonormal set of basis functions, known as shapelets. To calculate the flux in an image plane pixel, the pixel is split into two or more triangles (depending on the local magnification), and each shapelet basis function is integrated over the source plane. Source regularization (enforcement of priors on the source) can also be performed analytically. This approach greatly reduces the number of source parameters from the thousands to hundreds and results in a posterior probability distribution that is much less noisy than pixel-based approaches.}, -archivePrefix = {arXiv}, -arxivId = {1505.00198}, -author = {Tagore, Amitpal S. and Jackson, Neal}, -doi = {10.1093/mnras/stw057}, -eprint = {1505.00198}, -isbn = {0027-8424 (Print)}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Gravitational lensing: strong,Methods: numerical}, -month = {apr}, -number = {3}, -pages = {3066--3075}, -pmid = {12481032}, -title = {{On the use of shapelets in modelling resolved, gravitationally lensed images}}, -volume = {457}, -year = {2016} -} -@article{Iwanus2017, -abstract = {We describe and test a novel dark matter annihilation feedback (DMAF) scheme that has been implemented into the well-known cosmological simulation code GADGET-2. In the models considered here, dark matter can undergo self-annihilation/decay into radiation and baryons. These products deposit energy into the surrounding gas particles and then the dark matter/baryon fluid is self-consistently evolved under gravity and hydrodynamics. We present tests of this new feedback implementation in the case of idealized dark matter haloes with gas components for a range of halomasses, concentrations and annihilation rates. For some darkmattermodels, DMAF's ability to evacuate gas is enhanced in lower mass, concentrated haloes where the injected energy is comparable to its gravitational binding energy. Therefore, we expect the strongest signs of darkmatter annihilation to imprint themselves on to the baryonic structure of concentrated dwarf galaxies through their baryonic fraction and star formation history. Finally, we present preliminary results of the first self-consistent DMAF cosmological box simulations showing that the small-scale substructure is washed out for large annihilation rates.}, -archivePrefix = {arXiv}, -arxivId = {1707.06770}, -author = {Iwanus, N. and Elahi, P. J. and Lewis, G. F.}, -doi = {10.1093/MNRAS/STX1974}, -eprint = {1707.06770}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Iwanus, Elahi, Lewis - 2017 - Dark matter annihilation feedback in cosmological simulations - I Code convergence and idealized haloes(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Large-scale structure of Universe}, -number = {1}, -pages = {1214--1225}, -title = {{Dark matter annihilation feedback in cosmological simulations - I: Code convergence and idealized haloes}}, -url = {http://arxiv.org/abs/1707.06770%0Ahttp://dx.doi.org/10.1093/mnras/stx1974}, -volume = {472}, -year = {2017} -} -@article{Peirani2008, -abstract = {If there is one key element in the social psychology of behaviour that is still missing from Stern's ABC model, it is the role of habit. Stern (2000) acknowledges this and proposes that an integrated model of environmentally significant behaviour would consist of four factors: 1) attitudes; 2) contextual factors; 3) personal capabilities; and 4) habits. The general thrust of Stern's suggestion is very similar to an attempt made almost thirty years ago by social psychologist Harry Triandis to develop an integrated model of 'interpersonal' behaviour. Triandis recognised the key role played by both social factors and emotions in forming intentions. He also highlighted the importance of past behaviour on the present. On the basis of these observations, Triandis proposed a Theory of Interpersonal Behaviour (Figure 4) in which intentions – as in many of the other models – are immediate antecedents of behaviour. But crucially, habits also mediate behaviour. And both these influences are moderated by facilitating conditions. Behaviour in any situation is, according to Triandis, a function partly of the intention, partly of the habitual responses, and partly of the situational constraints and conditions. The intention is influenced by social and affective factors as well as by rational deliberations. One is neither fully deliberative, in Triandis' model, nor fully automatic. One is neither fully autonomous nor entirely social. Behaviour is influenced by moral beliefs, but the impact of these is moderated both by emotional drives and cognitive limitations. Social factors include norms, roles and self-concept. Norms are the social rules about what should and should not be done. Roles are 'sets of behaviours that are considered appropriate for persons holding particular positions in a group' (Triandis, 1977). Self-concept refers to the idea that a person has of his/herself, the goals that it is appropriate for the person to pursue or to eschew, and the behaviours that the person does or does not engage in. Emotional responses to a decision or to a decision situation are assumed distinct from rational-instrumental evaluations of consequences, and may include both positive and negative emotional responses of varying strengths. Affect has a more or less unconscious input to decision-making, and is governed by instinctive behavioural responses to particular situations. Figure 3 Triandis' Theory of Interpersonal Behaviour Triandis offers an explicit role for affective factors on behavioural intentions. In more recent writings, the attempt to incorporate emotional antecedents into a model of action has received a lot of support (Bagozzi et al., 2002, Steg et al., 2001). Triandis theory of interpersonal behaviour captures many of the criticisms levelled at rational choice theory in a way that is not done by some of the other models. It also can be, and has been, used as a framework for empirical analysis of the strengths and weaknesses of the component factors in different kinds of situations. It also can be, and has been, used as the framework for empirical analysis of the strengths and weaknesses of the component factors in different kinds of situations. Far less use has been made of Triandis work than was made of the Ajzen-Fishbein work. However, where it has been used, it appears to have additional explanatory value over Ajzen's model, in particular, by including role beliefs and habits. Affect}, -archivePrefix = {arXiv}, -arxivId = {arXiv:0803.1210v1}, -author = {Chadid, M. and Wade, G. and Landstreet, J.}, -doi = {10.1051/0004-6361}, -eprint = {arXiv:0803.1210v1}, -isbn = {0902009192}, -issn = {0004-6361}, -journal = {Astronomy and Astrophysics -Berlin-}, -keywords = {Activit{\'{e}} stellaire,Champ intense,Champ magn{\'{e}}tique,Espectropolarimetr{\'{i}}a,Etoile magn{\'{e}}tique,Etoile type RR Lyrae,High field,Magnetic fields,Magnetic stars,Modelo,Models,Mod{\`{e}}le,RR Lyr,RR Lyrae stars,Spectropolarimetry,Spectropolarim{\'{e}}trie,Stellar activity,stars: individual: RR Lyrae,stars: magnetic fields,stars: oscillations,stars: variables: RR Lyr,techniques: spectroscopic, polarimetric}, -month = {feb}, -number = {3}, -pages = {1087--1094}, -pmid = {9010224}, -title = {{No evidence of a strong magnetic field in the Blazhko star RR Lyrae}}, -volume = {413}, -year = {2004} -} -@article{Bower2017, -abstract = {Galaxies fall into two clearly distinct types: 'blue-sequence' galaxies which are rapidly forming young stars, and 'red-sequence' galaxies in which star formation has almost completely ceased. Most galaxies more massive than 3 × 1010M⊙ follow the red sequence, while less massive central galaxies lie on the blue sequence. We show that these sequences are created by a competition between star formation-driven outflows and gas accretion on to the supermassive black hole at the galaxy's centre. We develop a simple analytic model for this interaction. In galaxies less massive than 3 × 1010M⊙, young stars and supernovae drive a high-entropy outflow which is more buoyant than any tenuous corona. The outflow balances the rate of gas inflow, preventing high gas densities building up in the central regions. More massive galaxies, however, are surrounded by an increasingly hot corona. Above a halo mass of $\sim$1012M⊙, the outflow ceases to be buoyant and star formation is unable to prevent the build-up of gas in the central regions. This triggers a strongly non-linear response from the black hole. Its accretion rate rises rapidly, heating the galaxy's corona, disrupting the incoming supply of cool gas and starving the galaxy of the fuel for star formation. The host galaxy makes a transition to the red sequence, and further growth predominantly occurs through galaxy mergers.We show that the analytic model provides a good description of galaxy evolution in the EAGLE hydrodynamic simulations. So long as star formation-driven outflows are present, the transition mass scale is almost independent of subgrid parameter choice.}, -archivePrefix = {arXiv}, -arxivId = {1607.07445}, -author = {Bower, Richard G. and Schaye, Joop and Frenk, Carlos S. and Theuns, Tom and Schaller, Matthieu and Crain, Robert A. and McAlpine, Stuart}, -doi = {10.1093/mnras/stw2735}, -eprint = {1607.07445}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an en(4).pdf:pdf;:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2017 - The dark nemesis of galaxy formation Why hot haloes trigger black hole growth and bring star formation to an en(5).pdf:pdf}, -isbn = {0000000000000}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Quasars: general}, -number = {1}, -pages = {32--44}, -title = {{The dark nemesis of galaxy formation: Why hot haloes trigger black hole growth and bring star formation to an end}}, -volume = {465}, -year = {2017} -} -@article{Arcetri2018, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0311619v2}, -author = {Arcetri, Astrofisico and Fermi, Largo and Firenze, I-}, -eprint = {0311619v2}, -keywords = {active - galaxies,black hole physics -,evolution - galaxies,galaxies,general - cosmology,miscellaneous,nuclei - quasars}, -number = {May}, -pages = {1--20}, -primaryClass = {arXiv:astro-ph}, -title = {{Local Supermassive Black Holes , Relics of Active Galactic Nuclei and the X-ray Background}}, -volume = {20}, -year = {2018} -} -@article{Wang2014, -abstract = {Observations have shown that the spatial distribution of satellite galaxies is not random, but aligned with the major axes of central galaxies. This alignment is dependent on galaxy properties, such that red satellites are more strongly aligned than blue satellites. Theoretical work conducted to interpret this phenomenon has found that it is due to the non-spherical nature of dark matter halos. However, most studies overpredict the alignment signal under the assumption that the central galaxy shape follows the shape of the host halo. It is also not clear whether the color dependence of alignment is due to an assembly bias or an evolution effect. In this paper we study these problems using a cosmological N-body simulation. Subhalos are used to trace the positions of satellite galaxies. It is found that the shapes of dark matter halos are mis-aligned at different radii. If the central galaxy shares the same shape as the inner host halo, then the alignment effect is weaker and agrees with observational data. However, it predicts almost no dependence of alignment on the color of satellite galaxies, though the late accreted subhalos show stronger alignment with the outer layer of the host halo than their early accreted counterparts. We find that this is due to the limitation of pure N-body simulations where satellite galaxies without associated subhalos ("orphan galaxies") are not resolved. These orphan (mostly red) satellites often reside in the inner region of host halos and should follow the shape of the host halo in the inner region. {\textcopyright} 2014. The American Astronomical Society. All rights reserved..}, -archivePrefix = {arXiv}, -arxivId = {1403.1008}, -author = {Wang, Yang Ocean and Lin, W. P. and Kang, X. and Dutton, Aaron and Yu, Yu and Macci{\`{o}}, Andrea V.}, -doi = {10.1088/0004-637X/786/1/8}, -eprint = {1403.1008}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Wang et al. - 2014 - Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulati.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxy: halo,Galaxy: structure,dark matter,methods: numerical,methods: statistical}, -number = {1}, -pages = {8}, -title = {{Satellite alignment. I. Distribution of substructures and their dependence on assembly history from n-body simulations}}, -url = {http://arxiv.org/abs/1403.1008%5Cnhttp://iopscience.iop.org/0004-637X/786/1/8/article;.c1?genre=bookitem&sid=IOPP%3Ajnl_ref&spage=305&title=ArA&volume=5&date=1969&v_showaffiliations=no&aulast=Holmberg%5Cnhttp://stacks.iop.org/0004-637X/786/i=1/a=8?key=cro}, -volume = {786}, -year = {2014} -} -@article{Rhodes2001, -abstract = {Weak lensing by large-scale structure provides a unique method to directly measure matter fluctuations in the universe and has recently been detected from the ground. Here we report the first detection of this ``cosmic shear'' based on space-based images. The detection was derived from the Hubble Space Telescope (HST) Survey Strip (or ``Groth Strip''), a 4'x42' set of 28 contiguous Wide Field Planetary Camera 2 (WFPC2) pointings with I〈27. The small size of the HST point-spread function affords both a lower statistical noise and a much weaker sensitivity to systematic effects, a crucial limiting factor of cosmic shear measurements. Our method and treatment of systematic effects were discussed in an earlier paper. We measure an rms shear of 1.8% on the WFPC2 chip scale (1.27′), in agreement with the predictions of cluster-normalized cold dark matter (CDM) models. Using a maximum likelihood analysis, we show that our detection is significant at the 99.5% confidence level (CL) and measure the normalization of the matter power spectrum to be $\sigma$8$\Omega$0.48m= 0.51+0.14-0.17, in a $\Lambda$CDM universe. These 68% CL errors include (Gaussian) cosmic variance, systematic effects, and the uncertainty in the redshift distribution of the background galaxies. The signal comes primarily from the chip scale (1.27′) with gradually decreasing contributions up to roughly 10'. Our result is consistent with earlier lensing measurements from the ground and with the normalization derived from cluster abundance. We discuss how our measurement can be improved with the analysis of a large number of independent WFPC2 fields.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0101213}, -author = {Rhodes, Jason and Refregier, Alexandre and Groth, Edward J.}, -doi = {10.1086/320336}, -eprint = {0101213}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rhodes, Refregier, Groth - 2001 - Detection of Cosmic Shear with the ITALHubble Space TelescopeITAL Survey Strip.pdf:pdf}, -issn = {0004637X}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {L85--L88}, -primaryClass = {astro-ph}, -title = {{Detection of Cosmic Shear with the [ITAL]Hubble Space Telescope[/ITAL] Survey Strip}}, -volume = {552}, -year = {2001} -} -@article{Coenda2017, -abstract = {We present a comparative analysis of the properties of passive, star-forming and transition (green valley) galaxies in four discrete environments: field, groups, the outskirts and the core of X-ray clusters. We construct samples of galaxies from the Sloan Digital Sky Survey in these environments so that they are bound to have similar redshift distributions. The classification of galaxies into the three sequences is based on theUV-optical colourNUV-r. We study a number of galaxy properties: stellar mass, morphology, specific star formation rate and the history of star formation. The analysis of green valley (GV) galaxies reveals that the physical mechanisms responsible for external quenching become more efficient moving from the field to denser environments. We confirm previous findings thatGVgalaxies have intermediate morphologies; moreover, we find that this appears to be independent of the environment. Regarding the stellar mass of GV galaxies, we find that they tend to be more massive in the field than in denser environments. On average, GV galaxies account for $\sim$20 per cent of all galaxies in groups and X-ray clusters. We find evidence that the field environment is inefficient in transforming lowmass galaxies. GV galaxies have average star formation histories intermediate between passive and star-forming galaxies, and have a clear and consistent dependence on the environment: both, the quenching time and the amplitude of the star formation rate, decrease towards higher density environments.}, -archivePrefix = {arXiv}, -arxivId = {1710.05928}, -author = {Coenda, Valeria and Mart{\'{i}}nez, H{\'{e}}ctor J. and Muriel, Hern{\'{a}}n}, -doi = {10.1093/mnras/stx2707}, -eprint = {1710.05928}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Coenda, Mart{\'{i}}nez, Muriel - 2018 - Green valley galaxies as a transition population in different environments.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: clusters: general,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: groups: general}, -number = {4}, -pages = {5617--5629}, -title = {{Green valley galaxies as a transition population in different environments}}, -url = {http://arxiv.org/abs/1710.05928}, -volume = {473}, -year = {2018} -} -@article{Jee2014, -abstract = {The distance-redshift relation plays a fundamental role in constraining cosmological models. In this paper, we show that measurements of positions and time delays of strongly lensed images of a background galaxy, as well as those of the velocity dispersion and mass profile of a lens galaxy, can be combined to extract the angular diameter distance of the lens galaxy. Physically, as the velocity dispersion and the time delay give a gravitational potential (GM/r) and a mass (GM) of the lens, respectively, dividing them gives a physical size (r) of the lens. Comparing the physical size with the image positions of a lensed galaxy gives the angular diameter distance to the lens. A mismatch between the exact locations at which these measurements are made can be corrected by measuring a local slope of the mass profile. We expand on the original idea put forward by Paraficz and Hjorth, who analyzed singular isothermal lenses, by allowing for an arbitrary slope of a power-law spherical mass density profile, an external convergence, and an anisotropic velocity dispersion. We find that the effect of external convergence cancels out when dividing the time delays and velocity dispersion measurements. We derive a formula for the uncertainty in the angular diameter distance in terms of the uncertainties in the observables. As an application, we use two existing strong lens systems, B1608+656 (zL=0.6304) and RXJ1131-1231 (zL=0.295), to show that the uncertainty in the inferred angular diameter distances is dominated by that in the velocity dispersion, $\sigma$2, and its anisotropy. We find that the current data on these systems should yield about 16% uncertainty in DA per object. This improves to 13% when we measure $\sigma$2 at the so-called sweet-spot radius. Achieving 7% is possible if we can determine $\sigma$2 with 5% precision.}, -archivePrefix = {arXiv}, -arxivId = {1410.7770}, -author = {Jee, I. and Komatsu, E. and Suyu, S. H.}, -doi = {10.1088/1475-7516/2015/11/033}, -eprint = {1410.7770}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {galaxy dynamics,gravitational lensing}, -number = {11}, -pages = {33}, -title = {{Measuring angular diameter distances of strong gravitational lenses}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2015JCAP...11..033J&link_type=ABSTRACT%5Cnpapers://dcc533b5-8613-47b7-b88c-2b0c0d39c33f/Paper/p10857}, -volume = {2015}, -year = {2015} -} -@article{Rosas-Guevara2016, -abstract = {We investigate the evolution of supermassive black holes in the 'Evolution and Assembly of GaLaxies and their Environments' (EAGLE) cosmological hydrodynamic simulations. The largest of the EAGLE volumes covers a (100 cMpc)3 and includes state-of-the-art physical models for star formation and black hole growth that depend only on local gas properties. We focus on the black hole mass function, Eddington ratio distribution and the implied duty cycle of nuclear activity. The simulation is broadly consistent with observational constraints on these quantities. In order to make a more direct comparison with observational data, we calculate the soft and hard X-ray luminosity functions of the active galactic nuclei (AGN). Between redshifts 0 and 1, the simulation is in agreement with data. At higher redshifts, the simulation tends to underpredict the luminosities of the brightest observed AGN. This may be due to the limited volume of the simulation, or a fundamental deficiency of the underlying model. It seems unlikely that additional unresolved variability can account for this difference. The simulation shows a similar 'downsizing' of the AGN population as seen in observational surveys.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1604.00020}, -author = {Rosas-Guevara, Yetli and Bower, Richard G and Schaye, Joop and McAlpine, Stuart and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stw1679}, -eprint = {1604.00020}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Black hole physics,Galaxies: active,Galaxies: formation,Methods: numerical,Quasars: general}, -number = {1}, -pages = {190--205}, -title = {{Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth}}, -volume = {462}, -year = {2016} -} -@article{Silk1998, -abstract = {Quasars are widely believed to be powered by accretion on to supermassive black holes and there is now considerable evidence for a link between mergers, the activity of quasars and the formation of spheroids. Cattaneo, Haehnelt & Rees have demonstrated that a very simple model in which supermassive black holes form and accrete most of their mass in mergers of galaxies of comparable masses can reproduce the observed relation of black hole mass to bulge luminosity if black holes accrete a fraction of the mass in the merging remnant that varies with redshift. Here we investigate whether this simple model can account for the luminosity function of quasars and for the redshift evolution of the quasar population. We simulate hierarchical galaxy formation through the extended Press-Schechter formalism and assume that, when two galaxies of comparable masses merge, their central black holes coalesce and a fraction of the gas in the merger remnant is accreted by the supermassive black hole. We find that the decrease in the merging rate with cosmic time and the depletion in the amount of cold gas available due to star formation are not sufficient to explain the strong decline in the space density of bright quasars since z ∼ 2, if the fraction of accreted gas does not decrease at low redshift, as larger and larger structures form, which can potentially host brighter and brighter quasars. Moreover, we need another mechanism besides major mergers to explain the emission from the brightest quasars, and we speculate that fuelling from hot gas may be this mechanism.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9801013}, -author = {Cattaneo, Andrea}, -doi = {10.1046/j.1365-8711.2001.04259.x}, -eprint = {9801013}, -isbn = {1872-7549 (Electronic)\r0166-4328 (Linking)}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Quasars: general}, -month = {mar}, -number = {1}, -pages = {128--140}, -pmid = {20633579}, -primaryClass = {astro-ph}, -title = {{Quasars and galaxy formation}}, -volume = {324}, -year = {2001} -} -@article{Szomoru2011a, -abstract = {We use ultra-deep Hubble Space Telescope Wide Field Camera 3/infrared imaging of the Hubble Ultra Deep Field to investigate the rest-frame optical morphologies of a mass-selected sample of galaxies at z ∼ 2. We find a large variety of galaxy morphologies, ranging from large, blue, disk-like galaxies to compact, red, early-type galaxies. We derive rest-frame u - g color profiles for these galaxies and show that most z ∼ 2galaxies in our sample have negative color gradients such that their cores are red. Although these color gradients may partly be caused by radial variations in dust content, they point to the existence of older stellar populations in the centers of z ∼ 2galaxies. This result is consistent with an "inside-out" scenario of galaxy growth. We find that the median color gradient is fairly constant with redshift: ($\Delta$(u - g rest)/$\Delta$(log r))median = -0.47, -0.33, and -0.46 for z ∼ 2, z ∼ 1, and z = 0, respectively. Using structural parameters derived from surface brightness profiles we confirm that at z ∼ 2 galaxy morphology correlates well with specific star formation rate. At the same mass, star-forming galaxies have larger effective radii, bluer rest-frame u - g colors, and lower S{\'{e}}rsic indices than quiescent galaxies. These correlations are very similar to those at lower redshift, suggesting that the relations that give rise to the Hubble sequence at z = 0 are already in place for massive galaxies at this early epoch. {\textcopyright}2011. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1106.1641}, -author = {Szomoru, Daniel and Franx, Marijn and Bouwens, Rychard J and {Van Dokkum}, Pieter G and Labb{\'{e}}, Ivo and Illingworth, Garth D and Trenti, Michele}, -doi = {10.1088/2041-8205/735/1/L22}, -eprint = {1106.1641}, -isbn = {2041-8205}, -issn = {20418205}, -journal = {Astrophysical Journal Letters}, -keywords = {cosmology: observations,galaxies: evolution,galaxies: formation,galaxies: high-redshift}, -number = {1}, -title = {{Morphological evolution of galaxies from ultra-deep hubble space telescope wide field camera 3 imaging: The hubble sequence at z ∼ 2}}, -url = {http://arxiv.org/abs/1106.1641%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/2041-8205/735/1/L22}, -volume = {735}, -year = {2011} -} -@article{Schombert2015a, -abstract = {Using isophotal radius correlations for a sample of Two Micron All Sky Survey ellipticals, we have constructed a series of template surface brightness profiles to describe the profile shapes of ellipticals as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that ellipticals are weakly nonhomologous with respect to structure. Through comparison to the templates, it is discovered that ellipticals are divided into two families: those well matched to the templates, and a second class of ellipticals with distinctly shallower profile slopes. We refer to this second type of ellipticals as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D ellipticals cover the same range of luminosity, size, and kinematics as normal ellipticals, but maintain a signature of recent equal-mass dry mergers. We propose that normal ellipticals grow after an initial dissipation formation era by accretion of low-mass companions as outlined in hierarchical formation scenarios, while D ellipticals are the result of later equal-mass mergers producing shallow luminosity profiles.}, -archivePrefix = {arXiv}, -arxivId = {1509.08381}, -author = {Schombert, James M}, -doi = {10.1088/0004-6256/150/5/162}, -eprint = {1509.08381}, -isbn = {doi:10.1088/0004-6256/150/5/162}, -issn = {00046256}, -journal = {Astronomical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: photometry,galaxies: structure}, -number = {5}, -pages = {162}, -publisher = {IOP Publishing}, -title = {{The structure of galaxies. III. Two structural families of ellipticals}}, -url = {http://dx.doi.org/10.1088/0004-6256/150/5/162}, -volume = {150}, -year = {2015} -} -@article{Fea, -author = {By, Llustrated}, -keywords = {pee r}, -number = {1987}, -pages = {3--6}, -title = {{P 2 P 2 P 2}}, -volume = {93}, -year = {2009} -} -@article{Gomez2016, -abstract = {It has been shown that a self-gravitating system of massive keV fermions in thermodynamic equilibrium correctly describes the dark matter (DM) distribution in galactic halos (from dwarf to spiral and elliptical galaxies) and that, at the same time, it predicts a denser quantum core towards the center of the configuration. Such a quantum core, for a fermion mass in the range of 50 keVmc2345 keV, can be an alternative interpretation of the central compact object in Sgr A∗, traditionally assumed to be a black hole (BH). We present in this work the gravitational lensing properties of this novel DM configuration in nearby Milky-Way-like spiral galaxies. We describe the lensing effects of the pure DM component both on halo scales, where we compare them to the effects of the Navarro-Frenk-White and the nonsingular isothermal sphere DM models, and near the galaxy center, where we compare them with the effects of a Schwarzschild BH. For the particle mass leading to the most compact DM core, mc2≈102 keV, we draw the following conclusions. At distances r20 pc from the center of the lens the effect of the central object on the lensing properties is negligible. However, we show that measurements of the deflection angle produced by the DM distribution in the outer region at a few kpc, together with rotation curve data, could help to discriminate between different DM models. In the inner regions 10-6r20 pc, the lensing effects of a DM quantum core alternative to the BH scenario becomes a theme of an analysis of unprecedented precision which is challenging for current technological developments. We show that at distances ∼10-4 pc strong lensing effects, such as multiple images and Einstein rings, may occur. Large differences in the deflection angle produced by a DM central core and a central BH appear at distances r10-6 pc; in this regime the weak-field formalism is no longer applicable and the exact general-relativistic formula has to be used for the deflection angle which may become bigger than 2$\pi$. An important difference in comparison to BHs is in the fact that quantum DM cores do not show a photon sphere; this implies that they do not cast a shadow (if they are transparent). Similar conclusions apply to the other DM distributions for other fermion masses in the above-specified range and for other galaxy types.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1610.03442}, -author = {G{\'{o}}mez, L Gabriel and Arg{\"{u}}elles, C R and Perlick, Volker and Rueda, J A and Ruffini, R}, -doi = {10.1103/PhysRevD.94.123004}, -eprint = {1610.03442}, -issn = {24700029}, -journal = {Physical Review D}, -keywords = {central compact object,dark matter,fermions,halo- galaxy,lens model}, -number = {12}, -pages = {1--10}, -title = {{Strong lensing by fermionic dark matter in galaxies}}, -volume = {94}, -year = {2016} -} -@article{Jackson2008, -abstract = {A complete manual search has been carried out of the list of 285 423 objects, nearly all of them galaxies, identified in the Cosmic Evolution Survey (COSMOS) field that are brighter than I = 25. Two certain and one highly probable new gravitational lenses are found, in addition to the lenses and candidate lens systems previously found by Faure et al. A further list of 112 candidate lens systems is presented. Few of these are likely to be true gravitational lens systems, most being star-forming rings or pairs of companion galaxies. It is possible to examine of order 106 objects by eye in a reasonable time, although reliable detection of lenses by such methods is likely to be possible only with high-resolution data. The loss of completeness involved in a rapid search is estimated as up to a factor of 2, depending on the morphology of the lens candidate. {\textcopyright} 2008 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0806.3693}, -author = {Jackson, Neal}, -doi = {10.1111/j.1365-2966.2008.13629.x}, -eprint = {0806.3693}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Jackson2008SLCandidiates.pdf:pdf}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Gravitational lensing}, -number = {3}, -pages = {1311--1318}, -title = {{Gravitational lenses and lens candidates identified from the COSMOS field}}, -volume = {389}, -year = {2008} -} -@article{Dutton12018, -abstract = {We use cosmological hydrodynamical galaxy formation simulations from the NIHAO project to investigate the impact of the threshold for star formation on the response of the dark matter (DM) halo to baryonic processes. The fiducial NIHAO threshold, n=10[cm-3], results in strong expansion of the DM halo in galaxies with stellar masses in the range 107.5 ≤ Mstar ≤ 109.5 M⊙. We find that lower thresholds such as n = 0.1 (as employed by the EAGLE/APOSTLE and Illustris/AURIGA projects) do not result in significant halo expansion at any mass scale. Halo expansion driven by supernova feedback requires significant fluctuations in the local gas fraction on sub-dynamical times (i.e. ≤50 Myr at galaxy half-light radii), which are themselves caused by variability in the star formation rate. At one per cent of the virial radius, simulations with n = 10 have gas fractions of ∼0.2 and variations of ∼0.1, while n = 0.1 simulations have order of magnitude lower gas fractions and hence do not expand the halo. The observed DM circular velocities of nearby dwarf galaxies are inconsistent with CDM simulations with n = 0.1 and n = 1, but in a reasonable agreement with n = 10. Star formation rates are more variable for higher n, lower galaxy masses, and when star formation is measured on shorter time-scales. For example, simulations with n = 10 have up to 0.4 dex higher scatter in specific star formation rates than simulations with n = 0.1. Thus observationally constraining the sub-grid model for star formation, and hence the nature of DM, should be possible in the near future.}, -archivePrefix = {arXiv}, -arxivId = {1811.10625}, -author = {Dutton, Aaron A. and MacCi{\`{o}}, Andrea V. and Buck, Tobias and Dixon, Keri L. and Blank, Marvin and Obreja, Aura}, -doi = {10.1093/mnras/stz889}, -eprint = {1811.10625}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Dutton et al. - 2019 - NIHAO XX The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,galaxies: formation,galaxies: kinematics and dynamics,galaxies: structure,methods: numerical}, -number = {1}, -pages = {655--671}, -title = {{NIHAO XX: The impact of the star formation threshold on the cusp-core transformation of cold dark matter haloes}}, -url = {http://arxiv.org/abs/1811.10625%0Ahttp://dx.doi.org/10.1093/mnras/stz889}, -volume = {486}, -year = {2019} -} -@techreport{Biretta2005, -abstract = {Hot pixels provide a potentially useful probe of CTE effects, as they can be used to mea-sure effects at the smallest scales --at single pixel level. Herein we outline a method of using the tails on hot pixels to quantify CTE effects, and apply it to CTE tails in WFPC2 dark frames. As we show, many of the behaviors associated with photometric CTE are also found for hot pixel tails including the dependences on CCD row, epoch, and target bright-ness. The brightness distribution of the tails are well fit by a sum of exponential decays with scale-lengths of 0.6, 6, and 96 pixels, with the vast majority of the counts being in the longest decay component. The integrated counts in the tail are nearly equal to the expected photometric CTE, suggesting these tails are in fact the photometric deficit. We also find significant tails near row zero (y=0), and show these tails would cause effects quantitatively similar to the " long vs. short " effect. Finally we show evidence for chip-to-chip differences in CTE with WF4 having the least CTE.}, -author = {Biretta, J and Kozhurina-Platais, V}, -booktitle = {Space Telescope WFPC2 Instrument Science Report}, -keywords = {HST,Hubble Space Telescope,Space Telescope Science Institute,WFC3,Wide Field Camera 3}, -month = {jul}, -pages = {1--23}, -title = {{Hot Pixels as a Probe of WFPC2 CTE Effects}}, -year = {2005} -} -@article{Huang2013a, -abstract = {Motivated by recent developments in our understanding of the formation and evolution of massive galaxies, we explore the detailed photometric structure of a representative sample of 94 bright, nearby elliptical galaxies, using high-quality optical images from the Carnegie-Irvine Galaxy Survey. The sample spans a range of environments and stellar masses, from M* = 10{\^{}}{\{}10.2{\}} to 10{\^{}}{\{}12.0{\}} solar mass. We exploit the unique capabilities of two-dimensional image decomposition to explore the possibility that local elliptical galaxies may contain photometrically distinct substructure that can shed light on their evolutionary history. Compared with the traditional one-dimensional approach, these two-dimensional models are capable of consistently recovering the surface brightness distribution and the systematic radial variation of geometric information at the same time. Contrary to conventional perception, we find that the global light distribution of the majority ({\textgreater}75{\%}) of elliptical galaxies is not well described by a single Sersic function. Instead, we propose that local elliptical galaxies generically contain three subcomponents: a compact (R{\_}e {\textless}1 kpc) inner component with luminosity fraction f {\$\sim${}} 0.1-0.15; an intermediate-scale (R{\_}e {\$\sim${}} 2.5 kpc) middle component with f {\$\sim${}} 0.2-0.25; and a dominant (f = 0.6), extended (R{\_}e {\$\sim${}} 10 kpc) outer envelope. All subcomponents have average Sersic indices n {\$\sim${}} 1-2, significantly lower than the values typically obtained from single-component fits. The individual subcomponents follow well-defined photometric scaling relations and the stellar mass-size relation. We discuss the physical nature of the substructures and their implications for the formation of massive elliptical galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1212.2639}, -author = {Huang, Song and Ho, Luis C and Peng, Chien Y and Li, Zhao Yu and Barth, Aaron J}, -doi = {10.1088/0004-637X/766/1/47}, -eprint = {1212.2639}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: formation,galaxies: photometry,galaxies: structure}, -number = {1}, -title = {{The Carnegie-Irvine Galaxy Survey. Iii. the three-component structure of nearby elliptical galaxies}}, -volume = {766}, -year = {2013} -} -@article{Donghia2010, -abstract = {We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10{\%} of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within {\$\sim${}}30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 109 M sun and a factor of 3 at 107 M sun. The most massive subhalos with 1010 M sun survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo.}, -archivePrefix = {arXiv}, -arxivId = {0907.3482}, -author = {D'Onghia, Elena and Springel, Volker and Hernquist, Lars and Keres, Dusan}, -doi = {10.1088/0004-637X/709/2/1138}, -eprint = {0907.3482}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxy: disk,Galaxy: formation}, -month = {feb}, -number = {2}, -pages = {1138--1147}, -title = {{Substructure depletion in the milky way halo by the disk}}, -url = {http://adsabs.harvard.edu/abs/2010ApJ...709.1138D}, -volume = {709}, -year = {2010} -} -@article{Barazza2008, -abstract = {We present a study of large-scale bars in the local Universe, based on a large sample of {\$\sim${}}3692 galaxies, with -18.5 {\textless}= M{\_}g {\textless} -22.0 mag and redshift 0.01 {\textless}= z {\textless} 0.03, drawn from the SDSS. Our sample includes many galaxies that are disk-dominated and of late Hubble types. Both color cuts and Sersic cuts yield a similar sample of {\$\sim${}}2000 disk galaxies. We characterize bars and disks by ellipse-fitting r-band images and applying quantitative criteria. After excluding highly inclined ({\textgreater}60 degrees) systems, we find the following results. (1) The optical r-band fraction (f{\_}opt-r) of barred galaxies is {\$\sim${}}48{\%}-52{\%}. (2) When galaxies are separated according to normalized half light radius (r{\_}e/R{\_}24), a remarkable result is seen: f{\_}opt-r rises sharply, from {\$\sim${}}40{\%} in galaxies that have small r{\_}e/R{\_}24 and visually appear to host prominent bulges, to {\$\sim${}}70{\%} for galaxies that have large r{\_}e/R{\_}24 and appear disk-dominated. (3) f{\_}opt-r rises for galaxies with bluer colors and higher central surface brightness. A weaker rise is seen toward lower masses. (4) We find that {\$\sim${}}20{\%} of our sample of disk galaxies appear to be ``quasi-bulgeless''. (5) If we restrict our sample to bright galaxies and only consider bars that are strong (ellipticity {\textgreater}=0.4) and large enough (semi-major axis {\textgreater}=1.5 kpc) to be reliably characterized via ellipse-fitting out to z{\$\sim${}}0.8, we get an optical r-band fraction for strong bars f{\_}opt-s of {\$\sim${}}34{\%}. This value is higher only by a modest factor of 1.4, compared to the value of {\$\sim${}}24{\%}+-4{\%} reported at z{\$\sim${}}0.7-1.0. If one assumes that the increasing obscuration by dust and star formation over z{\$\sim${}}0 to 1.0 causes a further artificial loss of bars, the data even allow for a constant or rising fraction of strong bars with redshift.}, -archivePrefix = {arXiv}, -arxivId = {0802.3961}, -author = {Johnson, Crockett}, -doi = {10.2307/3616804}, -eprint = {0802.3961}, -issn = {00255572}, -journal = {The Mathematical Gazette}, -keywords = {Astrophysics}, -number = {407}, -pages = {17}, -title = {{A Construction for a Regular Heptagon}}, -url = {http://arxiv.org/abs/0802.3961}, -volume = {59}, -year = {2007} -} -@article{Targett2013, -abstract = {We have exploited the Hubble Space Telescope (HST) Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) J and H-band Wide Field Camera 3 (WFC3)/infrared (IR) imaging to study the properties of (sub-)millimetre galaxies within the Great Observatories Origins Deep Survey South (GOODS-South) field. After using the deep radio (Very Large Array 1.4 GHz) and Spitzer (Infrared Array Camera 8 $\mu$m) imaging to identify galaxy counterparts for the (sub-)millimetre sources, we have then utilized the new CANDELS WFC3/IR imaging in two ways. First, the addition of new deep near-IR photometry from both HST and (at K band) the VLT to the existing GOODS-South data base has enabled us to derive improved photometric redshifts and stellar masses, confirming that the (sub-)millimetre sources are massive (〈M*〉 = 2.2 × 1011 ± 0.2Mȯ) galaxies at z ≃ 1-3. Secondly, we have exploited the depth and resolution of the WFC3/IR imaging to determine the sizes and morphologies of the galaxies at rest-frame optical wavelengths $\lambda$rest > 4000 {\AA}. Specifically, we have fitted two-dimensional axisymmetric galaxy models to the WFC3/IR images, varying luminosity, axial ratio, half-light radius r1/2 and S{\'{e}}rsic index n. Crucially, the wavelength and depth of the WFC3/IR imaging enables modelling of the mass-dominant galaxy, rather than the blue high surface-brightness features which often dominate optical (rest-frame ultraviolet) images of (sub-)millimetre galaxies, and can confuse visual morphological classification. As a result of this analysis, we find that >95 per cent of the rest-frame optical light in almost all of the (sub-)millimetre galaxies is well described by either a single exponential disc (n ≃ 1), or a multiple-component system in which the dominant constituent is disc like. We demonstrate that this conclusion is completely consistent with the results of recent high-quality groundbased K-band imaging sampling even longer rest-frame wavelengths, and explain why it is so. These massive disc galaxies are reasonably extended (〈r1/2〉 = 4.5 ± 0.5 kpc; median r1/2 = 4.0 kpc), consistent with the sizes of other massive star-forming discs at z ≃ 2. In many cases, we find evidence of blue clumps within the sources, with the mass-dominant disc component becoming more significant at longer wavelengths. Finally, only a minority of the sources show evidence for a major galaxy-galaxy interaction. Taken together, these results support the view that most (sub-)millimetre galaxies at z ≃ 2 are simply the most extreme examples of normal star-forming galaxies at that era. Interestingly, the only two bulge-dominated galaxies are also the two lowest redshift sources in the sample (z ≃ 1), a result which may reflect the structural evolution of high-mass galaxies in general. {\textcopyright} 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1208.3464}, -author = {Targett, T. A. and Dunlop, J. S. and Cirasuolo, M. and McLure, R. J. and Bruce, V. A. and Fontana, A. and Galametz, A. and Paris, D. and Dav{\'{e}}, R. and Dekel, A. and Faber, S. M. and Ferguson, H. C. and Grogin, N. A. and Kartaltepe, J. S. and Kocevski, D. D. and Koekemoer, A. M. and Kurczynski, P. and Lai, K. and Lotz, J.}, -doi = {10.1093/mnras/stt482}, -eprint = {1208.3464}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: active,Galaxies: evolution,Galaxies: fundamental parameters,Galaxies: starburst,Infrared: galaxies}, -number = {3}, -pages = {2012--2042}, -title = {{The properties of (sub-)millimetre-selected galaxies as revealed by CANDELS HST WFC3/IR imaging in GOODS-south}}, -volume = {432}, -year = {2013} -} -@article{Murray2013a, -abstract = {Pocket-pumping is an established technique for identifying the locations of charge trapping sites within the transport channels of CCDs. Various parameters of the pumping process can be manipulated to increase the efficiency, or allow characterisation of the trap sites effective during nominal operating modes. A CCD273 was irradiated in a triangular region by protons to a 10 MeV equivalent fluence of 1.2E9 p.cm-2, ensuring a suitably low trap density for the development of an automated trap recognition algorithm. X-rays of 5, 898 eV were incident on the CCD above the region irradiated with the triangle, such that events could be analysed having passed through an increasing length of irradiated silicon and hence number of trapping sites as a function of column number. Here we present the relationship between the number of traps identified by pocket pumping within the parallel transport channels of a CCD273 and the amount of signal that is deferred by the trapping process during readout. {\textcopyright} 2013 SPIE.}, -author = {Murray, Neil J. and Burt, David J. and Hall, David and Holland, Andrew D.}, -doi = {10.1117/12.2024826}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Murray et al. - 2013 - The relationship between pumped traps and signal loss in buried channel CCDs(2).pdf:pdf}, -isbn = {9780819497109}, -issn = {0277786X}, -journal = {UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VI}, -keywords = {ccd,cic,cte,eper,euclid vis,fpr,multi-level,pocket pumping,trap pumping,tri-level}, -number = {0}, -pages = {88600H}, -title = {{The relationship between pumped traps and signal loss in buried channel CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2024826}, -volume = {8860}, -year = {2013} -} -@article{Emcee, -abstract = {We introduce a stable, well tested Python implementation of the affine-invariant ensemble sampler for Markov chain Monte Carlo (MCMC) proposed by Goodman {\&} Weare (2010). The code is open source and has already been used in several published projects in the astrophysics literature. The algorithm behind emcee has several advantages over traditional MCMC sampling methods and it has excellent performance as measured by the autocorrelation time (or function calls per independent sample). One major advantage of the algorithm is that it requires hand-tuning of only 1 or 2 parameters compared to {\$}\backslashsim N{\^{}}2{\$} for a traditional algorithm in an N-dimensional parameter space. In this document, we describe the algorithm and the details of our implementation and API. Exploiting the parallelism of the ensemble method, emcee permits any user to take advantage of multiple CPU cores without extra effort. The code is available online at http://dan.iel.fm/emcee under the MIT License.}, -archivePrefix = {arXiv}, -arxivId = {1202.3665}, -author = {Foreman-Mackey, Daniel and Hogg, David W and Lang, Dustin and Goodman, Jonathan}, -doi = {10.1086/670067}, -eprint = {1202.3665}, -issn = {00046280}, -journal = {Publications of the Astronomical Society of the Pacific}, -number = {925}, -pages = {306--312}, -title = {{emcee : The MCMC Hammer }}, -volume = {125}, -year = {2013} -} -@article{Mandelbaum2018, -abstract = {We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58 arcsec in the i band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including an {\$\sim${}}10 per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally,we check the sensitivity of our shear calibration estimates to other cutsmade on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalogue are controlled at the 1 per cent level.}, -archivePrefix = {arXiv}, -arxivId = {1710.00885}, -author = {Mandelbaum, Rachel and Lanusse, Fran{\c{c}}ois and Leauthaud, Alexie and Armstrong, Robert and Simet, Melanie and Miyatake, Hironao and Meyers, Joshua E and Bosch, James and Murata, Ryoma and Miyazaki, Satoshi and Tanaka, Masayuki}, -doi = {10.1093/mnras/sty2420}, -eprint = {1710.00885}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Gravitational lensing: weak,Methods: data analysis,Methods: numerical,Techniques: image processing}, -number = {3}, -pages = {3170--3195}, -title = {{Weak lensing shear calibration with simulations of the HSC survey}}, -volume = {481}, -year = {2018} -} -@article{Scipy2020, -author = {Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and van der Walt, St{\'{e}}fan J and Brett, Matthew and Wilson, Joshua and {Jarrod Millman}, K and Mayorov, Nikolay and Nelson, Andrew R.$\sim$J. and Jones, Eric and Kern, Robert and Larson, Eric and Carey, C J and Polat, \.Ilhan and Feng, Yu and Moore, Eric W and Vand erPlas, Jake and Laxalde, Denis and Perktold, Josef and Cimrman, Robert and Henriksen, Ian and Quintero, E.$\sim$A. and Harris, Charles R and Archibald, Anne M and Ribeiro, Ant{\^{o}}nio H and Pedregosa, Fabian and van Mulbregt, Paul and Contributors, SciPy 1. 0}, -doi = {https://doi.org/10.1038/s41592-019-0686-2}, -journal = {Nature Methods}, -pages = {261--272}, -title = {{SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python}}, -volume = {17}, -year = {2020} -} -@article{Wang2018b, -abstract = {We explore the isothermal total density profiles of early-type galaxies (ETGs) in the IllustrisTNG simulation. For the selected 559 ETGs at z = 0 with stellar masses {\$}10{\^{}}{\{}10.7{\}}\backslash, \backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot {\}} \backslashleqslant M{\_}{\{}\backslashast {\}} \backslashleqslant 10{\^{}}{\{}11.9{\}}\backslash, \backslashmathrm{\{}M{\}}{\_}{\{}\backslashodot {\}}{\$}, the total power-law slope has a mean of 〈$\gamma$′〉 = 2.011 ± 0.007 and a scatter of {\$}\backslashsigma {\_}{\{}\backslashgamma {\^{}}{\{}\backslashprime {\}}{\}} = 0.171{\$} over the radial range 0.4–4 times the stellar half-mass radius. Several correlations between $\gamma$′ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction, and in situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduces many correlation trends, and in particular, $\gamma$′ is almost constant with redshift below z = 2. Through analysing IllustrisTNG model variations, we show that black hole kinetic winds are crucial to lowering $\gamma$′ and matching observed galaxy correlations. The effects of stellar winds on $\gamma$′ are subdominant compared to active galactic nucleus (AGN) feedback, and differ due to the presence of AGN feedback from previous works. The density profiles of the ETG dark matter haloes are well described by steeper than NFW profiles, and they are steeper in the full physics (FP) run than their counterparts in the dark matter-only (DMO) run. Their inner density slopes anticorrelate (remain constant) with the halo mass in the FP (DMO) run, and anticorrelate with the halo concentration parameter c200 in both the types of runs. The dark matter haloes of low-mass ETGs are contracted whereas high-mass ETGs are expanded, suggesting that variations in the total density profile occur through the different halo responses to baryons.}, -archivePrefix = {arXiv}, -arxivId = {1811.06545}, -author = {Wang, Yunchong and Vogelsberger, Mark and Xu, Dandan and Mao, Shude and Springel, Volker and Li, Hui and Barnes, David and Hernquist, Lars and Pillepich, Annalisa and Marinacci, Federico and Pakmor, R{\"{u}}ediger and Weinberger, Rainer and Torrey, Paul}, -doi = {10.1093/mnras/stz3348}, -eprint = {1811.06545}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cd,elliptical and lenticular,evolution,formation,galaxies,kine-,matics and dynamics,stellar content}, -number = {4}, -pages = {5188--5215}, -title = {{Early-type galaxy density profiles from IllustrisTNG – I. Galaxy correlations and the impact of baryons}}, -url = {http://arxiv.org/abs/1811.06545}, -volume = {491}, -year = {2020} -} -@article{Sales2012a, -abstract = {The major morphological features of a galaxy are thought to be determined by the assembly history and net spin of its surrounding dark halo. In the simplest scenario, disc galaxies form predominantly in haloes with high angular momentum and quiet recent assembly history, whereas spheroids are the slowly rotating remnants of repeated merging events. We explore these assumptions using 100 systems with halo masses similar to that of the Milky Way, identified in a series of cosmological gasdynamical simulations: the Galaxies-Intergalactic Medium Interaction Calculation (gimic). At z= 0, the simulated galaxies exhibit a wide variety of morphologies, from dispersion-dominated spheroids to pure disc galaxies. Surprisingly, these morphological features are very poorly correlated with their halo properties: discs form in haloes with high and low net spin, and mergers play a negligible role in the formation of spheroids, whose stars form primarily in situ. With hindsight, this weak correlation between halo and galaxy properties is unsurprising given that a minority of the available baryons (∼40 per cent) end up in galaxies. More important to morphology is the coherent alignment of the angular momentum of baryons that accrete over time to form a galaxy. Spheroids tend to form when the spin of newly accreted gas is misaligned with that of the extant galaxy, leading to the episodic formation of stars with different kinematics that cancel out the net rotation of the system. Discs, on the other hand, form out of gas that flows in with similar angular momentum to that of earlier accreted material. Gas accretion from a hot corona thus favours disc formation, whereas gas that flows 'cold', often along separate, misaligned filaments, favours the formation of spheroids. In this scenario, many spheroids consist of the superposition of stellar components with distinct kinematics, age and metallicity, an arrangement that might survive to the present day given the paucity of major mergers. Since angular momentum is acquired largely at turnaround, morphology depends on the early interplay between the tidal field and the shape of the material destined to form a galaxy. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1112.2220}, -author = {Sales, Laura V and Navarro, Julio F and Theuns, Tom and Schaye, Joop and White, Simon D M and Frenk, Carlos S and Crain, Robert A and {Dalla Vecchia}, Claudio}, -doi = {10.1111/j.1365-2966.2012.20975.x}, -eprint = {1112.2220}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxy: formation,Galaxy: kinematics and dynamics,Galaxy: structure}, -number = {2}, -pages = {1544--1555}, -title = {{The origin of discs and spheroids in simulated galaxies}}, -volume = {423}, -year = {2012} -} -@article{Grant2006, -abstract = {Soon after launch, the Advanced CCD Imaging Spectrometer (ACIS), one of the focal plane instruments on the Chandra X-ray Observatory, suffered radiation damage from exposure to soft protons during passages through the Earth's radiation belts. The primary effect of the damage was to increase the charge transfer inefficiency (CTI) of the eight front illuminated CCDs by more than two orders of magnitude. The ACIS instrument team is continuing to study the properties of the damage with an emphasis on developing techniques to mitigate CTI and spectral resolution degradation. We present the initial temperature dependence of ACIS CTI from -120 to -60 degrees Celsius and the current temperature dependence after more than six years of continuing slow radiation damage. We use the change of shape of the temperature dependence to speculate on the nature of the damaging particles.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0606178}, -author = {Grant, C. E. and Bautz, M. W. and Kissel, S. E. and LaMarr, B. and Prigozhin, G. Y.}, -doi = {10.1117/12.672019}, -eprint = {0606178}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Grant et al. - 2006 - Temperature dependence of charge transfer inefficiency in Chandra X-ray CCDs.pdf:pdf}, -isbn = {0819463418}, -issn = {0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy II}, -keywords = {acis,chandra,charge coupled devices,charge transfer inefficiency,radiation damage}, -pages = {62761O}, -primaryClass = {astro-ph}, -title = {{Temperature dependence of charge transfer inefficiency in Chandra X-ray CCDs}}, -url = {http://arxiv.org/abs/astro-ph/0606178%0Ahttp://dx.doi.org/10.1117/12.672019}, -volume = {6276}, -year = {2006} -} -@article{Li2018a, -abstract = {We investigate the discrepancy between the two-dimensional projected lensing mass and the dynam- ical mass for an ensemble of 97 strong gravitational lensing systems discovered by the Sloan Lens ACS (SLACS) Survey, the BOSS Emission-Line Lens Survey (BELLS), and the BELLS for GALaxy-Ly{\{}$\backslash$alpha{\}} EmitteR sYs- tems (BELLS GALLERY) Survey. We fit the lensing data to obtain the Einstein mass, and use the velocity dispersion of the lensing galaxies provided by the Sloan Digital Sky Survey (SDSS) to get the projected dynamical mass within the Einstein radius by assuming the power-law mass approximation. The discrepancy is found to be obvious and quantified by Bayesian analysis. For the singular isothermal sphere (SIS) mass model, we obtain that the Einstein mass is 20.7{\%} more than the dynamical mass, and the discrepancy increases with the redshift of the lensing galaxies. For more general power-law mass model, the discrepancy still exists within 1{\{}$\backslash$sigma{\}} credible region. The main reason of the the discrepancy could be mass contamination, including all invisible masses along the line of sight. In addition, the measurement errors and the approximation of the mass models could lead to part of the discrepancy.}, -archivePrefix = {arXiv}, -arxivId = {1803.00819}, -author = {Li, Rui and Wang, Jiancheng and Shu, Yiping and Xu, Zhaoyi}, -doi = {10.3847/1538-4357/aaab50}, -eprint = {1803.00819}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {64}, -title = {{The Discrepancy between Einstein Mass and Dynamical Mass for SIS and Power-law Mass Models}}, -url = {http://arxiv.org/abs/1803.00819%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aaab50}, -volume = {855}, -year = {2018} -} -@article{Greene2015, -abstract = {We examine stellar population gradients in ∼100 massive early-type galaxies spanning 180 {\textless} $\sigma$∗ {\textless} 370 km s-1 and MK of -22.5 to -26.5 mag, observed as part of the MASSIVE survey. Using integral-field spectroscopy from the Mitchell Spectrograph on the 2.7 m telescope at McDonald Observatory, we create stacked spectra as a function of radius for galaxies binned by their stellar velocity dispersion, stellar mass, and group richness. With excellent sampling at the highest stellar mass, we examine radial trends in stellar population properties extending to beyond twice the effective radius (∼2.5 Re). Specifically, we examine trends in age, metallicity, and abundance ratios of Mg, C, N, and Ca, and discuss the implications for star formation histories and elemental yields. At a fixed physical radius of 3-6 kpc (the likely size of the galaxy cores formed at high redshift), stellar age and [$\alpha$/Fe] increase with increasing $\sigma$∗ and depend only weakly on stellar mass, as we might expect if denser galaxies form their central cores earlier and faster. If we instead focus on 1-1.5 Re, the trends in abundance and abundance ratio are washed out, as might be expected if the stars at large radius were accreted by smaller galaxies. Finally, we show that when controlling for $\sigma$∗, there are only very subtle differences in stellar population properties or gradients as a function of group richness; even at large radius, internal properties matter more than environment in determining star formation history.}, -archivePrefix = {arXiv}, -arxivId = {1504.02483}, -author = {Greene, Jenny E and Janish, Ryan and Ma, Chung Pei and McConnell, Nicholas J and Blakeslee, John P and Thomas, Jens and Murphy, Jeremy D}, -doi = {10.1088/0004-637X/807/1/11}, -eprint = {1504.02483}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {cD,galaxies: elliptical and lenticular,galaxies: evolution,galaxies: kinematics and dynamics,galaxies: stellar content}, -number = {1}, -title = {{the Massive Survey. Ii. Stellar Population Trends Out To Large Radius in Massive Early-Type Galaxies}}, -url = {http://arxiv.org/abs/1504.02483}, -volume = {807}, -year = {2015} -} -@article{Pota2013, -abstract = {We present a spectrophotometric survey of 2522 extragalactic globular clusters (GCs) around 12 early-type galaxies, nine of which have not been published previously. Combining spacebased and multicolour wide-field ground-based imaging, with spectra from the Keck/DEep Imaging Multi-Object Spectrograph (DEIMOS) instrument, we obtain an average of 160 GC radial velocities per galaxy, with a high-velocity precision of $\sim$15 km s-1 per GC. After studying the photometric properties of the GC systems, such as their spatial and colour distributions, we focus on the kinematics of metal-poor (blue) and metal-rich (red) GC subpopulations to an average distance of $\sim$8 effective radii from the galaxy centre. Our results show that for some systems the bimodality in GC colour is also present in GC kinematics. The kinematics of the red GC subpopulations are strongly coupled with the host galaxy stellar kinematics. The blue GC subpopulations are more dominated by random motions, especially in the outer regions, and decoupled from the red GCs. Peculiar GC kinematic profiles are seen in some galaxies: the blue GCs in NGC 821 rotate along the galaxy minor axis, whereas the GC system of the lenticulargalaxy NGC 7457 appears to be strongly rotation supported in the outer region. We supplement our galaxy sample with data from the literature and carry out a number of tests to study the kinematic differences between the two GC subpopulations. We confirm that the GC kinematics are coupled with the hostgalaxy properties and find that the velocity kurtosis and the slope of their velocity dispersion profiles are different between the two GC subpopulations in more massive galaxies.{\textcopyright} 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1209.4351}, -author = {Pota, Vincenzo and Forbes, Duncan A. and Romanowsky, Aaron J. and Brodie, Jean P. and Spitler, Lee R. and Strader, Jay and Foster, Caroline and Arnold, Jacob A. and Benson, Andrew and Blom, Christina and Hargis, Jonathan R. and Rhode, Katherine L. and Usher, Christopher}, -doi = {10.1093/mnras/sts029}, -eprint = {1209.4351}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Evolution-galaxies,General,General-galaxies,Globular clusters,Kinematics and dynamics-galaxies,Star clusters}, -number = {1}, -pages = {389--420}, -title = {{The SLUGGS Survey: Kinematics for over 2500 globular clusters in 12 early-type galaxies}}, -volume = {428}, -year = {2013} -} -@article{Mei2009, -abstract = {We apply detailed observations of the color-magnitude relation (CMR) with the Advanced Camera for Surveys on the Hubble Space Telescope to study galaxy evolution in eight clusters at z 1. The early-type red sequence is well defined and elliptical and lenticular galaxies lie on similar CMRs. We analyze CMR parameters - scatter, slope, and zero point - as a function of redshift, galaxy properties and cluster mass. For bright galaxies (MB < -21 mag), the CMR scatter of the elliptical population in cluster cores is smaller than that of the S0 population, although the two become similar at faint magnitudes (MB > - 21 mag). While the bright S0 population consistently shows larger scatter than the ellipticals, the scatter of the latter increases in the peripheral cluster regions. If we interpret these results as due to age differences, bright elliptical galaxies in cluster cores are, on average, older than S0 galaxies and peripheral elliptical galaxies (by about 0.5 Gyr, using a simple, single-burst solar metallicity stellar population model). The CMR zero point, slope, and scatter in the (U - B)z=0 rest-frame show no significant evolution out to redshift z 1.3 or significant dependence on cluster mass. Two of our clusters display CMR zero points that are redder (by 2$\sigma$) than the average (U - B)z=0 of our sample. We also analyze the fraction of morphological early-type and late-type galaxies on the red sequence. We find that, while in the majority of the clusters most (80% to 90%) of the CMR population is composed of early-type galaxies, in the highest-redshift, low-mass cluster of our sample, the CMR late-type/early-type fractions are similar (50%), with most of the late-type population composed of galaxies classified as S0/a. This trend is not correlated with the cluster's X-ray luminosity, or with its velocity dispersion, and could be a real evolution with redshift. {\textcopyright} 2009. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {0810.1917}, -author = {Mei, Simona and Holden, Brad P. and Blakeslee, John P. and Ford, Holland C. and Franx, Marijn and Homeier, Nicole L. and Illingworth, Garth D. and Jee, Myungkook J. and Overzier, Roderik and Postman, Marc and Rosati, Piero and {Van Der Wel}, Arjen and Bartlett, James G.}, -doi = {10.1088/0004-637X/690/1/42}, -eprint = {0810.1917}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Galaxies: clusters: general,Galaxies: elliptical and lenticular, cD,Galaxies: evolution}, -month = {jan}, -number = {1}, -pages = {42--68}, -title = {{Evolution of the color-magnitude relation in galaxy clusters at z ∼ 1 from the ACS intermediate redshift cluster survey}}, -url = {http://stacks.iop.org/0004-637X/690/i=1/a=42?key=crossref.7b7332474db54e3be81ff5bbe4952e0d}, -volume = {690}, -year = {2009} -} -@article{Greene2017, -abstract = {We study 379 central and 159 satellite early-type galaxies with two-dimensional kinematics from the integral-field survey Mapping Nearby Galaxies at APO (MaNGA) to determine how their angular momentum content depends on stellar and halo mass. Using the Yang et. al. (2007) group catalog, we identify central and satellite galaxies in groups with halo masses in the range 10{\^{}}12.5 h{\^{}}-1 M{\_}sun {\textless} M{\_}200b {\textless} 10{\^{}}15 h{\^{}}-1 M{\_}sun. As in previous work, we see a sharp dependence on stellar mass, in the sense that {\$\sim${}} 70{\%} of galaxies with stellar mass M{\_}* {\textgreater} 10{\^{}}11 h{\^{}}-2 M{\_}sun tend to have very little rotation, while nearly all galaxies at lower mass show some net rotation. The {\$\sim${}} 30{\%} of high-mass galaxies that have significant rotation do not stand out in other galaxy properties except for a higher incidence of ionized gas emission. Our data are consistent with recent simulation results suggesting that major merging and gas accretion have more impact on the rotational support of lower-mass galaxies. When carefully matching the stellar mass distributions, we find no residual differences in angular momentum content between satellite and central galaxies at the 20$\backslash${\%} level. Similarly, at fixed mass, galaxies have consistent rotation properties across a wide range of halo mass. However, we find that errors in classification of centrals and satellites with group finders systematically lowers differences between satellite and central galaxies at a level that is comparable to current measurement uncertainties. To improve constraints, the impact of group finding methods will have to be forward modeled via mock catalogs.}, -archivePrefix = {arXiv}, -arxivId = {1708.07845}, -author = {Greene, J E and Leauthaud, A and Emsellem, E and Ge, J and Arag{\'{o}}n-Salamanca, A and Greco, J and Lin, Y.-T. and Mao, S and Masters, K and Merrifield, M and More, S and Okabe, N and Schneider, D P and Thomas, D and Wake, D A and Pan, K and Bizyaev, D and Oravetz, D and Simmons, A and Yan, R and van den Bosch, F}, -doi = {10.3847/1538-4357/aa9bde}, -eprint = {1708.07845}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {1}, -pages = {36}, -title = {{SDSS-IV MaNGA: Uncovering the Angular Momentum Content of Central and Satellite Early-type Galaxies}}, -url = {http://arxiv.org/abs/1708.07845%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/1538-4357/aa9bde}, -volume = {852}, -year = {2018} -} -@article{VanDerWel2012, -abstract = {We present global structural parameter measurements of 109,533 unique, H F160W-selected objects from the CANDELS multi-cycle treasury program. S{\'{e}}rsic model fits for these objects are produced with GALFIT in all available near-infrared filters (H F160W, J F125W and, for a subset, Y F105W). The parameters of the best-fitting S{\'{e}}rsic models (total magnitude, half-light radius, S{\'{e}}rsic index, axis ratio, and position angle) are made public, along with newly constructed point-spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties, we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements - to 10{\%} or better - of all structural parameters can typically be obtained for galaxies with H F160W {\textless} 23, with comparable fidelity for basic size and shape measurements for galaxies to H F160W ∼ 24.5. {\textcopyright}2012. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {1211.6954}, -author = {{Van Der Wel}, A and Bell, E F and H{\"{a}}ussler, B and McGrath, E J and Chang, Yu Yen and Guo, Yicheng and McIntosh, D H and Rix, H W and Barden, M and Cheung, E and Faber, S M and Ferguson, H C and Galametz, A and Grogin, N A and Hartley, W and Kartaltepe, J S and Kocevski, D D and Koekemoer, A M and Lotz, J and Mozena, M and Peth, M A and Peng, Chien Y}, -doi = {10.1088/0067-0049/203/2/24}, -eprint = {1211.6954}, -isbn = {0067-0049}, -issn = {00670049}, -journal = {Astrophysical Journal, Supplement Series}, -keywords = {catalogs,galaxies: high-redshift,galaxies: statistics,galaxies: structure surveys}, -number = {2}, -title = {{Structural parameters of galaxies in candels}}, -volume = {203}, -year = {2012} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the haloes' virial radius while describing the infalling matter via fluxes through a spherical shell; we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP first described in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one and two points statistics.The infall takes place preferentially in the plane perpendicular to the direction defined by the halo's spin. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be {\$\sim${}}15 {\%}. The substructures have their spin orthogonal to their velocity vector in the halo's rest frame at a level of about 5{\%}, suggestive of an image of a flow along filamentary structures which provides an explanation for the measured anisotropy. We conclude that a halo does not see its environment as an isotropic perturbation, investigate how the anisotropy is propagated inwards using perturbation theory, and discuss briefly implications for weak lensing, warps and the thickness of galactic disks.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D and Pichon, C and Colombi, S}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Pillepich2017, -abstract = {We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multimode feedback. In this paper, we give a comprehensive description of the physical and numerical advances that form the core of the IllustrisTNG (The Next Generation) framework.We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black-hole-driven kinetic feedback at low accretion rates, magnetohydrodynamics and improvements to the numerical scheme. Using a suite of (25Mpc h-1)3 cosmological boxes, we assess the outcome of the new model at our fiducial resolution. The presence of a selfconsistently amplified magnetic field is shown to have an important impact on the stellar content of 1012M⊙ haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low-mass end of the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {1703.02970}, -author = {Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R{\"{u}}diger and Hernquist, Lars and Torrey, Paul and Vogelsberger, Mark and Weinberger, Rainer and Marinacci, Federico}, -doi = {10.1093/mnras/stx2656}, -eprint = {1703.02970}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Pillepich et al. - 2018 - Simulating galaxy formation with the IllustrisTNG model.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {4077--4106}, -title = {{Simulating galaxy formation with the IllustrisTNG model}}, -url = {http://arxiv.org/abs/1703.02970%0Ahttp://dx.doi.org/10.1093/mnras/stx2656}, -volume = {473}, -year = {2018} -} -@article{Schaller2015c, -abstract = {We investigate the internal structure and density profiles of haloes of mass 1010-1014 M&sun; in the Evolution and Assembly of Galaxies and their Environment (EAGLE) simulations. These follow the formation of galaxies in a Lambda cold dark matter Universe and include a treatment of the baryon physics thought to be relevant. The EAGLE simulations reproduce the observed present-day galaxy stellar mass function, as well as many other properties of the galaxy population as a function of time. We find significant differences between the masses of haloes in the EAGLE simulations and in simulations that follow only the dark matter component. Nevertheless, haloes are well described by the Navarro-Frenk-White density profile at radii larger than ˜5 per cent of the virial radius but, closer to the centre, the presence of stars can produce cuspier profiles. Central enhancements in the total mass profile are most important in haloes of mass 1012-1013 M&sun;, where the stellar fraction peaks. Over the radial range where they are well resolved, the resulting galaxy rotation curves are in very good agreement with observational data for galaxies with stellar mass M* < 5 × 1010 M&sun;. We present an empirical fitting function that describes the total mass profiles and show that its parameters are strongly correlated with halo mass.}, -archivePrefix = {arXiv}, -arxivId = {1409.8617}, -author = {Schaller, M. and Frenk, C. S. and Bower, R. G. and Theuns, T. and Jenkins, A. and Schaye, J. and Crain, R. A. and Furlong, M. and {Dalla Vecchia}, C. and McCarthy, I. G.}, -doi = {10.1093/mnras/stv1067}, -eprint = {1409.8617}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {cosmology: theory,dark matter,large-scale structure of Universe}, -number = {2}, -pages = {1247--1267}, -title = {{Baryon effects on the internal structure of CDM haloes in the EAGLE simulations}}, -url = {http://adsabs.harvard.edu/abs/2014arXiv1409.8617S}, -volume = {451}, -year = {2015} -} -@article{Johnston2016, -abstract = {With the availability of large integral-field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, how galaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present BUDDI, a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GalfitM, a modified form of Galfit which can fit multi-waveband images simultaneously. The benefit of this technique over traditional multi-waveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the SDSS-IV Mapping Nearby Galaxies at APO (MaNGA) survey with redshifts z{\textless}0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec FWHM and field of view of {\textgreater}22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from the MaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data.}, -archivePrefix = {arXiv}, -arxivId = {1611.00609}, -author = {Johnston, Evelyn J and H{\"{a}}u{\ss}ler, Boris and Arag{\'{o}}n-Salamanca, Alfonso and Merrifield, Michael R and Bamford, Steven and Bershady, Matthew A and Bundy, Kevin and Drory, Niv and Fu, Hai and Law, David and Nitschelm, Christian and Thomas, Daniel and Lopes, Alexandre Roman and Wake, David and Yan, Renbin}, -doi = {10.1093/mnras/stw2823}, -eprint = {1611.00609}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: bulges,Galaxies: evolution,Galaxies: formation,Galaxies: stellar content,Galaxies: structure}, -number = {2}, -pages = {2317--2341}, -title = {{SDSS-IV MaNGA: Bulge-disc decomposition of IFU data cubes (BUDDI)}}, -url = {http://arxiv.org/abs/1611.00609%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw2823}, -volume = {465}, -year = {2017} -} -@article{Baugh1996, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9602085}, -author = {Baugh, C. M. and Cole, S. and Frenk, C. S.}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Baugh, Cole, Frenk - 1996 - Evolution of the Bubble sequence in hierarchical models for galaxy formation(2).pdf:pdf}, -isbn = {0612410986}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function, mass function}, -number = {4}, -pages = {1361--1378}, -primaryClass = {astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -volume = {283}, -year = {1996} -} -@article{Barnabe2009b, -abstract = {We apply the joint lensing and dynamics code for the analysis of early-type galaxies, 'Combined Algorithm for Unified Lensing and Dynamics ReconstructiON (cauldron)', to a rotating N-body stellar system with dark matter halo which significantly violates the two major assumptions of the method, i.e. axial symmetry supported by a two-integral distribution function. The goal is to study how cauldron performs in an extreme case, and to determine which galaxy properties can still be robustly recovered. Three data sets, corresponding to orthogonal lines of sight, are generated from the N-body system and analysed with the identical procedure followed in the study of real lens galaxies, adopting an axisymmetric power-law total density distribution. We find that several global properties of the N-body system are recovered with remarkable accuracy, despite the fact that the adopted power-law model is too simple to account for the lack of symmetry of the true density distribution. In particular, the logarithmic slope of the total density distribution is robustly recovered to within less than 10 per cent (with the exception of the ill-constrained very inner regions), the inferred angle-averaged radial profile of the total mass closely follows the true distribution, and the dark matter fraction of the system (inside the effective radius) is correctly determined within ∼10 per cent of the total mass. Unless the line-of-sight direction is almost parallel to the total angular momentum vector of the system, reliably recovered quantities also include the angular momentum, the V/$\sigma$ ratio and the anisotropy parameter $\delta$. We conclude that the cauldron code can be safely and effectively applied to real early-type lens galaxies, also providing reliable information for the systems that depart significantly from the method's assumptions. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0808.3916}, -author = {Barnab{\`{e}}, Matteo and Nipoti, Carlo and Koopmans, L{\'{e}}on V.E. and Vegetti, Simona and Ciotti, Luca}, -doi = {10.1111/j.1365-2966.2008.14208.x}, -eprint = {0808.3916}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: kinematics and dynamics,Galaxies: structure,Gravitational lensing,Methods: N-body simulations}, -month = {mar}, -number = {4}, -pages = {1114--1126}, -title = {{Crash-testing the cauldron code for joint lensing and dynamics analysis of early-type galaxies}}, -volume = {393}, -year = {2009} -} -@article{Barnabe2011, -abstract = {We combine in a self-consistent way the constraints from both gravitational lensing and stellar kinematics to perform a detailed investigation of the internal mass distribution, amount of dark matter, and dynamical structure of the 16 early-type lens galaxies from the Sloan Lens ACS Survey (SLACS Survey), at z= 0.08-0.33, for which both Hubble Space Telescope/Advanced camera for Surveys and NICMOS high-resolution imaging and Very Large Telescope VIMOS integral-field spectroscopy are available. Based on this data set, we analyse the inner regions of the galaxies, that is, typically within one (three-dimensional) effective radius re, under the assumption of axial symmetry and by constructing dynamical models supported by two-integral stellar distribution functions. For all systems, the total mass density distribution is found to be well approximated by a simple power law (with m being the ellipsoidal radius): this profile is on average slightly super-isothermal, with a logarithmic slope 〈$\gamma$'〉= 2.074+0.043-0.041 (errors indicate the 68 per cent confidence interval) and an intrinsic scatter, and is fairly round, with an average axial ratio 〈q〉= 0.77 ± 0.04. The lower limit for the dark matter fraction (fDM) inside re ranges, in individual systems, from nearly zero to almost a half, with a median value of 12 per cent. By including stellar masses derived from stellar population synthesis models with a Salpeter initial mass function (IMF), we obtain an average fDM= 31 per cent, and the corresponding stellar profiles are physically acceptable, with the exception of two cases where they only marginally exceed the total mass profile. fDM rises to 61 per cent if, instead, a Chabrier IMF is assumed. For both IMFs, the dark matter fraction increases with the total mass of the galaxy (correlation significant at the 3$\sigma$ level). Based on the intrinsic angular momentum parameter calculated from our models, we find that the galaxies can be divided into two dynamically distinct groups, which are shown to correspond to the usual classes of the (observationally defined) slow and fast rotators. Overall, the SLACS systems are structurally and dynamically very similar to their nearby counterparts, indicating that the inner regions of early-type galaxies have undergone little, if any, evolution since redshift z≈ 0.35. {\textcopyright} 2011 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright} 2011 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1102.2261}, -author = {Barnab{\`{e}}, Matteo and Czoske, Oliver and Koopmans, L{\'{e}}on V.E. and Treu, Tommaso and Bolton, Adam S.}, -doi = {10.1111/j.1365-2966.2011.18842.x}, -eprint = {1102.2261}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Galaxies: kinematics and dynamics,Galaxies: structure,Gravitational lensing: strong}, -month = {aug}, -number = {3}, -pages = {2215--2232}, -title = {{Two-dimensional kinematics of SLACS lenses - III. Mass structure and dynamics of early-type lens galaxies beyond z ≃ 0.1}}, -volume = {415}, -year = {2011} -} -@article{Savorgnan2015a, -abstract = {In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, {\$}M{\_}{\{}BH{\}}{\$}, that had been imaged at {\$}3.6{\\sim{}}\backslashmu m{\$} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between {\$}M{\_}{\{} BH{\}}{\$} and the host spheroid (and galaxy) luminosity, {\$}L{\_}{\{}sph{\}}{\$} (and {\$}L{\_}{\{}gal{\}}{\$}), and also stellar mass, {\$}M{\_}{\{}*,sph{\}}{\$}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {\$}M{\_}{\{}BH{\}} {\textless} 10{\^{}}7{\\sim{}}M{\_}\backslashodot{\$}, and allows us to better investigate the poorly studied low-mass end of the {\$}M{\_}{\{}BH{\}} - M{\_}{\{}*,sph{\}}{\$} correlation. The bulges of early-type galaxies follow {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}1.04 \backslashpm 0.10{\}}{\$} and define a tight red sequence with intrinsic scatter {\$}\backslashepsilon = 0.43 \backslashpm 0.06{\\sim{}}dex{\$} and a median {\$}M{\_}{\{}BH{\}}/M{\_}{\{}*,sph{\}}{\$} ratio of {\$}0.68 \backslashpm 0.04\backslash{\%}{\$}, i.e.{\$\sim${}}a {\$}\backslashpm 2\backslashsigma{\$} range of 0.1-5{\%}. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {\$}M{\_}{\{}BH{\}} \backslashpropto M{\_}{\{}*,sph{\}}{\^{}}{\{}2-3{\}}{\$}, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index {\$}n{\textless}2{\$}, argued by some to be pseudo-bulges, are not offset to lower {\$}M{\_}{\{}BH{\}}{\$} from the correlation defined by the current bulge sample with {\$}n{\textgreater}2{\$}; and iii) {\$}L{\_}{\{}sph{\}}{\$} and {\$}L{\_}{\{}gal{\}}{\$} correlate equally well with {\$}M{\_}{\{}BH{\}}{\$}, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with {\$}L{\_}{\{} sph{\}}{\$} is better than that with {\$}L{\_}{\{}gal{\}}{\$}.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1511.07437}, -author = {Savorgnan, Giulia A D and Graham, Alister W and Marconi, Alessandro and Sani, Eleonora}, -doi = {10.3847/0004-637X/817/1/21}, -eprint = {1511.07437}, -issn = {1538-4357}, -title = {{Supermassive black holes and their host spheroids II. The red and blue sequence in the {\$}M{\_}{\{}\backslashrm BH{\}} - M{\_}{\{}\backslashrm *,sph{\}}{\$} diagram}}, -url = {http://arxiv.org/abs/1511.07437%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/0004-637X/817/1/21}, -year = {2015} -} -@article{Xie2014, -abstract = {Recent work has suggested that the amplitude of the size-mass relation of massive early-type galaxies (ETGs) evolves with redshift. Here we use a semi-analytical galaxy formation model to study the size evolution of massive ETGs. We find this model is able to reproduce the amplitude and slope of the relation between size and stellar mass for these galaxies, as well as its evolution. The amplitude of this relation reflects the typical compactness of dark haloes at the time when most of the stars are formed. This link between size and star formation epoch is propagated in galaxy mergers. Mergers of high or moderate mass ratio (less than 1:3) become increasingly important with increasing present day stellar mass for galaxies more massive than 1011.4M. At lower masses, low mass ratio mergers play a more important role. In situ star formation contributes more to the size growth than it does to stellar mass growth.We also find that, for ETGs identified at z = 2, minor mergers dominate subsequent growth both for stellar mass and in size, consistent with earlier theoretical results.}, -archivePrefix = {arXiv}, -arxivId = {1410.2341}, -author = {Xie, Lizhi and Guo, Qi and Cooper, Andrew P and Frenk, Carlos S and Li, Ran and Gao, Liang}, -doi = {10.1093/mnras/stu2487}, -eprint = {1410.2341}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Methods: numerical}, -number = {1}, -pages = {636--645}, -title = {{The size evolution of elliptical galaxies}}, -url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stu2487}, -volume = {447}, -year = {2015} -} -@article{Geometryeg, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(7).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Siverd2009, -abstract = {We identify, categorize, and quantify alignment effects among host and satellite galaxies using a spectroscopically-confirmed, low-redshift (z<0.23) galaxy sample from the Sloan Digital Sky Survey Data Release 6. Consistent with other recent findings, we find that satellite galaxies (SGs) of red, centrally concentrated (elliptical) host galaxies (HGs) with radial velocity separation |Delta_V|<600 km/s preferentially reside near the projected major axes of their HGs. Among these, this preference is strongest for highly concentrated, red SGs. We find that fractional anisotropy increases with decreasing \Delta_V and Delta_R and is nearly 40% greater among the closest SGs (Delta_R<250 kpc/h) relative to more distant (Delta_R>500 kpc/h) SGs. For highly concentrated SGs at small (<300 kpc/h) projected separation, we observe a strong radial (hostward) alignment signal in isophotal position angles (PAs) due to isophotal twisting and contamination that is not present when using galaxy model PAs. Among objects for which both isophotal and galaxy model PAs agree to <15 degrees, this elongation signal is significantly weaker. We also investigate the "Holmberg Effect," a well-known result wherein nearby (<40 kpc/h) SGs of large, inclined spiral HGs were seen to preferentially reside near the minor axes of their HGs. Survey limitations preclude a strict test of this effect using only SDSS spectroscopic galaxies. By adopting a looser set of cuts than those of Holmberg's study, we recover a comparable preference among faint blue SGs for the HG minor axis at marginal significance ($\sim$3 sigma). We conclude that several types of alignment likely exist among different galaxy populations, but that the observed nature and strength of alignment trends depend sensitively on both selection criteria and on the method used to determine galaxy orientation.}, -archivePrefix = {arXiv}, -arxivId = {0903.2264}, -author = {Siverd, R. J. and Ryden, B. S. and Gaudi, B. S.}, -eprint = {0903.2264}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Siverd, Ryden, Gaudi - 2009 - Galaxy Orientation and Alignment Effects in the SDSS DR6.pdf:pdf}, -journal = {arXiv}, -pages = {1--58}, -title = {{Galaxy Orientation and Alignment Effects in the SDSS DR6}}, -url = {http://arxiv.org/abs/0903.2264}, -volume = {astro-ph.G}, -year = {2009} -} -@article{Velliscig2015, -abstract = {We report the alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE (Evolution and Assembly of GaLaxies and their Environments) and cosmo-OWLS(Over- Whelmingly Large Simulations) simulations. The combination of these state-of-the-art hydrodynamical cosmological simulations enables us to span four orders of magnitude in halo mass (11 ≤ log10(M200/[h-1M⊙]) ≤ 15), a wide radial range (-2.3 ≤ log10(r/[h-1 Mpc]) ≤ 1.3) and redshifts 0 ≤ z ≤ 1. The shape parameters of the dark matter, stellar and hot gas distributions follow qualitatively similar trends: they become more aspherical (and triaxial) with increasing halo mass, radius, and redshift. We measure the misalignment of the baryonic components (hot gas and stars) of galaxies with their host halo as a function of halo mass, radius, redshift, and galaxy type (centrals versus satellites and early- versus late-type). Overall, galaxies align well with the local distribution of the total (mostly dark) matter. However, the stellar distributions on galactic scales exhibit a median misalignment of about 45-50 deg with respect to their host haloes. This misalignment is reduced to 25-30 deg in the most massive haloes (13 ≤ log10(M200/[h-1M⊙]) ≤ 15). Half of the disc galaxies in the EAGLE simulations have a misalignment angle with respect to their host haloes larger than 40 deg. We present fitting functions and tabulated values for the probability distribution of galaxy-halo misalignment to enable a straightforward inclusion of our results into models of galaxy formations based on purely collisionless N-body simulations.}, -archivePrefix = {arXiv}, -arxivId = {1504.04025}, -author = {Velliscig, Marco and Cacciato, Marcello and Schaye, Joop and Crain, Robert A. and Bower, Richard G. and {Van Daalen}, Marcel P. and Vecchia, Claudio Dalla and Frenk, Carlos S. and Furlong, Michelle and McCarthy, I. G. and Schaller, Matthieu and Theuns, Tom}, -doi = {10.1093/mnras/stv1690}, -eprint = {1504.04025}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: Theory,Galaxies: Formation,Galaxies: Haloes,Large-scale structure of Universe}, -month = {oct}, -number = {1}, -pages = {721--738}, -title = {{The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations}}, -volume = {453}, -year = {2015} -} -@article{Governato2015, -abstract = {We use high-resolution Hydro+N-Body cosmological simulations to compare the assembly and evolution of a small field dwarf (stellar mass {\$\sim${}}106-7 M⊙, total mass 1010 M⊙) in $\Lambda$-dominated cold dark matter (CDM) and 2 keV warm dark matter (WDM) cosmologies. We find that star formation (SF) in the WDM model is reduced and delayed by 1-2 Gyr relative to the CDM model, independently of the details of SF and feedback. Independent of the dark matter (DM) model, but proportionally to the SF efficiency, gas outflows lower the central mass density through 'dynamical heating', such that all realizations have circular velocities {\textless} 20 km s-1 at 500 pc, in agreement with local kinematic constraints. As a result of dynamical heating, older stars are less centrally concentrated than younger stars, similar to stellar population gradients observed in nearby dwarf galaxies. Introducing an important diagnostic of SF and feedback models, we translate our simulations into artificial colour- magnitude diagrams and star formation histories (SFHs) in order to directly compare to available observations. The simulated galaxies formed most of their stars in many {\$\sim${}}10 Myr long bursts. The CDM galaxy has a global SFH, HI abundance and Fe/H and alpha-elements distribution well matched to current observations of dwarf galaxies. These results highlight the importance of directly including 'baryon physics' in simulations when (1) comparing predictions of galaxy formation models with the kinematics and number density of local dwarf galaxies and (2) differentiating between CDM and non-standard models with different DM or power spectra.}, -archivePrefix = {arXiv}, -arxivId = {1407.0022}, -author = {Governato, F and Weisz, D and Pontzen, A and Loebman, S and Reed, D and Brooks, A M and Behroozi, P and Christensen, C and Madau, P and Mayer, L and Shen, S and Walker, M and Quinn, T and Keller, B W and Wadsley, J}, -doi = {10.1093/mnras/stu2720}, -eprint = {1407.0022}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: formation,Galaxy: formation,Hydrodynamics}, -number = {1}, -pages = {792--803}, -title = {{Faint dwarfs as a test of DM models: WDM versus CDM}}, -volume = {448}, -year = {2015} -} -@article{Tonini2006, -abstract = {We propose that angular momentum transfer from the baryons to the dark matter (DM) during the early stages of galaxy formation can flatten the halo inner density profile and modify the halo dynamics. We compute the phase-space distribution function of DM halos that corresponds to the density and anisotropy profiles obtained from N-body simulations in the concordance cosmology. We then describe an injection of angular momentum into the halo by modifying the distribution function and show that the system evolves into a new equilibrium configuration; the latter features a constant central density and a tangentially dominated anisotropy profile in the inner regions, while the structure is nearly unchanged beyond 10% of the virial radius. Then we propose a toy model to account for such a halo evolution, based on the angular momentum exchange due to dynamical friction; at the epoch of galaxy formation this is efficiently exerted by the DM onto the gas clouds spiralling down the potential well. The comparison between the angular momentum profile gained by the halo through dynamical friction and that provided by the perturbed distribution function reveals a surprising similarity, hinting at the reliability of the process. {\textcopyright} 2006. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0603051}, -author = {Tonini, C. and Lapi, A. and Salucci, P.}, -doi = {10.1086/506431}, -eprint = {0603051}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Formation,Galaxies: Halos,Galaxies: Kinematics and Dynamics,Galaxies: Structure}, -month = {oct}, -number = {2}, -pages = {591--598}, -primaryClass = {astro-ph}, -title = {{Angular Momentum Transfer in Dark Matter Halos: Erasing the Cusp}}, -url = {http://stacks.iop.org/0004-637X/649/i=2/a=591}, -volume = {649}, -year = {2006} -} -@article{Schneider1992, -abstract = {The behavior of the gravitational lens mapping near cusps is studied, both analytically and numerically, paying particular attention to magnification probabilities. We demonstrate that the three images of a point source inside a cusp satisfy the relation that the sum of the magnifications of the two images with the same parity equals, up to a sign, the magnification of the third image (of opposite parity). This property will then be used to show that the asymptotic magnification cross section for point sources, in the limit mus approaching infinity, derived previously for folds only, is also valid in the presence of cusps. The next order term of such an expansion, which is due to sources just outside of cusps, is derived. We apply these relations to a special gravitational lens models and show that these asymptotic relations are indeed very good approximations for the large-mus cross sections. For the study of the magnification of extended sources near cusps, we generalize the ray-shooting method to allow for very small sources. The magnification cross-sections for extended sources are then compared to those for point sources. A magnification contour plot for extended sources near a cusp is obtained.}, -author = {SCHNEIDER, P and WEISS, A}, -issn = {0004-6361}, -journal = {Astronomy and astrophysics (Berlin. Print)}, -keywords = {Analytical method,Aumento,Cartograf{\'{i}}a,Cartographie,Cartography,Catastrophe theory,Cusp,C{\'{u}}spide,Ecuaci{\'{o}}n,Equation,Gravitational lens,Grossissement,Lente gravitacional,Lentille gravitationnelle,Magnification,M{\'{e}}thode analytique,M{\'{e}}thode num{\'{e}}rique,M{\'{e}}todo anal{\'{i}}tico,M{\'{e}}todo num{\'{e}}rico,Numerical method,Point rebroussement,Teor{\'{i}}a cat{\'{a}}strofe,Th{\'{e}}orie catastrophe}, -month = {jul}, -number = {1}, -pages = {1--13}, -title = {{The gravitational lens equation near cusps}}, -url = {http://adsabs.harvard.edu/abs/1992A&A...260....1S}, -volume = {260}, -year = {1992} -} -@article{Carlson1992, -abstract = {The particle physics nature of dark matter (DM) can leave an imprint on the structure of Universe. If DM has a sizable cross section for self-interactions (much larger than the typical weak scale cross section), this can affect the density profiles of DM halos. Moreover, there exist long-standing discrepancies on small scales between astrophysical observations and predictions from N-body simulations of collisionless DM, which suggests that DM may be self-interacting. Here, we review these discrepancies, we discuss the particle physics implications of self-interacting DM, and we show that DM self-interactions have interesting implications for direct and indirect detection searches. {\textcopyright} 2014 AIP Publishing LLC.}, -archivePrefix = {arXiv}, -arxivId = {1711.02970}, -author = {Tulin, Sean}, -doi = {10.1063/1.4883420}, -eprint = {1711.02970}, -isbn = {9780735412385}, -issn = {15517616}, -journal = {AIP Conference Proceedings}, -keywords = {Dark Matter}, -pages = {121--127}, -pmid = {22759447}, -title = {{Self-interacting dark matter}}, -url = {http://arxiv.org/abs/astro-ph/0006344}, -volume = {1604}, -year = {2014} -} -@article{Holl2012, -abstract = {Gaia, the next astrometric mission of the European Space Agency, will use a camera composed of 106 CCDs to collect multiple observations for one billion stars. The astrometric core solution of Gaia will use the estimated location of the stellar images on the CCDs to derive the astrometric parameters (position, parallax and proper motion) of the stars. The Gaia CCDs will suffer from charge transfer inefficiency (CTI) mainly caused by radiation damage. CTI is expected to significantly degrade the quality of the collected images which ultimately affects the astrometric accuracy of Gaia. This paper is the second and last in a study aiming at characterizing and quantifying the impact of CCD radiation damage on Gaia astrometry. Here we focus on the effect of the image location errors induced by CTI on the astrometric solution. We apply the Gaia Astrometric Global Iterative Solution (AGIS) to simulated Gaia-like observations for 1 million stars including CTI-induced errors as described in the first paper. We show that a magnitude-dependent image location bias is propagated in the astrometric solution, biasing the estimation of the astrometric parameters as well as decreasing its precision. We demonstrate how the Gaia scanning law dictates this propagation and the ultimate sky distribution of the CTI-induced errors. The possibility of using the residuals of the astrometric solution to improve the calibration of the CTI effects is investigated. We also estimate the astrometric errors caused by (faint) disturbing stars preceding the stellar measurements on the CCDs. Finally, we show that, for single stars, the overall astrometric accuracy of Gaia can be preserved to within 10per cent of the CTI-free case for all magnitudes by appropriate modelling at the image location estimation level and using the solution residuals. {\textcopyright}2012 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2012 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1110.1547}, -author = {Holl, B and Prod'homme, T and Lindegren, L and Brown, A G A}, -doi = {10.1111/j.1365-2966.2012.20429.x}, -eprint = {1110.1547}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astrometry,Instrumentation: detectors,Methods: analytical,Methods: numerical,Space vehicles}, -number = {4}, -pages = {2786--2807}, -title = {{The impact of CCD radiation damage on Gaia astrometry - II. Effect of image location errors on the astrometric solution}}, -volume = {422}, -year = {2012} -} -@article{Berg2018, -abstract = {We report new observations of SL2SJ021737-051329, a lens system consisting of a bright arc at z=1.84435, magnified {\$\sim${}}17x by a massive galaxy at z=0.65. SL2SJ0217 is a low-mass (M {\textless}10{\^{}}9 M*), low-metallicity (Z{\$\sim${}}1/20 Z*) galaxy, with extreme star-forming conditions that produce strong nebular UV emission lines in the absence of any apparent outflows. Here we present several notable features from rest-frame UV Keck/LRIS spectroscopy: (1) Very strong narrow emission lines are measured for CIV 1548,1550, HeII 1640, OIII] 1661,1666, SiIII] 1883,1892, and CIII] 1907,1909. (2) Double-peaked LyA emission is observed with a dominant blue peak and centered near the systemic velocity. (3) The low- and high-ionization absorption features indicate very little or no outflowing gas along the sightline to the lensed galaxy. The relative emission line strengths can be reproduced with a very high-ionization, low-metallicity starburst with binaries, with the exception of He $\backslash$ii, which indicates an additional ionization source is needed. We rule out large contributions from AGN and shocks to the photoionization budget, suggesting that the emission features requiring the hardest radiation field likely result from extreme stellar populations that are beyond the capabilities of current models. Therefore, SL2S0217 serves as a template for the extreme conditions that are important for reionization and thought to be more common in the early Universe.}, -archivePrefix = {arXiv}, -arxivId = {1803.02340}, -author = {Berg, Danielle A and Erb, Dawn K and Auger, Matthew W and Pettini, Max and Brammer, Gabriel B}, -doi = {10.3847/1538-4357/aab7fa}, -eprint = {1803.02340}, -isbn = {0004-637X}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -number = {2}, -pages = {164}, -title = {{ A Window on the Earliest Star Formation: Extreme Photoionization Conditions of a High-ionization, Low-metallicity Lensed Galaxy at z ∼ 2* }}, -url = {http://arxiv.org/abs/1803.02340}, -volume = {859}, -year = {2018} -} -@article{Agustsson2007a, -abstract = {We investigate the locations of the satellites of relatively isolated host galaxies in the Sloan Digital Sky Survey and the Millennium Run simulation. Provided we use two distinct prescriptions to embed luminous galaxies within the simulated dark matter halos (ellipticals share the shapes of their halos, while disks have angular momenta that are aligned with the net angular momenta of their halos), we find a fair agreement between observation and theory. Averaged over scales rp 500 kpc, the satellites of red, high-mass hosts with low star formation rates are found preferentially near the major axes of their hosts. In contrast, the satellites of blue, low-mass hosts with low star formation rates show little to no anisotropy when averaged over the same scale. The difference between the locations of the satellites of red and blue hosts cannot be explained by the effects of interlopers in the data. Instead, it is caused primarily by marked differences in the dependence of the mean satellite location, $\phi$, on the projected distance at which the satellites are found. We also find that the locations of red, high-mass satellites with low star formation rates show considerably more anisotropy than do the locations of blue, low-mass satellites with high star formation rates. There are two contributors to this result. First, the blue satellites have only recently arrived within their hosts' halos, while the red satellites arrived in the far distant past. Second, the sample of blue satellites is heavily contaminated by interlopers, which suppresses the measured anisotropy compared to the intrinsic anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {0704.3441}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1088/0004-637X/709/2/1321}, -eprint = {0704.3441}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: dwarf,Galaxies: fundamental parameters,Galaxies: halos,Galaxies: structure}, -number = {2}, -pages = {1321--1336}, -title = {{Anisotropic locations of satellite galaxies: Clues to the orientations of galaxies within their dark matter halos}}, -url = {http://arxiv.org/abs/0704.3441%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/0004-637X/709/2/1321}, -volume = {709}, -year = {2010} -} -@article{Oosterloo2002, -author = {{Thomas A. Oosterloo, Raffaella Morganti, Elaine M. Sadler, Daniela Vergani} and Caldwell, Nelson}, -journal = {The Astronomical Journal}, -keywords = {eso 263-g48,galaxies,individual,ism,kinematics and dynamics,ngc 1947,ngc 3108,ngc 7049,ngc 7070a}, -number = {2}, -pages = {729--744}, -title = {{EXTENDED H i DISKS IN DUST LANE ELLIPTICAL GALAXIES 1 Thomas A. Oosterloo and Raffaella Morganti}}, -volume = {123}, -year = {2002} -} -@article{Michalowski2012, -abstract = {Establishing the stellar masses, and hence specific star-formation rates of submillimetre galaxies is crucial for determining the role of such objects in the cosmic history of galaxy/star formation. However, there is as yet no consensus over the typical stellar masses of submillimetre galaxies, as illustrated by the widely differing results reported from recent optical-infrared studies of submillimetre galaxies with spectroscopic redshifts z ≈ 2-3. Specifically, even for the same set of submillimetre galaxies, the reported average stellar masses have ranged over an order of magnitude, from ≈ 5 × 1010 M⊙ to ≈ 5 × 10 11 M⊙. Here we study how different methods of analysis can lead to such widely varying results. We find that, contrary to recent claims in the literature, potential contamination of IRAC 3-8 $\mu$m photometry from hot dust associated with an active nucleus is not the origin of the published discrepancies in derived stellar masses. Instead, we expose in detail how inferred stellar mass depends on assumptions made in the photometric fitting, and quantify the individual and cumulative effects of different choices of initial mass function, different "brands" of evolutionary synthesis models, and different forms of assumed star-formation history. We review current observational evidence for and against these alternatives as well as clues from the hydrodynamical simulations, and conclude that, for the most justifiable choices of these model inputs, the average stellar mass of luminous (S850 ≈ 5 mJy) submillimetre galaxies is ≈ 2 × 10 11 M⊙ to within a factor ≈ 2. We also check and confirm that this number is perfectly reasonable in the light of the latest measurements of the dynamical masses of these objects (≈ 2-6 × 10 11 M⊙ from CO (1-0) observations), and the evolving stellar mass function of the overall galaxy population. Galaxy stellar masses of this orderstar-formation rate of submillimetre galaxies is comparable to that of other star-forming galaxies at z > 2, at 2-3 Gyr-1. This supports the view that, while rare outliers may be found at any stellar mass, most submillimetre galaxies simply form the top end of the "main- sequence" of star-forming galaxies at these redshifts. Conversely, this argues strongly against the viewpoint, frequently simply asserted in the literature, that submillimetre galaxies are extreme pathological objects, of little relevance in the cosmic history of star-formation. {\textcopyright} 2012 ESO.}, -archivePrefix = {arXiv}, -arxivId = {1108.6058}, -author = {Micha{\l}owski, M. J. and Dunlop, J. S. and Cirasuolo, M. and Hjorth, J. and Hayward, C. C. and Watson, D.}, -doi = {10.1051/0004-6361/201016308}, -eprint = {1108.6058}, -issn = {14320746}, -journal = {Astronomy and Astrophysics}, -keywords = {Galaxies: ISM,Galaxies: active,Galaxies: evolution,Galaxies: high-redshift,Galaxies: starburst,Submillimeter: galaxies}, -pages = {A85}, -title = {{The stellar masses and specific star-formation rates of submillimetre galaxies}}, -url = {http://www.aanda.org/10.1051/0004-6361/201016308}, -volume = {541}, -year = {2012} -} -@article{Faure2008, -abstract = {We present the first catalog of 67 strong galaxy-galaxy lens candidates discovered in the 1.64 square degree Hubble Space Telescope COSMOS survey. Twenty of these systems display multiple images or strongly curved large arcs. Our initial search is performed by visual inspection of the data and is restricted, for practical considerations, to massive early-type lens galaxies with arcs found at radii smaller than $\sim$5''. Simple mass models are constructed for the best lens candidates and our results are compared to the strong lensing catalogs of the SLACS survey and the CASTLES database. These new strong galaxy-galaxy lensing systems constitute a valuable sample to study the mass distribution of early-type galaxies and their associated dark matter halos. We further expect this sample to play an important role in the testing of software algorithms designed to automatically search for strong gravitational lenses. From our analysis a robust lower limit is derived for the expected occurrence of strong galaxy-galaxy systems in current and future space-based wide-field imaging surveys. We expect that such surveys should uncover a large number of strong lensing systems (more than 10 systems per square degree), which will allow for a detailed statistical analysis of galaxy properties and will likely lead to constraints on models of gravitational structure formation and cosmology. The sample of strong lenses is available here: http://cosmosstronglensing.uni-hd.de/}, -archivePrefix = {arXiv}, -arxivId = {0802.2174}, -author = {Faure, Cecile and Kneib, Jean‐Paul and Covone, Giovanni and Tasca, Lidia and Leauthaud, Alexie and Capak, Peter and Jahnke, Knud and Smolcic, Vernesa and de la Torre, Sylvain and Ellis, Richard and Finoguenov, Alexis and Koekemoer, Anton and {Le Fevre}, Oliver and Massey, Richard and Mellier, Yannick and Refregier, Alexandre and Rhodes, Jason and Scoville, Nick and Schinnerer, Eva and Taylor, James and {Van Waerbeke}, Ludovic and Walcher, Jakob}, -doi = {10.1086/526426}, -eprint = {0802.2174}, -file = {:C\:/Users/Jammy/Documents/Papers/COSMOS/Faure2008SLCandidiates.pdf:pdf}, -issn = {0067-0049}, -journal = {ApJSS}, -number = {1}, -pages = {19--38}, -title = {{First Catalog of Strong Lens Candidates in the COSMOS Field}}, -volume = {176}, -year = {2008} -} -@article{RomanoDiaz2008, -abstract = {We study the central dark matter (DM) cusp evolution in cosmological galactic halos. Models with and without baryons (baryons+DM, hereafter BDM model, and pure DM, PDM model, respectively) are advanced from identical initial conditions. The DM cusp properties are contrasted by a direct comparison of pure DM and baryonic models. We find a divergent evolution between the PDM and BDM models within the inner {\$\sim${}}10 kpc region. The PDM model forms a R{\^{}}{\{}-1{\}} cusp as expected, while the DM in the BDM model forms a larger isothermal cusp R{\^{}}{\{}-2{\}} instead. The isothermal cusp is stable until z{\$\sim${}}1 when it gradually levels off. This leveling proceeds from inside out and the final density slope is shallower than -1 within the central 3 kpc (i.e., expected size of the R{\^{}}{\{}-1{\}} cusp), tending to a flat core within {\$\sim${}}2 kpc. This effect cannot be explained by a finite resolution of our code which produces only a 5{\%} difference between the gravitationally softened force and the exact Newtonian force of point masses at 1 kpc from the center. Neither is it related to the energy feedback from stellar evolution or angular momentum transfer from the bar. Instead it can be associated with the action of DM+baryon subhalos heating up the cusp region via dynamical friction and forcing the DM in the cusp to flow out and to `cool' down. The process described here is not limited to low z and can be efficient at intermediate and even high z.}, -archivePrefix = {arXiv}, -arxivId = {0808.0195}, -author = {Romano-Diaz, Emilio and Shlosman, Isaac and Hoffman, Yehuda and Heller, Clayton}, -doi = {10.1086/592687}, -eprint = {0808.0195}, -issn = {0004-637X}, -journal = {The Astrophysical Journal}, -keywords = {Cosmology: Dark Matter,Galaxies: Evolution,Galaxies: Formation,Galaxies: Halos,Galaxies: Interactions,Galaxies: Kinematics and Dynamics}, -month = {oct}, -number = {2}, -pages = {L105----L108}, -title = {{Erasing Dark Matter Cusps in Cosmological Galactic Halos with Baryons}}, -url = {http://arxiv.org/abs/0808.0195%7B%5C%25%7D0Ahttp://dx.doi.org/10.1086/592687}, -volume = {685}, -year = {2008} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S{\$}\backslash{\$}'{\{}e{\}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as {\$}M{\_}{\{}h{\}}(M{\_}{\{}*{\}}) \backslashbackslashpropto r{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}eff{\{}\backslash{\}}{\}}{\}}{\^{}}{\{}\backslashbackslasheta{\{}\backslash{\}}{\}}(M{\_}{\{}*{\}}){\$}. We find that on average, our lens galaxies have an {\$}\backslashbackslasheta = 0.42\backslashbackslashpm0.12{\$}, i.e. larger galaxies live in more massive dark matter haloes. The {\$}\backslashbackslasheta{\{}\backslash{\$}{\}} is strongest for high mass luminous red galaxies (LRGs). Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed {\$}M{\_}{\{}*{\}}{\$}, satellite galaxies have a larger {\$}\backslashbackslasheta{\{}\backslash{\$}{\}} and greater scatter in the {\$}M{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}h{\{}\backslash{\}}{\}}{\}}{\$} and {\$}r{\_}{\{}\backslashbackslashmathrm{\{}\backslash{\{}{\}}eff{\{}\backslash{\}}{\}}{\}}{\$} relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J L and Hudson, Michael J and Balogh, Michael L and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Li2016b, -abstract = {The cold dark matter (CDM) cosmological model unambiguously predicts that a large number of haloes should survive as subhaloes when they are accreted into a larger halo. TheCDMmodel would be ruled out if such substructures were shown not to exist. By contrast, if the darkmatter consists of Warm Dark Matter (WDM) particles, then below a threshold mass that depends on the particle mass far fewer substructures would be present. Finding subhaloes below a certain mass would then rule out warm particle masses below some value. Strong gravitational lensing provides a clean method to measure the subhalomass function through distortions in the structure of Einstein rings and giant arcs. Using mock lensing observations constructed from high-resolution N-body simulations, we show that measurements of approximately 100 strong lens systems with a detection limit of Mlow = 107h-1Mo˙ would clearly distinguish CDM fromWDMin the casewhere this consists of 7 keV sterile neutrinos such as those that might be responsible for the 3.5 keV X-ray emission line recently detected in galaxies and clusters.}, -archivePrefix = {arXiv}, -arxivId = {1512.06507}, -author = {Li, Ran and Frenk, Carlos S. and Cole, Shaun and Gao, Liang and Bose, Sownak and Hellwing, Wojciech A.}, -doi = {10.1093/mnras/stw939}, -eprint = {1512.06507}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Li et al. - 2016 - Constraints on the identity of the dark matter from strong gravitational lenses.pdf:pdf}, -isbn = {9781420032086}, -issn = {13652966}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies,Gravitational lensing,Haloes,Methods,Statistical,Strong}, -number = {1}, -pages = {363--372}, -pmid = {21356229}, -title = {{Constraints on the identity of the dark matter from strong gravitational lenses}}, -volume = {460}, -year = {2016} -} -@inproceedings{MartinNavarro2013, -author = {Mart\$\backslash\$'\$\backslash\$in-Navarro, I and Vazdekis, A and Bongiovanni, A and Falc{\'{o}}n-Barroso, J and Cepa, J and Cenarro, J and S{\'{a}}nchez-Bl{\'{a}}zquez, P}, -booktitle = {Highlights of Spanish Astrophysics VII}, -editor = {Guirado, J.\$\sim$C. and Lara, L.\$\sim$M. and Quilis, V and Gorgas, J}, -month = {may}, -pages = {275--280}, -title = {{Kinematical mapping of the outskirts of elliptical galaxies using the OSIRIS tunable lters at GTC: a novel approach}}, -year = {2013} -} -@article{Aubert2004, -abstract = {We measure the anisotropy of dark matter flows on small scales (∼500 kpc) in the near environment of haloes using a large set of simulations. We rely on two different approaches to quantify the anisotropy of the cosmic infall: we measure the flows at the virial radius of the haloes while describing the infalling matter via fluxes through a spherical shell; and we measure the spatial and kinematical distributions of satellites and substructures around haloes detected by the subclump finder ADAPTAHOP described for the first time in the appendix. The two methods are found to be in agreement both qualitatively and quantitatively via one- and two-point statistics. The peripheral and advected momenta are correlated with the spin of the embedded halo at levels of 30 and 50 per cent. The infall takes place preferentially in the plane perpendicular to the direction defined by the spin of the halo. We computed the excess of equatorial accretion both through rings and via a harmonic expansion of the infall. The level of anisotropy of infalling matter is found to be ∼15 per cent. The substructures have their spin orthogonal to their velocity vector in the rest frame of the halo at a level of about 5 per cent, suggestive of an image of a flow along filamentary structures, which provides an explanation for the measured anisotropy. Using a 'synthetic' stacked halo, it is shown that the positions and orientations of satellites relative to the direction of spin of the halo are not random even in projection. The average ellipticity of stacked haloes is 10 per cent, while the alignment excess in projection reaches 2 per cent. All measured correlations are fitted by a simple three-parameter model. We conclude that a halo does not see its environment as an Isotropic perturbation, we investigate how the anisotropy is propagated inwards using perturbation theory, and we discuss briefly the implications for weak lensing, warps and the thickness of galactic discs.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0402405}, -author = {Aubert, D and Pichon, C and Colombi, S}, -doi = {10.1111/j.1365-2966.2004.07883.x}, -eprint = {0402405}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation,Galaxies: haloes}, -number = {2}, -pages = {376--398}, -primaryClass = {astro-ph}, -title = {{The origin and implications of dark matter anisotropic cosmic infall on ≈ L* haloes}}, -volume = {352}, -year = {2004} -} -@article{Krist2004a, -author = {Krist, John and Hook, Richard and Tim, Tiny}, -journal = {Changes}, -number = {June}, -pages = {1--35}, -title = {{The Tiny Tim User ' s Guide}}, -url = {http://tinytim.stsci.edu/static/tinytim.pdf%7B%5C%25%7D5Cnpapers2://publication/uuid/994E8BF5-B9AC-489B-A26F-2AE8BC664FEE}, -year = {2004} -} -@article{Agustsson2007a, -abstract = {We investigate the locations of the satellites of relatively isolated host galaxies in the Sloan Digital Sky Survey and the Millennium Run simulation. Provided we use two distinct prescriptions to embed luminous galaxies within the simulated dark matter halos (ellipticals share the shapes of their halos, while disks have angular momenta that are aligned with the net angular momenta of their halos), we find a fair agreement between observation and theory. Averaged over scales rp 500 kpc, the satellites of red, high-mass hosts with low star formation rates are found preferentially near the major axes of their hosts. In contrast, the satellites of blue, low-mass hosts with low star formation rates show little to no anisotropy when averaged over the same scale. The difference between the locations of the satellites of red and blue hosts cannot be explained by the effects of interlopers in the data. Instead, it is caused primarily by marked differences in the dependence of the mean satellite location, $\phi$, on the projected distance at which the satellites are found. We also find that the locations of red, high-mass satellites with low star formation rates show considerably more anisotropy than do the locations of blue, low-mass satellites with high star formation rates. There are two contributors to this result. First, the blue satellites have only recently arrived within their hosts' halos, while the red satellites arrived in the far distant past. Second, the sample of blue satellites is heavily contaminated by interlopers, which suppresses the measured anisotropy compared to the intrinsic anisotropy.}, -archivePrefix = {arXiv}, -arxivId = {0704.3441}, -author = {Agustsson, Ingolfur and Brainerd, Tereasa G}, -doi = {10.1088/0004-637X/709/2/1321}, -eprint = {0704.3441}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {Dark matter,Galaxies: dwarf,Galaxies: fundamental parameters,Galaxies: halos,Galaxies: structure}, -number = {2}, -pages = {1321--1336}, -title = {{Anisotropic locations of satellite galaxies: Clues to the orientations of galaxies within their dark matter halos}}, -url = {http://arxiv.org/abs/0704.3441%7B%5C%25%7D0Ahttp://dx.doi.org/10.1088/0004-637X/709/2/1321}, -volume = {709}, -year = {2010} -} -@article{VandeSande2016, -abstract = {Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the high-order stellar kinematic moments h3 ($\sim$skewness) and h4 ($\sim$kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using 2D integral field data from the SAMI Galaxy Survey. A proxy for the spin parameter ($\lambda_{R_e}$) and ellipticity ($\epsilon_e$) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h3 versus $V/\sigma$ anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h3 and $V/\sigma$. Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h3 versus $V/\sigma$ signatures. We identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar $\lambda_{R_e}-\epsilon_e$ values can show distinctly different h3-$V/\sigma$ signatures. Class 5 objects are previously unidentified fast rotators that show a weak h3 versus $V/\sigma$ anti-correlation. These objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h3 versus $V/\sigma$ as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.}, -archivePrefix = {arXiv}, -arxivId = {1611.07039}, -author = {van de Sande, Jesse and Bland-Hawthorn, Joss and Fogarty, Lisa M. R. and Cortese, Luca and D'Eugenio, Francesco and Croom, Scott M. and Scott, Nicholas and Allen, James T. and Brough, Sarah and Bryant, Julia J. and Cecil, Gerald and Colless, Matthew and Couch, Warrick J. and Davies, Roger and Elahi, Pascal J. and Foster, Caroline and Goldstein, Gregory and Goodwin, Michael and Groves, Brent and Ho, I-Ting and Jeong, Hyunjin and Jones, D. Heath and Konstantopoulos, Iraklis S. and Lawrence, Jon S. and Leslie, Sarah K. and L{\'{o}}pez-S{\'{a}}nchez, {\'{A}}ngel R. and McDermid, Richard M. and McElroy, Rebecca and Medling, Anne M. and Oh, Sree and Owers, Matt S. and Richards, Samuel N. and Schaefer, Adam L. and Sharp, Rob and Sweet, Sarah M. and Taranu, Dan and Tonini, Chiara and Walcher, C. Jakob and Yi, Sukyoung K.}, -doi = {10.3847/1538-4357/835/1/104}, -eprint = {1611.07039}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Sande et al. - 2017 - the Sami Galaxy Survey Revisiting Galaxy Classification Through High-Order Stellar Kinematics.pdf:pdf}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -keywords = {cosmology,dynamics,evolution,formation,galaxies,kinematics and,observations,stellar content,structure}, -number = {1}, -pages = {104}, -title = {{the Sami Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics}}, -url = {http://arxiv.org/abs/1611.07039%0Ahttp://dx.doi.org/10.3847/1538-4357/835/1/104}, -volume = {835}, -year = {2017} -} -@article{Fleury2021, -abstract = {While most strong-gravitational-lensing systems may be roughly modelled by a single massive object between the source and the observer, in the details all the structures near the light path contribute to the observed images. These additional contributions, known as line-of-sight effects, are non-negligible in practice. This article proposes a new theoretical framework to model the line-of-sight effects, together with very promising applications at the interface of weak and strong lensing. Our approach relies on the dominant-lens approximation, where one deflector is treated as the main lens while the others are treated as perturbations. The resulting framework is technically simpler to handle than the multi-plane lensing formalism, while allowing one to consistently model any sub-critical perturbation. In particular, it is not limited to the usual external-convergence and external-shear parameterisation. As a first application, we identify a specific notion of line-of-sight shear that is not degenerate with the ellipticity of the main lens, and which could thus be extracted from strong-lensing images. This result supports and improves the recent proposal that Einstein rings might be powerful probes of cosmic shear. As a second application, we investigate the distortions of strong-lensing critical curves under line-of-sight effects, and more particularly their correlations across the sky. We find that such correlations may be used to probe, not only the large-scale structure of the Universe, but also the dark-matter halo profiles of strong lenses. This last possibility would be a key asset to improve the accuracy of the measurement of the Hubble-Lema{\^{i}}tre constant via time-delay cosmography.}, -archivePrefix = {arXiv}, -arxivId = {2104.08883}, -author = {Fleury, Pierre and Larena, Julien and Uzan, Jean Philippe}, -doi = {10.1088/1475-7516/2021/08/024}, -eprint = {2104.08883}, -file = {:C\:/Users/Jammy/Documents/Papers/Strong_Lens/Fleury2022LosShear.pdf:pdf}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {Galaxy surveys,Gravitational lensing,Weak gravitational lensing}, -number = {8}, -title = {{Line-of-sight effects in strong gravitational lensing}}, -volume = {2021}, -year = {2021} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z {\textgreater} 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright}2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R G and Benson, A J and Malbon, R and Helly, J C and Frenk, C S and Baugh, C M and Cole, S and Lacey, C G}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -month = {aug}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -volume = {370}, -year = {2006} -} -@article{Tabor2016, -abstract = {To ascertain whether photometric decompositions of galaxies into bulges and disks are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disk components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to CALIFA integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component, and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed.}, -archivePrefix = {arXiv}, -arxivId = {1612.01957}, -author = {Tabor, Martha and Merrifield, Michael and Arag{\'{o}}n-Salamanca, Alfonso and Cappellari, Michele and Bamford, Steven P and Johnston, Evelyn}, -doi = {10.1093/mnras/stw3183}, -eprint = {1612.01957}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {elliptical and lenticular,galaxies,kinematics and dynamics}, -number = {2}, -pages = {2024--2033}, -title = {{Untangling galaxy components: full spectral bulge–disc decomposition}}, -url = {http://arxiv.org/abs/1612.01957%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stw3183}, -volume = {466}, -year = {2017} -} -@article{Fornasa2013, -abstract = {The LAT-Fermi collaboration has recently reported the detection of angular power above the photon noise level in the diffuse gamma-ray background between 1 and 50 GeV. Such signal can be used to constrain a possible contribution from dark matter (DM) induced photons. We estimate the intensity and features of the angular power spectrum (APS) of this potential DM signal, for both decaying and annihilating DM candidates, by constructing template all-sky gamma-ray maps for the emission produced in the galactic halo and its substructures, as well as in extragalactic (sub)haloes. The DM distribution is given by state-of-the-art N-body simulations of cosmic structure formation, namely Millennium-II for extragalactic (sub)haloes, and Aquarius for the galactic halo and its subhaloes. We use a hybrid method of extrapolation to accountfor (sub)structures that are below the resolution limit of the simulations, allowing us to estimate the total emission all the way down to the minimal self-bound halo mass. We describe in detail the features appearing in the APS of our template maps and we estimate the effect of various uncertainties such as the value of the minimal halo mass, the fraction of substructures hosted in a halo and the shape of the DM density profile. Our results indicate that the fluctuation APS of the DM-induced emission is of the same order as the Fermi-LAT APS, suggesting that one can constrain this hypothetical emission from the comparison with the measured anisotropy. We also quantify the uncertainties affecting our results, finding 'theoretical error bands' spanning more than two orders of magnitude and dominated (for a given particle physics model) by our lack of knowledge of the abundance of low-mass (sub)haloes. {\textcopyright} 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.}, -archivePrefix = {arXiv}, -arxivId = {1207.0502}, -author = {Fornasa, Mattia and Zavala, Jes{\'{u}}s and S{\'{a}}nchez-Conde, Miguel A. and Siegal-Gaskins, Jennifer M. and Delahaye, Timur and Prada, Francisco and Vogelsberger, Mark and Zandanel, Fabio and Frenk, Carlos S.}, -doi = {10.1093/mnras/sts444}, -eprint = {1207.0502}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Astroparticle physics,Cosmology: dark matter,Gammarays: diffuse background,Methods: numerical}, -number = {2}, -pages = {1529--1553}, -title = {{Characterization of dark-matter-induced anisotropies in the diffuse gamma-ray background}}, -volume = {429}, -year = {2013} -} -@article{Geometryem, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Qi2018, -abstract = {Ultra-compact structure in radio quasars, with milliarcsecond angular sizes measured by very-long-baseline interferometry (VLBI), provides an important source of angular diameter distances that can be observed up to higher redshifts. In this paper, with the latest catalog of galactic-scale strong gravitational lensing systems and the VLBI observation of milliarcsecond compact structure in intermediate-luminosity quasars, we place constraints on the curvature of the universe through the well-known distance sum rule, without assuming any fiducial cosmological model. Assuming power-law density profiles for the total mass density of lensing galaxies ({\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashgamma{\}}{\$}), we find that, although the zero cosmic curvature is still included within {\$}2 \backslashsigma{\$} confidence level, a closed universe is seemed to be more favored in our analysis. In addition, in the framework of a more general lens model which allows the luminosity density profile {\$}\backslashrho\backslashsim r{\^{}}{\{}-\backslashalpha{\}}{\$} to be different from that of the total-mass density profile {\$}\backslashnu\backslashsim r{\^{}}{\{}-\backslashdelta{\}}{\$}, a weaker constraint on the curvature ({\$}\backslashOmega{\_}k{\textless}0.197{\$} at 68$\backslash${\%} confidence level)is obtained indicates that a more general lens model does have a significant impact on the measurement of cosmic curvature. Finally, based on the mock samples of strong gravitational lenses and quasars with the current measurement accuracy, we find that with about 16000 strong lensing events (observed by the forthcoming LSST survey) combined with the distance information provided by 500 compact uv-coverage, one can constrain the cosmic curvature with an accuracy of {\$}\backslashDelta \backslashOmega{\_}k\backslashsimeq 10{\^{}}{\{}-3{\}}{\$}, which is comparable to the precision of Planck 2015 results.}, -archivePrefix = {arXiv}, -arxivId = {1803.01990}, -author = {Qi, Jing-Zhao and Cao, Shuo and Zhang, Sixuan and Biesiada, Marek and Wu, Yan and Zhu, Zong-Hong}, -eprint = {1803.01990}, -pages = {1--8}, -title = {{A revised test of cosmic curvature at high redshifts: the distance sum rule}}, -url = {http://arxiv.org/abs/1803.01990}, -year = {2018} -} -@article{Seabroke2008, -abstract = {The Gaia satellite is a high-precision astrometry, photometry and $\backslash$nspectroscopic ESA cornerstone mission, currently scheduled for launch in$\backslash$nlate 2011. Its primary science drivers are the composition, formation$\backslash$nand evolution of the Galaxy. Gaia will not achieve its scientific$\backslash$nrequirements without detailed calibration and correction for radiation$\backslash$ndamage. Microscopic models of Gaia's CCDs are being developed to$\backslash$nsimulate the effect of radiation damage, charge trapping, which causes$\backslash$ncharge transfer inefficiency. The key to calculating the probability of$\backslash$na photoelectron being captured by a trap is the 3D electron density$\backslash$nwithin each CCD pixel. However, this has not been physically modelled$\backslash$nfor Gaia CCD pixels. In this paper, the first of a series, we motivate$\backslash$nthe need for such specialised 3D device modelling and outline how its$\backslash$nfuture results will fit into Gaia's overall radiation calibration$\backslash$nstrategy.}, -archivePrefix = {arXiv}, -arxivId = {0809.0293}, -author = {Seabroke, George and Holland, Andrew and Cropper, Mark}, -doi = {10.1117/12.790968}, -eprint = {0809.0293}, -isbn = {9780819472311}, -issn = {0277-786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy III}, -keywords = {astrometry,ccds,focal plane,gaia}, -pages = {70211P}, -title = {{Modelling radiation damage to ESA's Gaia satellite CCDs}}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.790968}, -volume = {7021}, -year = {2008} -} -@article{Iodice:2016aa, -abstract = {[Abrigded] We have started a new deep, multi-imaging survey of the Fornax cluster, dubbed Fornax Deep Survey (FDS), at the VLT Survey Telescope. In this paper we present the deep photometry inside two square degrees around the bright galaxy NGC1399 in the core of the cluster. We found a very extended and diffuse envelope surrounding the luminous galaxy NGC1399: we map the surface brightness out to 33 arcmin ($\sim$ 192 kpc) from the galaxy center and down to about 31 mag/arcsec^2 in the g band. The deep photometry allows us to detect a faint stellar bridge in the intracluster region between NGC1399 and NGC1387. By analyzing the integrated colors of this feature, we argue that it could be due to the ongoing interaction between the two galaxies, where the outer envelope of NGC1387 on its east side is stripped away. By fitting the light profile, we found that it exists a physical break radius in the total light distribution at R=10 arcmin ($\sim$58 kpc) that sets the transition region between the bright central galaxy and the outer exponential stellar halo. We discuss the main implications of this work on the build-up of the stellar halo at the center of the Fornax cluster. By comparing with the numerical simulations of the stellar halo formation for the most massive BCGs, we find that the observed stellar halo mass fraction is consistent with a halo formed through the multiple accretion of progenitors with a stellar mass in the range 10^8 - 10^11 M_sun. This might suggest that the halo of NGC1399 has also gone through a major merging event. The absence of a significant number of luminous stellar streams and tidal tails out to 192 kpc suggests that the epoch of this strong interaction goes back to an early formation epoch. Therefore, differently from the Virgo cluster, the extended stellar halo around NGC1399 is characterised by a more diffuse and well-mixed component, including the ICL.}, -archivePrefix = {arXiv}, -arxivId = {1602.02149}, -author = {Iodice, E. and Capaccioli, M. and Grado, A. and Limatola, L. and Spavone, M. and Napolitano, N. R. and Paolillo, M. and Peletier, R. F. and Cantiello, M. and Lisker, T. and Wittmann, C. and Venhola, A. and Hilker, M. and D'Abrusco, R. and Pota, V. and Schipani, P.}, -doi = {10.3847/0004-637x/820/1/42}, -eprint = {1602.02149}, -issn = {1538-4357}, -journal = {The Astrophysical Journal}, -month = {mar}, -number = {1}, -pages = {42}, -title = {{THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc}}, -url = {http://arxiv.org/abs/1602.02149%0Ahttp://dx.doi.org/10.3847/0004-637X/820/1/42}, -volume = {820}, -year = {2016} -} -@article{Hall2014a, -abstract = {Charge-Coupled Devices are the detector of choice for the focal planes of many optical and X-ray space telescopes. In recent years, EM-CCDs, SCDs and CMOS sensors have been used, or baselined, for missions in which the detection of X-ray and visible photons are key to the science goals of the mission. When placed in orbit, silicon-based detectors will suffer radiation damage as a consequence of the harsh space radiation environment, creating traps in the silicon. The radiation-induced traps will capture and release signal electrons, effectively "smearing" the image. Without correction, this smearing of the image would have major consequences on the science goals of the missions. Fitting to observed results, through careful planning of observation strategies while the radiation dose received remains low in the early stages of the mission, has previously been used to correct against the radiation damage effects. As the science goals becoming increasingly demanding, however, the correction algorithms require greater accuracy and a more physical approach is required, removing the effects of the radiation damage by modelling the trap capture and release mechanisms to a high level of detail. The drive for increasingly accurate trap parameters has led to the development of new methods of characterisation of traps in the silicon, measuring the trap properties and their effects to the single-trap level in situ. Here, we summarise the latest developments in trap characterisation techniques for n-channel and p-channel devices. ? 2014 SPIE.}, -author = {Hall, David J and Murray, Neil and Gow, Jason and Wood, Daniel and Holland, Andrew}, -doi = {10.1117/12.2055906}, -isbn = {9780819496225}, -issn = {1996756X 0277786X}, -journal = {High Energy, Optical, and Infrared Detectors for Astronomy VI}, -keywords = {CTI,Defect,Euclid,Gaia,HST,N-channel,P,[CCD}, -number = {0}, -pages = {915408}, -title = {{ In situ trap parameter studies in CCDs for space applications }}, -url = {http://proceedings.spiedigitallibrary.org/proceeding.aspx?doi=10.1117/12.2055906}, -volume = {9154}, -year = {2014} -} -@article{Hughes1998, -abstract = {In the local Universe, most galaxies are dominated by stars, with less than ten per cent of their visible mass in the form of gas. Determining when most of these stars formed is one of the central issues of observational cosmology. Optical and ultraviolet observations of high-redshift galaxies (particularly those in the Hubble Deep Field) have been interpreted as indicating that the peak of star formation occurred between redshifts of 1 and 1.5. But it is known that star formation takes place in dense clouds, and is often hidden at optical wavelengths because of extinction by dust in the clouds. Here we report a deep submillimetre-wavelength survey of the Hubble Deep Field; these wavelengths trace directly the emission from dust that has been warned by massive star-formation activity. The combined radiation of the five most significant detections accounts for 30-50 per cent of the previously unresolved background emission in this area. Four of these sources appear to be galaxies in the redshift range 2 10-1014M{\textperiodcentered} in the Evolution and Assembly of Galaxies and their Environment (EAGLE) simulations. These follow the formation of galaxies in a $\Delta$ cold dark matter Universe and include a treatment of the baryon physics thought to be relevant. The EAGLE simulations reproduce the observed present-day galaxy stellar mass function, as well as many other properties of the galaxy population as a function of time.We find significant differences between the masses of haloes in the EAGLE simulations and in simulations that follow only the dark matter component. Nevertheless, haloes are well described by the Navarro-Frenk-White density profile at radii larger than $\sim$5 per cent of the virial radius but, closer to the centre, the presence of stars can produce cuspier profiles. Central enhancements in the total mass profile are most important in haloes of mass 1012-1013M{\textperiodcentered}, where the stellar fraction peaks. Over the radial range where they are well resolved, the resulting galaxy rotation curves are in very good agreement with observational data for galaxies with stellar mass M* < 5 × 1010M{\textperiodcentered}.We present an empirical fitting function that describes the total mass profiles and show that its parameters are strongly correlated with halo mass.}, -archivePrefix = {arXiv}, -arxivId = {1409.8617}, -author = {Schaller, Matthieu and Frenk, Carlos S. and Bower, Richard G. and Theuns, Tom and Jenkins, Adrian and Schaye, Joop and Crain, Robert A. and Furlong, Michelle and Vecchia, Claudio Dalla and McCarthy, I. G.}, -doi = {10.1093/mnras/stv1067}, -eprint = {1409.8617}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Large-scale structure of universe}, -month = {aug}, -number = {2}, -pages = {1247--1267}, -title = {{Baryon effects on the internal structure of $\Delta$CDM haloes in the EAGLE simulations}}, -url = {http://adsabs.harvard.edu/abs/2014arXiv1409.8617S}, -volume = {451}, -year = {2015} -} -@article{Bayliss2017, -abstract = {We report the detection of extended Lyman-{\$}\backslashalpha{\$} emission from the host galaxy of SDSS{\$\sim${}}J2222+2745, a strongly lensed quasar at {\$}z = 2.8{\$}. Spectroscopic follow-up clearly reveals extended Lyman-{\$}\backslashalpha{\$} in emission between two images of the central active galactic nucleus (AGN). We reconstruct the lensed quasar host galaxy in the source plane by applying a strong lens model to HST imaging, and resolve spatial scales as small as {\$}\backslashsim{\$}200 parsecs. In the source plane we recover the host galaxy morphology to within a few hundred parsecs of the central AGN, and map the extended Lyman-{\$}\backslashalpha{\$} emission to its physical origin on one side of the host galaxy at radii {\$}\backslashsim{\$}0.5-2 kpc from the central AGN. There are clear morphological differences between the Lyman-{\$}\backslashalpha{\$} and rest-frame ultraviolet stellar continuum emission from the quasar host galaxy. Furthermore, the relative velocity profiles of quasar Lyman-{\$}\backslashalpha{\$}, host galaxy Lyman-{\$}\backslashalpha{\$}, and metal lines in outflowing gas reveal differences in the absorbing material affecting the AGN and host galaxy. These data indicate the presence of patchy local intervening gas in front of the central quasar and its host galaxy. This interpretation is consistent with the central luminous quasar being obscured across a substantial fraction of its surrounding solid angle, resulting in strong anisotropy in the exposure of the host galaxy to ionizing radiation from the AGN. This work demonstrates the power of strong lensing-assisted studies to probe spatial scales that are currently inaccessible by other means.}, -archivePrefix = {arXiv}, -arxivId = {1708.00453}, -author = {Bayliss, Matthew B and Sharon, Keren and Acharyya, Ayan and Gladders, Michael D and Rigby, Jane R and Bian, Fuyan and Bordoloi, Rongmon and Runnoe, Jessie and Dahle, Hakon and Kewley, Lisa and Florian, Michael and Johnson, Traci and Paterno-Mahler, Rachel}, -doi = {10.3847/2041-8213/aa831a}, -eprint = {1708.00453}, -issn = {00160032}, -keywords = {emission lines,galaxies,general,gravitational lensing,high-,quasars,strong}, -pages = {1--7}, -title = {{Spatially Resolved Patchy Lyman-{\$}\backslashalpha{\$} Emission Within the Central Kiloparsec of a Strongly Lensed Quasar Host Galaxy at z = 2.8}}, -url = {http://arxiv.org/abs/1708.00453%7B%5C%25%7D0Ahttp://dx.doi.org/10.3847/2041-8213/aa831a}, -year = {2017} -} -@article{Angulo2009, -abstract = {We use the Millennium Simulation, a large, high-resolution N-body simulation of the evolution of structure in a $\Lambda$ cold dark matter cosmology, to study the properties and fate of substructures within a large sample of dark matter haloes. We find that the subhalo mass function departs significantly from a power law at the high-mass end. We also find that the radial and angular distributions of substructures depend on subhalo mass. In particular, high-mass subhaloes tend to be less radially concentrated and to have angular distributions closer to the direction perpendicular to the spin of the host halo than their less massive counterparts. We find that mergers between subhaloes occur. These tend to be between substructures that were already dynamically associated before accretion into the main halo. For subhaloes larger than 0.001 times the mass of the host halo, it is more likely that the subhalo will merge with the central or main subhalo than with another subhalo larger than itself. For lower masses, subhalo-subhalo mergers become equally likely to mergers with the main subhalo. Our results have implications for the variation of galaxy properties with environment and for the treatment of mergers in galaxy formation models. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0810.2177}, -author = {Angulo, R. E. and Lacey, C. G. and Baugh, C. M. and Frenk, C. S.}, -doi = {10.1111/j.1365-2966.2009.15333.x}, -eprint = {0810.2177}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Dark matter,Galaxies: haloes,Galaxies: interactions}, -month = {oct}, -number = {2}, -pages = {983--995}, -title = {{The fate of substructures in cold dark matter haloes}}, -volume = {399}, -year = {2009} -} -@article{Vegetti2009b, -abstract = {A Bayesian statistical formalism is developed to quantify the level at which the mass function (dN/dm ∝ m-$\alpha$) and the projected cumulative mass fraction (f) of [cold dark matter (CDM)] substructure in strong gravitational lens galaxies, with arcs or Einstein rings, can be recovered as function of the lens survey parameters and the detection threshold of the substructure mass. The method is applied to different sets of mock data to explore a range of observational limits: (i) the number of lens galaxies in the survey; (ii) the mass threshold, Mlow, for the detection of substructures and (iii) the uncertainty of the measured substructure masses. We explore two different priors on the mass function slope: a uniform prior and a Gaussian prior with $\alpha$ = 1.90 ± 0.1. With a substructure detection threshold Mlow = 3 × 108 M⊙, the number of lenses available now (nl = 30), a true dark matter mass fraction in (CDM) substructure ≤1.0 per cent and a prior of $\alpha$ = 1.90 ± 0.1, we find that the upper limit of f can be constrained down to a level ≤1.0 per cent [95 per cent confidence level (CL)]. In the case of a uniform prior, the complete substructure mass distribution (i.e. mass fraction and slope) can only be characterized in a number of favourable cases with a large number of detected substructures. This can be achieved by an increase of the resolution and the signal-to-noise ratio of the lensed images. In the case of a Gaussian prior on $\alpha$, instead, it is always possible to set stringent constraints on both parameters. We also find that lowering the detection threshold has the largest impact on the ability to recover $\alpha$, because of the (expected) steep mass function slope. In the future, thanks to new surveys with telescopes, such as Square Kilometre Array (SKA), Large Synoptic Survey Telescope (LSST) and Joint Dark Energy Mission (JDEM) and follow-up telescopes with high-fidelity data, a significant increase in the number of known lenses (i.e. ≫104) will allow us to recover the satellite population in its completeness. For example, a sample of 200 lenses, equivalent in data quality to the Sloan Lens ACS Survey and a detection threshold of 108 M⊙, allows one to determine f = 0.5 ± 0.1 per cent (68 per cent CL) and $\alpha$ = 1.90 ± 0.2 (68 per cent CL). {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0903.4752}, -author = {Vegetti, Simona and Koopmans, L. V.E.}, -doi = {10.1111/j.1365-2966.2009.15559.x}, -eprint = {0903.4752}, -issn = {00358711}, -journal = {MNRAS}, -keywords = {Dark matter,Galaxies: haloes,Galaxies: structure,Gravitational lensing,Methods: statistical}, -month = {dec}, -number = {3}, -pages = {1583--1592}, -title = {{Statistics of mass substructure from strong gravitational lensing: Quantifying the mass fraction and mass function}}, -volume = {400}, -year = {2009} -} -@article{Bower2006, -abstract = {Recent observations of the distant Universe suggest that much of the stellar mass of bright galaxies was already in place at z > 1. This presents a challenge for models of galaxy formation because massive haloes are assembled late in the hierarchical clustering process intrinsic to the cold dark matter (CDM) cosmology. In this paper, we discuss a new implementation of the Durham semi-analytic model of galaxy formation in which feedback due to active galactic nuclei (AON) is assumed to quench cooling flows in massive haloes. This mechanism naturally creates a break in the local galaxy luminosity function at bright magnitudes. The model is implemented within the Millennium N-body simulation. The accurate dark matter merger trees and large number of realizations of the galaxy formation process enabled by this simulation result in highly accurate statistics. After adjusting the values of the physical parameters in the model by reference to the properties of the local galaxy population, we investigate the evolution of the K-band luminosity and galaxy stellar mass functions. We calculate the volume-averaged star formation rate density of the Universe as a function of redshift and the way in which this is apportioned amongst galaxies of different mass. The model robustly predicts a substantial population of massive galaxies out to redshift z ∼ 5 and a star formation rate density which rises at least out to z ∼ 2 in objects of all masses. Although observational data on these properties have been cited as evidence for 'antihierarchical' galaxy formation, we find that when AGN feedback is taken into account, the fundamentally hierarchical CDM model provides a very good match to these observations. {\textcopyright} 2006 RAS.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/0511338}, -author = {Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G.}, -doi = {10.1111/j.1365-2966.2006.10519.x}, -eprint = {0511338}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Bower et al. - 2006 - Breaking the hierarchy of galaxy formation(2).pdf:pdf}, -isbn = {0035-8711}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function}, -month = {aug}, -number = {2}, -pages = {645--655}, -primaryClass = {astro-ph}, -title = {{Breaking the hierarchy of galaxy formation}}, -volume = {370}, -year = {2006} -} -@article{Hopkins2009, -abstract = {Transformation of discs into spheroids via mergers is a well-accepted element of galaxy formation models. However, recent simulations have shown that the bulge formation is suppressed in increasingly gas-rich mergers. We investigate the global implications of these results in a cosmological framework, using independent approaches: empirical halo-occupation models (where galaxies are populated in haloes according to observations) and semi-analytic models. In both, ignoring the effects of gas in mergers leads to the overproduction of spheroids: low- and intermediate-mass galaxies are predicted to be bulge-dominated (B/T ∼ 0.5 at <10 10 M ⊙, with almost no 'bulgeless' systems), even if they have avoided major mergers. Including the different physical behaviour of gas in mergers immediately leads to a dramatic change: bulge formation is suppressed in low-mass galaxies, observed to be gas-rich (giving B/T ∼ 0.1 at <10 10 M ⊙, with a number of bulgeless galaxies in good agreement with observations). Simulations and analytic models which neglect the similarity-breaking behaviour of gas have difficulty reproducing the strong observed morphology-mass relation. However, the observed dependence of gas fractions on mass, combined with suppression of bulge formation in gas-rich mergers, naturally leads to the observed trends. Discrepancies between observations and models that ignore the role of gas increase with redshift; in models that treat gas properly, galaxies are predicted to be less bulge-dominated at high redshifts, in agreement with the observations. We discuss implications for the global bulge mass density and future observational tests. {\textcopyright} 2009 RAS.}, -archivePrefix = {arXiv}, -arxivId = {0901.4111}, -author = {Hopkins, Philip F. and Somerville, Rachel S. and Cox, Thomas J. and Hernquist, Lars and Jogee, Shardha and Kere{\v{s}}, Dusan and Ma, Chung Pei and Robertson, Brant and Stewart, Kyle}, -doi = {10.1111/j.1365-2966.2009.14983.x}, -eprint = {0901.4111}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Hopkins et al. - 2009 - The effects of gas on morphological transformation in mergers Implications for bulge and disc demographics(2).pdf:pdf}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: evolution,Galaxies: formation,Galaxies: spiral}, -number = {2}, -pages = {802--814}, -title = {{The effects of gas on morphological transformation in mergers: Implications for bulge and disc demographics}}, -volume = {397}, -year = {2009} -} -@article{Lauer2005, -abstract = {We present observations of 77 early-type galaxies imaged with the PC1 CCD of the Hubble Space Telescope (HST) WFPC2. "Nuker-law" parametric fits to the surface brightness profiles are used to classify the central structure into "core" or "power-law" forms. Core galaxies are typically rounder than power-law galaxies. Nearly all power-law galaxies with central ellipticities $\epsilon$ ≥ 0.3 have stellar disks, implying that disks are present in power-law galaxies with $\epsilon$ {\textless} 0.3 but are not visible because of unfavorable geometry. A few low-luminosity flattened core galaxies also have disks; these may be transition forms from power-law galaxies to more luminous core galaxies, which lack disks. Several core galaxies have strong isophote twists interior to their break radii, although power-law galaxies have interior twists of similar physical significance when the photometric perturbations implied by the twists are evaluated. Central color gradients are typically consistent with the envelope gradients; core galaxies have somewhat weaker color gradients than power-law galaxies. Nuclei are found in 29{\%} of the core galaxies and 60{\%} of the power-law galaxies. Nuclei are typically bluer than the surrounding galaxy. While some nuclei are associated with active galactic nuclei (AGNs), just as many are not; conversely, not all galaxies known to have a low-level AGN exhibit detectable nuclei in the broadband filters. NGC 4073 and 4382 are found to have central minima in their intrinsic starlight distributions; NGC 4382 resembles the double nucleus of M31. In general, the peak brightness location is coincident with the photocenter of the core to a typical physical scale of {\textless} 1 pc. Five galaxies, however, have centers significantly displaced from their surrounding cores; these may be unresolved asymmetric double nuclei. Finally, as noted by previous authors, central dust is visible in about half of the galaxies. The presence and strength of dust correlates with nuclear emission; thus, dust may outline gas that is falling into the central black hole. The prevalence of dust and its morphology suggest that dust clouds form, settle to the center, and disappear repeatedly on ∼ 10 8 yr timescales. We discuss the hypothesis that cores are created by the decay of a massive black hole binary formed in a merger. Apart from their brightness profiles, there are no strong differences between core galaxies and power-law galaxies that demand this scenario; however, the rounder shapes of core, their lack of disks, and their reduced color gradients may be consistent with it. {\textcopyright}2005. The American Astronomical Society. All rights reserved.}, -archivePrefix = {arXiv}, -arxivId = {arXiv:astro-ph/0412040}, -author = {Lauer, Tod R and Faber, S M and Gebhardt, Karl and Richstone, Douglas and Tremaine, Scott and Ajhar, Edward A and Aller, M C and Bender, Ralf and Dressler, Alan and Filippenko, Alexei V and Green, Richard and Grillmair, Carl J and Ho, Luis C and Kormendy, John and Magorrian, John and Pinkney, Jason and Siopis, Christos}, -doi = {10.1086/429565}, -eprint = {0412040}, -issn = {0004-6256}, -journal = {The Astronomical Journal}, -number = {5}, -pages = {2138--2185}, -primaryClass = {arXiv:astro-ph}, -title = {{ The Centers of Early-Type Galaxies with Hubble Space Telescope . V. New WFPC2 Photometry }}, -url = {http://stacks.iop.org/1538-3881/129/i=5/a=2138}, -volume = {129}, -year = {2005} -} -@article{2001ev, -author = {عامر, د. وفاء محروس}, -journal = {مجلة اسيوط للدراسات البيئة}, -pages = {43}, -title = {{No Title" المعالجة الحيوية للمولوثات البيئية}}, -volume = {العدد الحا}, -year = {2001} -} -@article{Baugh:1996aa, -abstract = {We present a model for the broad morphological distinction between the disc and spheroidal components of galaxies. Elaborating on the hierarchical clustering scheme of galaxy formation proposed by Cole et al., we assume that galaxies form stars quiescently in a disc until they are disrupted into a spheroidal configuration by mergers. Bulges and spheroids may continue to accrete gas from their hot coronae, and so they may grow discs again. Thus an individual galaxy may pass through various phases of disc or spheroid dominance during its lifetime. To distinguish between discs and spheroids we add one additional free parameter to the semi-analytic model of Cole et al., which we fix by requiring that the predicted morphological mix should match that observed locally. Assuming an $\Omega$ = 1, standard cold dark matter cosmology, we calculate formation and merging histories, and the evolution in colour, luminosity and morphology of the galaxy populations in different environments. Our model predicts that the bulges of spirals were assembled before the spheroids of ellipticals, and that the spheroids of cluster ellipticals were assembled before those of field ellipticals. About 50 per cent of ellipticals, but only about 15 per cent of spirals, have undergone a major merger during the redshift interval 0.0 ≤z ≤ 0.5. In spite of their violent formation history, elliptical galaxies turn out to have colour-magnitude diagrams with remarkably small scatter. Apart from a general blueing of the galaxy population with redshift, the colour-magnitude diagrams are remarkably similar at redshift z = 0.5 and at the present day. The morphological mix of galaxies that become rich cluster members at high redshift is dominated by spiral galaxies, due to the long time-scale for galaxy mergers compared with the time-scale for cluster assembly at high redshift. The assembly of low-redshift clusters is slower, allowing more galaxy mergers to occur in the progenitor haloes. As a result, z = 0 rich clusters become E/SO dominated, and we find a 'Butcher-Oemler' effect that becomes weaker for poorer groups at high redshift. The field luminosity function of red galaxies shows little evolution out to z ≃ 1, and the reddest galaxies at these redshifts are as bright as their local counterparts. The blue luminosity function, on the other hand, evolves rapidly with redshift, increasing its characteristic luminosity and becoming steeper at the faint end. These trends are similar to those recently observed in the Canada-France Redshift Survey. Our calculations serve to demonstrate that a simple prescription for the distinction between discs and spheroids that is compatible with hierarchical clustering goes a long way towards explaining many of the systematic trends observed in the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {astro-ph/9602085}, -author = {Baugh, C M and Cole, S and Frenk, C S}, -doi = {10.1093/mnras/283.4.1361}, -eprint = {9602085}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Galaxies: luminosity function,mass function}, -month = {dec}, -number = {4}, -pages = {1361--1378}, -primaryClass = {astro-ph}, -title = {{Evolution of the Bubble sequence in hierarchical models for galaxy formation}}, -url = {http://adsabs.harvard.edu/abs/1996MNRAS.283.1361B}, -volume = {283}, -year = {1996} -} -@article{Charlton2017, -abstract = {Stellar mass has been shown to correlate with halo mass, with non-negligible scatter. The stellar mass-size and luminosity-size relationships of galaxies also show significant scatter in galaxy size at fixed stellar mass. It is possible that, at fixed stellar mass and galaxy colour, the halo mass is correlated with galaxy size. Galaxy-galaxy lensing allows us to measure the mean masses of dark matter haloes for stacked samples of galaxies. We extend the analysis of the galaxies in the CFHTLenS catalogue by fitting single S{\`{e}}rsic surface brightness profiles to the lens galaxies in order to recover half-light radius values, allowing us to determine halo masses for lenses according to their size. Comparing our halo masses and sizes to baselines for that stellar mass yields a differential measurement of the halo mass-galaxy size relationship at fixed stellar mass, defined as Mh(M*) ∝ reff$\eta$ (M*). We find that, on average, our lens galaxies have an $\eta$ = 0.42 ± 0.12, i.e. larger galaxies live in more massive dark matter haloes. The $\eta$ is strongest for high-mass luminous red galaxies. Investigation of this relationship in hydrodynamical simulations suggests that, at a fixed M*, satellite galaxies have a larger $\eta$ and greater scatter in the Mh and reff relationship compared to central galaxies.}, -archivePrefix = {arXiv}, -arxivId = {1707.04924}, -author = {Charlton, Paul J L and Hudson, Michael J and Balogh, Michael L and Khatri, Sumeet}, -doi = {10.1093/MNRAS/STX2068}, -eprint = {1707.04924}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: observations,Darkmatter,Galaxies: haloes,Galaxies: structure,Gravitational lensing: weak}, -number = {2}, -pages = {2367--2387}, -title = {{The dependence of halo mass on galaxy size at fixed stellar mass using weak lensing}}, -volume = {472}, -year = {2017} -} -@article{Geometryee, -author = {Paulista, Universidade Estadual and Em, Programa D E P{\'{o}}s-gradua{\c{c}}{\~{a}}o and Biol{\'{o}}gicas, Ci{\^{e}}ncias}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Paulista, Em, Biol{\'{o}}gicas - Unknown - No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title(15).pdf:pdf}, -isbn = {9789896540821}, -pages = {1--16}, -title = {{No 主観的健康感を中心とした在宅高齢者における 健康関連指標に関する共分散構造分析Title}} -} -@article{Ding2019, -abstract = {Correlations between the mass of a supermassive black hole and the properties of its host galaxy (e.g., total stellar mass (M*), luminosity (Lhost)) suggest an evolutionary connection. A powerful test of a co-evolution scenario is to measure the relations MBH-Lhost and MBH-M* at high redshift and compare with local estimates. For this purpose, we acquired HST imaging with WFC3 of 32 X-ray-selected broad-line AGN at 1.2 1013 M⊙ and always stays below the peak, indicating that quenching mechanisms are present in massive halos that keep the star-formation efficiency low. Finally, we compared our results with three hydrodynamical simulations: Horizon-AGN, TNG100 of the IllustrisTNG project, and EAGLE.We find that the most significant discrepancy is at the high-mass end, where the simulations generally show that satellites have a higher contribution to the total stellar mass budget than the observations. This, together with the finding that the fraction of satellites is higher in the simulations, indicates that the feedback mechanisms acting in both group- and cluster-scale halos appear to be less efficient in quenching the mass assembly of satellites - and that quenching occurs much later in the simulations.}, -archivePrefix = {arXiv}, -arxivId = {2203.10895}, -author = {Shuntov, M. and McCracken, H. J. and Gavazzi, R. and Laigle, C. and Weaver, J. R. and Davidzon, I. and Ilbert, O. and Kauffmann, O. B. and Faisst, A. and Dubois, Y. and Koekemoer, A. M. and Moneti, A. and Milvang-Jensen, B. and Mobasher, B. and Sanders, D. B. and Toft, S.}, -doi = {10.1051/0004-6361/202243136}, -eprint = {2203.10895}, -file = {:C\:/Users/Jammy/Documents/Papers/Collaborations/Shuntov2022StellarHaloCOMSOS2020.pdf:pdf}, -issn = {14320746}, -journal = {A\&A}, -keywords = {Galaxies: evolution,Galaxies: halos,Large-scale structure of Universe}, -number = {43136}, -title = {{COSMOS2020: Cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z ∼5}}, -volume = {664}, -year = {2022} -} -@article{Jee2014, -abstract = {The distance-redshift relation plays a fundamental role in constraining cosmological models. In this paper, we show that measurements of positions and time delays of strongly lensed images of a background galaxy, as well as those of the velocity dispersion and mass profile of a lens galaxy, can be combined to extract the angular diameter distance of the lens galaxy. Physically, as the velocity dispersion and the time delay give a gravitational potential (GM/r) and a mass (GM) of the lens, respectively, dividing them gives a physical size (r) of the lens. Comparing the physical size with the image positions of a lensed galaxy gives the angular diameter distance to the lens. A mismatch between the exact locations at which these measurements are made can be corrected by measuring a local slope of the mass profile. We expand on the original idea put forward by Paraficz and Hjorth, who analyzed singular isothermal lenses, by allowing for an arbitrary slope of a power-law spherical mass density profile, an external convergence, and an anisotropic velocity dispersion. We find that the effect of external convergence cancels out when dividing the time delays and velocity dispersion measurements. We derive a formula for the uncertainty in the angular diameter distance in terms of the uncertainties in the observables. As an application, we use two existing strong lens systems, B1608+656 (zL=0.6304) and RXJ1131-1231 (zL=0.295), to show that the uncertainty in the inferred angular diameter distances is dominated by that in the velocity dispersion, $\sigma$2, and its anisotropy. We find that the current data on these systems should yield about 16% uncertainty in DA per object. This improves to 13% when we measure $\sigma$2 at the so-called sweet-spot radius. Achieving 7% is possible if we can determine $\sigma$2 with 5% precision.}, -archivePrefix = {arXiv}, -arxivId = {1410.7770}, -author = {Jee, I. and Komatsu, E. and Suyu, S. H.}, -doi = {10.1088/1475-7516/2015/11/033}, -eprint = {1410.7770}, -issn = {14757516}, -journal = {Journal of Cosmology and Astroparticle Physics}, -keywords = {galaxy dynamics,gravitational lensing}, -number = {11}, -pages = {33}, -title = {{Measuring angular diameter distances of strong gravitational lenses}}, -url = {http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2015JCAP...11..033J&link_type=ABSTRACT%5Cnpapers://dcc533b5-8613-47b7-b88c-2b0c0d39c33f/Paper/p10857}, -volume = {2015}, -year = {2015} -} -@article{Peirani2019, -abstract = {Using the two large cosmological hydrodynamical simulations, Horizon-AGN (H AGN) and Horizon-noAGN (H noAGN, no AGN feedback), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the total density profiles (dark matter+ stars) at the effective radius of massive early-type galaxies (M∗ ≥ 1011, M⊙). We have studied the dependencies of the mass-weighted density slope $\gamma$′tot with the effective radius, the galaxy mass and the host halo mass at z $\sim$ 0.3 and found that the inclusion of AGN feedback always leads to a much better agreement with observational values and trends. Our analysis also suggests that the inclusion of AGN feedback favours a strong correlation between $\gamma$′tot and the density slope of the dark matter component while, in the absence of AGN activity, $\gamma$′tot is rather strongly correlated with the density slope of the stellar component. Finally, we find that $\gamma$′tot derived from our samples of galaxies increases from z = 2 to z = 0, in good agreement with the expected observational trend. The derived slopes are slightly lower than in the data when AGN is included because the simulated galaxies tend to be too extended, especially the least massive ones. However, the simulated compact galaxies without AGN feedback have $\gamma$′tot values that are significantly too high compared to observations.}, -archivePrefix = {arXiv}, -arxivId = {1801.09754}, -author = {Peirani, S{\'{e}}bastien and Sonnenfeld, Alessandro and Gavazzi, Rapha{\"{e}}l and Oguri, Masamune and Dubois, Yohan and Silk, Joe and Pichon, Christophe and Devriendt, Julien and Kaviraj, Sugata}, -doi = {10.1093/mnras/sty3475}, -eprint = {1801.09754}, -file = {:C\:/Users/Jammy/Documents/Papers/Simulation/Peirani2019TotalPLSlopesHorizonAGN.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {dark matter,galaxies: evolution,galaxies: haloes,galaxies: jets,methods: numerical}, -number = {4}, -pages = {4615--4627}, -title = {{Total density profile of massive early-type galaxies in H orizon -AGN simulation: Impact of AGN feedback and comparison with observations}}, -volume = {483}, -year = {2019} -} -@article{Rydberg2018, -abstract = {Supernovae (SNe) could be powerful probes of the properties of stars and galaxies at high redshifts in future surveys. Wide fields and longer exposure times are required to offset diminishing star formation rates and lower fluxes to detect useful number of events at high redshift. In principle, the Large Synoptic Survey Telescope (LSST) could discover large numbers of early SNe because of its wide fields but only at lower redshifts because of its AB mag limit of ∼24. However, gravitational lensing by galaxy clusters and massive galaxies could boost flux from ancient SNe and allow LSST to detect them at earlier times. Here, we calculate detection rates for lensed SNe at z ∼ 5-7 for LSST. We find that the LSST Wide Fast Deep survey could detect up to 120 lensed Population (Pop) I and II SNe but no lensed Pop III SNe. Deep-drilling programs in 10 deg2 fields could detect Pop I and II core-collapse SNe at AB magnitudes of 27-28 and 26, respectively.}, -archivePrefix = {arXiv}, -arxivId = {1805.02662}, -author = {Rydberg, Claes Erik and Whalen, Daniel J. and Maturi, Matteo and Collett, Thomas and Carrasco, Mauricio and Magg, Mattis and Klessen, Ralf S.}, -doi = {10.1093/mnras/stz3203}, -eprint = {1805.02662}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Rydberg et al. - 2020 - Detecting strongly lensed supernovae at z ∼ 5-7 with LSST(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Cosmology: dark ages,Cosmology: observations,First stars: early universe,Galaxies: high,Gravitational lensing: strong,Redshift,Reionization,Stars: Population III,Supernovae: general}, -number = {2}, -pages = {2447--2459}, -title = {{Detecting strongly lensed supernovae at z ∼ 5-7 with LSST}}, -url = {http://arxiv.org/abs/1805.02662}, -volume = {491}, -year = {2020} -} -@article{Khochfar2011a, -abstract = {We propose a simple model for the origin of fast and slow rotator early-type galaxies (ETG) within the hierarchical $\Lambda$cold dark matter ($\Lambda$CDM) scenario, that is based on the assumption that the mass fraction of stellar discs in ETGs is a proxy for the specific angular momentum expressed via $\lambda$R. Within our model we reproduce the fraction of fast and slow rotators as a function of magnitude in the ATLAS3D survey, assuming that fast-rotating ETGs have at least 10 per cent of their total stellar mass in a disc component. In agreement with ATLAS3D observations we find that slow rotators are predominantly galaxies with M* {\textgreater} 1010.5 Msun contributing ˜20 per cent to the overall ETG population. We show in detail that the growth histories of fast and slow rotators are different, supporting the classification of ETGs into these two categories. Slow rotators accrete between ˜50 and 90 per cent of their stellar mass from satellites and their most massive progenitors have on average up to three major mergers during their evolution. Fast rotators in contrast accrete less than 50 per cent and have on average less than one major merger in their past. We find that the underlying physical reason for the different growth histories is the slowing down and ultimately complete shut-down of gas cooling in massive galaxies. Once cooling and associated star formation in disc stop, galaxies grow via infall from satellites. Frequent minor mergers thereby destroy existing stellar discs via violent relaxation and also tend to lower the specific angular momentum of the main stellar body, lowering $\lambda$R into the slow rotator regime. On average, the last gas-rich major merger interaction in slow rotators happens at z {\textgreater} 1.5, followed by a series of minor mergers. These results support the idea that kinematically decoupled cores (KDC) form during gas-rich major mergers at high z followed by minor mergers, which build-up the outer layers of the remnant, and make remnants that are initially too flat compared to observations become rounder. Fast rotators are less likely to form such KDCs due to the fact that they have on average less than one major merger in their past. Fast rotators in our model have different formation paths. The majority, 78 per cent, has bulge-to-total stellar mass ratios (B/T) {\textgreater} 0.5 and managed to grow stellar discs due to continued gas cooling or bulges due to frequent minor mergers. The remaining 22 per cent live in high-density environments and consist of low B/T galaxies with gas fractions below 15 per cent, that have exhausted their cold gas reservoir and have no hot halo from which gas can cool. These fast rotators most likely resemble the flattened disc-like fast rotators in the ATLAS3D survey. Our results predict that ETGs can change their state from fast to slow rotator and vice versa, while the former is taking place predominantly at low z (z {\textless} 2), the latter is occurring during cosmic epochs when cooling times are short and galaxies gas-rich. We predict that the ratio of the number density of slow to fast rotators is a strong function of redshift, with massive ({\textgreater}1010 Msun) fast rotators being more than one order of magnitude more frequent at z˜ 2.}, -archivePrefix = {arXiv}, -arxivId = {1107.5059}, -author = {Khochfar, Sadegh and Emsellem, Eric and Serra, Paolo and Bois, Maxime and Alatalo, Katherine and Bacon, R and Blitz, Leo and Bournaud, Fr{\'{e}}d{\'{e}}ric and Bureau, M and Cappellari, Michele and Davies, Roger L and Davis, Timothy A and de Zeeuw, P T and Duc, Pierre Alain and Krajnovi{\'{c}}, Davor and Kuntschner, Harald and Lablanche, Pierre Yves and McDermid, Richard M and Morganti, Raffaella and Naab, Thorsten and Oosterloo, Tom and Sarzi, Marc and Scott, Nicholas and Weijmans, Anne Marie and Young, Lisa M}, -doi = {10.1111/j.1365-2966.2011.19486.x}, -eprint = {1107.5059}, -isbn = {13844}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: structure,cD}, -number = {2}, -pages = {845--862}, -pmid = {13736}, -title = {{The ATLAS 3D project - VIII. Modelling the formation and evolution of fast and slow rotator early-type galaxies within $\Lambda$CDM}}, -volume = {417}, -year = {2011} -} -@article{Lovell2011, -abstract = {We calculate the orbital angular momentum of dark matter subhaloes in the Aquarius simulations of cold dark matter galactic haloes. We calculate the orientation of their angular momentum relative to that of the spin vector of their host halo and find a variety of different configurations. All six Aquarius haloes contain statistically significant populations of subhalo orbits that are aligned with the main halo spin. All haloes posses a population of subhaloes that rotates in the same direction as the main halo and three of them possess, in addition, a population that rotates in the opposite direction. These configurations arise from the filamentary accretion of subhaloes. Quasi-planar distributions of coherently rotating satellites, such as those inferred in the Milky Way and other galaxies, arise naturally in simulations of a {\$}\backslashbackslashLambda{\{}\backslash{\$}{\}}CDM universe.}, -archivePrefix = {arXiv}, -arxivId = {1008.0484}, -author = {Lovell, Mark R and Eke, Vincent R and Frenk, Carlos S and Jenkins, Adrian}, -doi = {10.1111/j.1365-2966.2011.18377.x}, -eprint = {1008.0484}, -issn = {00358711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Dark matter,Galaxies: formation}, -number = {4}, -pages = {3013--3021}, -title = {{The link between galactic satellite orbits and subhalo accretion}}, -volume = {413}, -year = {2011} -} -@article{Jin2017, -abstract = {We report the results from a recent 133 ks XMM-Newton observation of a highly super-Eddington narrow-line Type-1 QSO RX J0439.6-5311. This source has one of the steepest AGN hard X-ray slopes, in addition to a prominent and smooth soft X-ray excess. Strong variations are found throughout the 0.3 to 10 keV energy range on all time-scales covered by the observation, with the soft excess mainly showing low frequency variations below 0.1 mHz while the hard X-rays show stronger variability at higher frequencies. We perform a full set of spectral-timing analysis on the X-ray data, including a simultaneous modelling of the time-average spectra, frequency-dependent RMS and covariance spectra, lag-frequency and lag-energy spectra. Especially, we find a significant time-lag signal in the low frequency band, which indicates that the soft X-rays lead the hard by {\$}\backslashsim{\$}4 ks, with a broad continuum-like profile in the lag spectrum. Our analysis strongly supports the model where the soft X-ray excess is dominated by a separate low temperature, optically thick Comptonisation component rather than relativistic reflection or a jet. This soft X-ray emitting region is several tens or hundreds of {\$}R{\_}{\{}g{\}}{\$} away from the hot corona emitting hard X-rays, and is probably associated with a geometrically thick (`puffed-up') inner disc region.}, -archivePrefix = {arXiv}, -arxivId = {1703.07118}, -author = {Jin, Chichuan and Done, Chris and Ward, Martin}, -doi = {10.1093/mnras/stx718}, -eprint = {1703.07118}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {accretion,accretion discs - galaxies,active - galaxies,nuclei}, -number = {3}, -pages = {3663--3681}, -title = {{Super-Eddington QSO RX J0439.6−5311 – I. Origin of the soft X-ray excess and structure of the inner accretion flow}}, -url = {http://arxiv.org/abs/1703.07118%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx718}, -volume = {468}, -year = {2017} -} -@article{Bertschinger2008, -abstract = {The acceleration of the Universe can be explained either through dark energy or through the modification of gravity on large scales. In this paper we investigate modified gravity models and compare their observable predictions with dark energy models. Modifications of general relativity are expected to be scale independent on superhorizon scales and scale dependent on subhorizon scales. For scale-independent modifications, utilizing the conservation of the curvature scalar and a parametrized post-Newtonian formulation of cosmological perturbations, we derive results for large-scale structure growth, weak gravitational lensing, and cosmic microwave background anisotropy. For scale-dependent modifications, inspired by recent f(R) theories we introduce a parametrization for the gravitational coupling G and the post-Newtonian parameter $\gamma$. These parametrizations provide a convenient formalism for testing general relativity. However, we find that if dark energy is generalized to include both entropy and shear stress perturbations, and the dynamics of dark energy is unknown a priori, then modified gravity cannot in general be distinguished from dark energy using cosmological linear perturbations. {\textcopyright} 2008 The American Physical Society.}, -archivePrefix = {arXiv}, -arxivId = {0801.2431}, -author = {Bertschinger, Edmund and Zukin, Phillip}, -doi = {10.1103/PhysRevD.78.024015}, -eprint = {0801.2431}, -issn = {15507998}, -journal = {Physical Review D - Particles, Fields, Gravitation and Cosmology}, -keywords = {Dark energy,Higher-dimensional gravity and other theories of,Modified theories of gravity}, -month = {jul}, -number = {2}, -pages = {24015}, -title = {{Distinguishing modified gravity from dark energy}}, -volume = {78}, -year = {2008} -} -@article{Hopkins2010a, -abstract = {The stellar surface mass density profiles at the centres of typical {\$\sim${}} L* and lower mass spheroids exhibit power-law 'cusps' with $\Sigma$ $\alpha$ R-$\eta$, where 0.5 ≲ $\eta$ ≲ 1 for radii {\$\sim${}} 1-100 pc. Observations and theory support models in which these cusps are formed by dissipative gas inflows and nuclear starbursts in gas-rich mergers. At these comparatively large radii, stellar relaxation is unlikely to account for, or strongly modify, the cuspy stellar profiles. We argue that the power-law surface density profiles observed are a natural consequence of the gravitational instabilities that dominate angular momentum transport in the gravitational potential of a central massive black hole. The dominant mode at these radii is an m = 1 lopsided/eccentric disc instability, in which stars torquing the gas can drive rapid inflow and accretion. Such a mode first generically appears at large radii and propagates inwards by exciting eccentricities at smaller and smaller radii, where M*({\textless} R) « MBH. When the stellar surface density profile is comparatively shallow with $\eta$ {\textless} 1/2, the modes cannot efficiently propagate to R = 0 and so gas piles up and star formation steepens the profile. But if the profile is steeper than $\eta$ = 1, the inward propagation of eccentricity is strongly damped, suppressing inflow and bringing $\eta$ down again. Together these results produce an equilibrium slope of 1/2 ≲ $\eta$ ≲ 1 in the potential of the central black hole. These physical arguments are supported by non-linear numerical simulations of gas inflow in galactic nuclei. Together, these results naturally explain the observed stellar density profiles of 'cusp' elliptical galaxies. {\textcopyright}2010 The Authors Monthly Notices of the Royal Astronomical Society {\textcopyright}2010 RAS.}, -archivePrefix = {arXiv}, -arxivId = {1011.3045}, -author = {Hopkins, Philip F and Quataert, Eliot}, -doi = {10.1111/j.1745-3933.2010.00995.x}, -eprint = {1011.3045}, -issn = {17453933}, -journal = {Monthly Notices of the Royal Astronomical Society: Letters}, -keywords = {Cosmology: theory,Galaxies: active,Galaxies: bulges,Galaxies: evolution,Galaxies: nuclei,Quasars: general}, -number = {1}, -title = {{An explanation for the slopes of stellar cusps in galaxy spheroids}}, -url = {http://arxiv.org/abs/1011.3045%7B%5C%25%7D0Ahttp://dx.doi.org/10.1111/j.1745-3933.2010.00995.x}, -volume = {411}, -year = {2011} -} -@article{Petrillo2017, -abstract = {The volume of data that will be produced by new-generation surveys requires automatic classification methods to select and analyse sources. Indeed, this is the case for the search for strong gravitational lenses, where the population of the detectable lensed sources is only a very small fraction of the full source population. We apply for the first time a morphological classification method based on a Convolutional Neural Network (CNN) for recognizing strong gravitational lenses in 255 deg2 of the Kilo Degree Survey (KiDS), one of the currentgeneration optical wide surveys. The CNN is currently optimized to recognize lenses with Einstein radii ≳1.4 arcsec, about twice the r-band seeing in KiDS. In a sample of 21 789 colour-magnitude selected luminous red galaxies (LRGs), of which three are known lenses, the CNN retrieves 761 strong-lens candidates and correctly classifies two out of three of the known lenses. The misclassified lens has an Einstein radius below the range on which the algorithm is trained. We down-select the most reliable 56 candidates by a joint visual inspection. This final sample is presented and discussed. A conservative estimate based on our results shows that with our proposed method it should be possible to find $\sim$100 massive LRGgalaxy lenses at z ≲ 0.4 in KiDS when completed. In the most optimistic scenario, this number can grow considerably (to maximally $\sim$2400 lenses), when widening the colour-magnitude selection and training the CNN to recognize smaller image-separation lens systems.}, -archivePrefix = {arXiv}, -arxivId = {1702.07675}, -author = {Petrillo, C. E. and Tortora, C. and Chatterjee, S. and Vernardos, G. and Koopmans, L. V.E. and Kleijn, G. Verdoes and Napolitano, N. R. and Covone, G. and Schneider, P. and Grado, A. and McFarland, J.}, -doi = {10.1093/mnras/stx2052}, -eprint = {1702.07675}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Petrillo et al. - 2017 - Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks(2).pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: elliptical and lenticular, cD,Gravitational lensing: strong,Methods: data analysis,Methods: statistical,Surveys}, -number = {1}, -pages = {1129--1150}, -title = {{Finding strong gravitational lenses in the Kilo Degree Survey with Convolutional Neural Networks}}, -volume = {472}, -year = {2017} -} -@article{Algorry2016, -abstract = {We examine the properties of barred disc galaxies in a LCDM cosmological hydrodynamical simulation from the EAGLE project. Our study follows the formation of 269 discs identified at z = 0 in the stellar mass range 10.6 {\textless} log Mstr /M {\textless} 11. These discs show a wide range of bar strengths, from unbarred discs to weak bars to strongly barred systems (= 20{\%}). Bars in these systems develop after redshift = 1.3, on timescales that depend sen- sitively on the strength of the pattern. Strong bars develop relatively quickly (in a few Gyr, = 10 disc rotation periods) in systems that are disc dominated, gas poor, and have declining rotation curves. Weak bars develop more slowly in systems where the disc is less gravitation- ally important, and are still growing at z = 0. Unbarred galaxies are comparatively gas-rich discs whose rotation speeds do not exceed the maximum circular velocity of the halos they inhabit. Bar lengths compare favourably with observations, ranging from 0.2 to 0.8 times the radius containing 90{\%} of the stars. Bars slow down remarkably quickly as they grow, causing the inner regions of the surrounding dark halo to expand. At z = 0 strong bars have corota- tion radii roughly ten times the bar length. Such slow bars are inconsistent with the few cases where pattern speeds have been measured or inferred observationally, a discrepancy that, if confirmed, might prove a challenge for disc galaxy formation in LCDM.}, -annote = {NULL}, -archivePrefix = {arXiv}, -arxivId = {1609.05909}, -author = {Algorry, David G and Navarro, Julio F and Abadi, Mario G and Sales, Laura V and Bower, Richard G and Crain, Robert A and {Dalla Vecchia}, Claudio and Frenk, Carlos S and Schaller, Matthieu and Schaye, Joop and Theuns, Tom}, -doi = {10.1093/mnras/stx1008}, -eprint = {1609.05909}, -issn = {0035-8711}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {disc,formation,galaxies,galaxy,kinematics and dynamics}, -number = {1}, -pages = {1054--1064}, -title = {{Barred galaxies in the EAGLE cosmological hydrodynamical simulation}}, -url = {http://arxiv.org/abs/1609.05909%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx1008}, -volume = {469}, -year = {2017} -} -@article{Pillepich2017, -abstract = {We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multimode feedback. In this paper, we give a comprehensive description of the physical and numerical advances that form the core of the IllustrisTNG (The Next Generation) framework.We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black-hole-driven kinetic feedback at low accretion rates, magnetohydrodynamics and improvements to the numerical scheme. Using a suite of (25Mpc h-1)3 cosmological boxes, we assess the outcome of the new model at our fiducial resolution. The presence of a selfconsistently amplified magnetic field is shown to have an important impact on the stellar content of 1012M⊙ haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low-mass end of the galaxy population.}, -archivePrefix = {arXiv}, -arxivId = {1703.02970}, -author = {Pillepich, Annalisa and Springel, Volker and Nelson, Dylan and Genel, Shy and Naiman, Jill and Pakmor, R{\"{u}}diger and Hernquist, Lars and Torrey, Paul and Vogelsberger, Mark and Weinberger, Rainer and Marinacci, Federico}, -doi = {10.1093/mnras/stx2656}, -eprint = {1703.02970}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {Galaxies: evolution,Galaxies: formation,Methods: numerical}, -number = {3}, -pages = {4077--4106}, -title = {{Simulating galaxy formation with the IllustrisTNG model}}, -url = {http://arxiv.org/abs/1703.02970%7B%5C%25%7D0Ahttp://dx.doi.org/10.1093/mnras/stx2656}, -volume = {473}, -year = {2018} -} -@article{Reines2015, -abstract = {Scaling relations between central black hole (BH) mass and host galaxy properties are of fundamental importance to studies of BH and galaxy evolution throughout cosmic time. Here we investigate the relationship between BH mass and host galaxy total stellar mass using a sample of 262 broad-line active galactic nuclei (AGNs) in the nearby universe (z < 0.055), as well as 79 galaxies with dynamical BH masses. The vast majority of our AGN sample is constructed using Sloan Digital Sky Survey spectroscopy and searching for Seyfert-like narrow-line ratios and broad H$\alpha$ emission. BH masses are estimated using standard virial techniques. We also include a small number of dwarf galaxies with total stellar masses Mstellar ≲ 109.5 Mo and a subsample of the reverberation-mapped AGNs. Total stellar masses of all 341 galaxies are calculated in the most consistent manner feasible using color-dependent mass-to-light ratios. We find a clear correlation between BH mass and total stellar mass for the AGN host galaxies, with MBH ∝ Mstellar, similar to that of early-type galaxies with dynamically detected BHs. However, the relation defined by the AGNs has a normalization that is lower by more than an order of magnitude, with a BH-to-total stellar mass fraction of MBH/Mstellar ∼ 0.025% across the stellar mass range 108 ≤ Mstellar/Mo ≤ 1012. This result has significant implications for studies at high redshift and cosmological simulations in which stellar bulges cannot be resolved.}, -archivePrefix = {arXiv}, -arxivId = {1508.06274}, -author = {Reines, Amy E. and Volonteri, Marta}, -doi = {10.1088/0004-637X/813/2/82}, -eprint = {1508.06274}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Reines, Volonteri - 2015 - RELATIONS between CENTRAL BLACK HOLE MASS and TOTAL GALAXY STELLAR MASS in the LOCAL UNIVERSE.pdf:pdf}, -issn = {15384357}, -journal = {Astrophysical Journal}, -keywords = {galaxies: Seyfert,galaxies: active,galaxies: evolution,galaxies: nuclei}, -number = {2}, -title = {{RELATIONS between CENTRAL BLACK HOLE MASS and TOTAL GALAXY STELLAR MASS in the LOCAL UNIVERSE}}, -volume = {813}, -year = {2015} -} -@article{Veale2017b, -abstract = {We measure the radial profiles of the stellar velocity dispersions, $\sigma$(R), for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude MK < -25.3mag, or stellar mass M* ≳ 4 × 1011M⊙, within 108 Mpc. Our wide-field 107 arcsec × 107 arcsec IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes $\gamma$ inner and $\gamma$ outer of s(R). While $\gamma$ inner is mostly negative, of the 56 galaxies with sufficient radial coverage to determine $\gamma$ outer we find 36 per cent to have rising outer dispersion profiles, 30 per cent to be flat within the uncertainties and 34 per cent to be falling. The fraction of galaxies with rising outer profiles increases with M* and in denser galaxy environment, with 10 of the 11 most massive galaxies in our sample having flat or rising dispersion profiles. The strongest environmental correlations are with local density and halo mass, but a weaker correlation with large-scale density also exists. The average $\gamma$ outer is similar for brightest group galaxies, satellites and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis h4. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone.}, -archivePrefix = {arXiv}, -arxivId = {1708.00870}, -author = {Veale, Melanie and Ma, Chung Pei and Greene, Jenny E. and Thomas, Jens and Blakeslee, John P. and Walsh, Jonelle L. and Ito, Jennifer}, -doi = {10.1093/MNRAS/STX2717}, -eprint = {1708.00870}, -file = {:C\:/Users/Jammy/AppData/Local/Mendeley Ltd./Mendeley Desktop/Downloaded/Veale et al. - 2018 - The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxie.pdf:pdf}, -issn = {13652966}, -journal = {Monthly Notices of the Royal Astronomical Society}, -keywords = {CD,Galaxies: elliptical and lenticular,Galaxies: evolution,Galaxies: formation,Galaxies: kinematics and dynamics,Galaxies: structure}, -number = {3}, -pages = {5446--5467}, -title = {{The MASSIVE survey - VIII. Stellar velocity dispersion profiles and environmental dependence of early-type galaxies}}, -url = {http://arxiv.org/abs/1708.00870}, -volume = {473}, -year = {2018} -} -@article{DSouza2014, -abstract = {We study the stellar haloes of galaxies out to 70-100 kpc as a function of stellar mass and galaxy type by stacking aligned r- and g-band images from a sample of 45 508 galaxies from Sloan Digital Sky Survey Data Release 9 in the redshift range 0.06≤z≤0.1 and in the mass range 1010.0M⊙