From 36ad58016b8d9bfcdd0265cfe095a4a74fe778e8 Mon Sep 17 00:00:00 2001 From: Madicken Munk Date: Tue, 10 Mar 2020 15:59:51 -0500 Subject: [PATCH 1/5] update figure captions to be in a smaller font size --- index.md | 3 ++- learn.md | 30 +++++++++++++++++------------- 2 files changed, 19 insertions(+), 14 deletions(-) diff --git a/index.md b/index.md index 477b610..bb2bf84 100644 --- a/index.md +++ b/index.md @@ -34,10 +34,11 @@ Here's what you'll find at the RSL: on how to access and analyze Renaissance Simulation data. ## About the Renaissance Simulations +
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Mass-weighted density projection of the (40 comoving Mpc)3 survey volume, showing the locations of the Rarepeak, Normal, and Void zoom-in regions.
diff --git a/learn.md b/learn.md index c1f1614..2a18f4b 100644 --- a/learn.md +++ b/learn.md @@ -25,7 +25,7 @@ use supercomputers to study them, and what this site enables you to do.
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The Universe at t=13,800,000,000 yr. (NASA and Space Telescope Science Institute)
@@ -40,18 +40,19 @@ galaxies”? And how do they differ from modern galaxies like the Milky Way?
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The Universe at t=380,000,000 yr. (ESA and Planck Collaboration) +learn +more
- [learn more](https://en.wikipedia.org/wiki/Cosmic_microwave_background) ## Growing Galaxies
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Simplified diagram showing hierarchical assembly of galaxies starting from small fluctuations in the density distribution of the early universe. (Australia Telescope National Facility)
@@ -72,7 +73,7 @@ assembly of thousands of protogalaxies which are much smaller.
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Conceptual diagram showing how the Hubble Space Telescope looks back into time at the earliest galaxies. The relative depth of the Hubble Deep Field and the Hubble Ultra-Deep Field is shown. (Wikipedia) @@ -95,7 +96,7 @@ galaxies.
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Composite of high redshift galaxies imaged by the Hubble Space Telescope. The galaxies appear red due to cosmological redshift. (Space Telescope Science Institute)
@@ -115,10 +116,11 @@ Before we delve into how we use supercomputers to study the first galaxies, we n to cover some basics. ## Supercomputers +
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The Blue Waters Sustained Petascale Supercomputer at the University of Illinois, Urbana-Champaign. (M. Norman, UCSD)
@@ -131,10 +133,11 @@ used for the Renaissance Simulations, has over 22,640 nodes, each with 16 cores, a total of 362,240 processing elements. [learn more](https://en.wikipedia.org/wiki/Blue_Waters) ## Parallel computing +
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Parallel computing subdivides the problem domain into many smaller domains, which are calculated simulateneously on many processors of a supercomputer. (M. Norman, UCSD)
@@ -150,10 +153,11 @@ synchronicity. Typically, the subdivision of the big problem into many smaller p is done using domain decomposition, illustrated at right. [learn more](https://en.wikipedia.org/wiki/Parallel_computing) ## Coping with an infinite universe +
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Simulation of cosmic structure is performed in a cubic volume assuming periodic boundary conditions in all 3 directions. (G. Bryan, Columbia & M. Norman, UCSD)
@@ -174,7 +178,7 @@ the box we are simulating.
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The expansion of the universe is removed from the simulation through the comoving coordinate transformation. (M. Norman, UCSD)
@@ -192,7 +196,7 @@ exactly the rate of the expanding universe. We say we simulate a co-moving volum
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Matter fluctuations consistent with CMB measurements are used to initialize the cosmology simulation. (M. Norman, UCSD)
@@ -212,7 +216,7 @@ we are able to adjust the amplitude accordingly, however the power spectrum rema
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The matter fluctuations grow in amplitude, forming the characteristic cosmic web large scale structure of the universe. (M. Norman, UCSD)
@@ -228,7 +232,7 @@ you want to simulate, and how finely resolved the simulation is. [learn more](ht
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Equations of cosmological hydrodynamics. (M. Norman, UCSD)
From e5f7b31b9837ebfe354fe5cb8b3378c9384b8f86 Mon Sep 17 00:00:00 2001 From: Madicken Munk Date: Tue, 10 Mar 2020 16:01:17 -0500 Subject: [PATCH 2/5] make image formatting consistent with other figures --- learn.md | 2 +- 1 file changed, 1 insertion(+), 1 deletion(-) diff --git a/learn.md b/learn.md index 2a18f4b..be787bc 100644 --- a/learn.md +++ b/learn.md @@ -37,7 +37,7 @@ fluctuations in the density of matter. How does a featureless universe “grow galaxies”? And how do they differ from modern galaxies like the Milky Way? [learn more](https://en.wikipedia.org/wiki/Hubble_Ultra-Deep_Field) -
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From 3f7c0ed4254b6d4fcf2f4b808fb4b17e7e56202b Mon Sep 17 00:00:00 2001 From: Madicken Munk Date: Tue, 10 Mar 2020 16:03:42 -0500 Subject: [PATCH 3/5] add line breaks to fix formatting issues from caption overflow --- learn.md | 13 +++++++++++++ showcase.md | 21 +++++++++++++++++---- 2 files changed, 30 insertions(+), 4 deletions(-) diff --git a/learn.md b/learn.md index be787bc..85a3d37 100644 --- a/learn.md +++ b/learn.md @@ -109,6 +109,11 @@ faint because they are distant. And they are very small compared to the Milky Way galaxy. A typical size is about 500 parsec, which is 1/50 the size of the Milky Way galaxy. [learn more](https://en.wikipedia.org/wiki/Redshift). +
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# How we use supercomputers to study the first galaxies @@ -131,6 +136,10 @@ a fast network so that it can act like a single, very powerful computer. Each no can have dozens of processing “cores”. For example, The Blue Waters supercomputer, used for the Renaissance Simulations, has over 22,640 nodes, each with 16 cores, for a total of 362,240 processing elements. [learn more](https://en.wikipedia.org/wiki/Blue_Waters) +
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## Parallel computing @@ -151,6 +160,10 @@ simultaneously, or “in parallel”, with information about their state being c communicated to neighboring processors in order to maintain physical correctness and synchronicity. Typically, the subdivision of the big problem into many smaller problems is done using domain decomposition, illustrated at right. [learn more](https://en.wikipedia.org/wiki/Parallel_computing) +
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## Coping with an infinite universe diff --git a/showcase.md b/showcase.md index 82d1ac9..0c38ed8 100644 --- a/showcase.md +++ b/showcase.md @@ -33,14 +33,15 @@ In [Xu et al. 2013](http://adsabs.harvard.edu/abs/2013ApJ...773...83X) the Rarep ### 2. HEATING THE INTERGALACTIC MEDIUM BY X-RAYS FROM POPULATION III BINARIES IN HIGH-REDSHIFT GALAXIES #### Hao Xu, Kyungjin Ahn, John H. Wise, Michael L. Norman, and Brian W. O’Shea, ApJ, 791:110, 2014 -
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If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [Xu et al. 2014](http://adsabs.harvard.edu/abs/2014ApJ...791..110X) calculate the x-ray feedback on the intergalactic medium (IGM) in the Rarepeak simulation. On average, the x-rays heat the IGM by 100 K, but much higher in the vicinity of the Rarepeak. +



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### 3. SCALING RELATIONS FOR GALAXIES PRIOR TO REIONIZATION #### Pengfei Chen, John H. Wise, Michael L. Norman, Hao Xu, and Brian W. O’Shea, ApJ, 795:144, 2014 @@ -53,6 +54,8 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [
[Chen et al. 2014](http://adsabs.harvard.edu/abs/2014ApJ...795..144C) examine statistical correlations amongst many baryonic and dark matter properties of interest in a sample of high redshift galaxies in the Rarepeak simulation. These correlations can be used to build semi-analytic models of the formation of early galaxies. +



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### 4. PROBING THE ULTRAVIOLET LUMINOSITY FUNCTION OF THE EARLIEST GALAXIES WITH THE RENAISSANCE SIMULATIONS #### Brian W. O’Shea, John H. Wise, Hao Xu, and Michael L. Norman, ApJLett, 807:L12, 2015 @@ -74,9 +77,12 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [
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[Ahn et al. 2015](http://adsabs.harvard.edu/abs/2015ApJ...802....8A) calculate the high redshift 21 cm signal resulting from the x-ray heating of the IGM modeled by Xu et al. (2014) as discussed above. The signal depends on the x-ray source model, but in the most optimistic scenario is detectable with the future Square Kilometer Array (SKA). The figure above shows the z=19 21 cm brightness temperature power spectrum for different x-ray source energies. +
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+ ### 6. LATE POP III STAR FORMATION DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS #### Hao Xu, Michael L. Norman, Brian W. O'Shea, and John H. Wise, ApJ, 823:140, 2016 @@ -100,6 +106,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [
[Xu et al. 2016b](http://adsabs.harvard.edu/abs/2016ApJ...832L...5X) calculate the x-ray background produced by Pop III stellar remnants, taking as input the extended Pop III star formation history presented in Xu et al. (2016a), and assuming a fair fraction of the stellar remnants are high mass x-ray binaries. It is found that Pop III stars can make a substantial contribution to the x-ray background. +

### 8. GALAXY PROPERTIES AND UV ESCAPE FRACTIONS DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS #### Hao Xu, John H. Wise, Michael L. Norman, Kyungjin Ahn, and Brian W. O'Shea, ApJ, 833:84, 2016 @@ -112,6 +119,8 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [
[Xu et al. 2016c](http://adsabs.harvard.edu/abs/2016ApJ...833...84X) present a detailed analysis of the galaxy properties and ionizing escape fraction from the combined Renaissance Simulations galaxy sample (over 10,000 high redshift galaxies). +



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### 9. First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations #### Kirk S. S. Barrow, John H. Wise, Michael L. Norman, Brian W. O'Shea, Hao Xu , MNRAS, 469:4863, 2017 @@ -124,6 +133,8 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [
[Barrow et al. 2017](http://adsabs.harvard.edu/abs/2017MNRAS.469.4863B) explore the photometric and spectroscopic properties of the galaxies in the Rarepeak Renaissance Simulation, in particular, as observed by the upcoming James Webb Space Telescope. +



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### 10. First light – II. Emission line extinction, population III stars, and X-ray binaries #### Kirk S S Barrow, John H Wise, Aycin Aykutalp, Brian W O'Shea, Michael L Norman, Hao Xu, MNRAS, 474:2617, 2018 @@ -136,6 +147,8 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [
[Barrow et al. 2018](http://adsabs.harvard.edu/abs/2018MNRAS.474.2617B) continue their exploration of the observable properties of high redshift galaxies as predicted by the renaissance Simulations. Here they focus on the spectroscopic features produced by small clusters of Pop III stars, as well as x-ray binaries they may leave behind as remnants. +



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### 11. The Growth of Black Holes from Population III Remnants in the Renaissance Simulations #### Britton Smith, John Regan, Turlough Downes, Michael Norman, Brian O'Shea, John Wise, MNRAS, submitted, 2018 From 9e3a742a9a303b19b0b71fa30fdc86c62c1d3c93 Mon Sep 17 00:00:00 2001 From: Madicken Munk Date: Tue, 10 Mar 2020 16:06:01 -0500 Subject: [PATCH 4/5] add padding on left-aligned images so text is readable --- showcase.md | 16 ++++++++-------- 1 file changed, 8 insertions(+), 8 deletions(-) diff --git a/showcase.md b/showcase.md index 0c38ed8..69b63a0 100644 --- a/showcase.md +++ b/showcase.md @@ -60,7 +60,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 4. PROBING THE ULTRAVIOLET LUMINOSITY FUNCTION OF THE EARLIEST GALAXIES WITH THE RENAISSANCE SIMULATIONS #### Brian W. O’Shea, John H. Wise, Hao Xu, and Michael L. Norman, ApJLett, 807:L12, 2015 -
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@@ -72,7 +72,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 5. SPATIALLY EXTENDED 21 cm SIGNAL FROM STRONGLY CLUSTERED UV AND X-RAY SOURCES IN THE EARLY UNIVERSE #### Kyungjin Ahn, Hao Xu, Michael L. Norman, Marcelo A. Alvarez, and John H. Wise, ApJ, 802:8, 2015 -
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@@ -86,7 +86,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 6. LATE POP III STAR FORMATION DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS #### Hao Xu, Michael L. Norman, Brian W. O'Shea, and John H. Wise, ApJ, 823:140, 2016 -
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@@ -98,7 +98,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 7. X-RAY BACKGROUND AT HIGH REDSHIFTS FROM POP III REMNANTS: RESULTS FROM POP III STAR FORMATION RATES IN THE RENAISSANCE SIMULATIONS #### Hao Xu, Kyungjin Ahn, Michael L. Norman, John H. Wise, and Brian W. O'Shea, ApJLett, 832:L5, 2016 -
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@@ -111,7 +111,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 8. GALAXY PROPERTIES AND UV ESCAPE FRACTIONS DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS #### Hao Xu, John H. Wise, Michael L. Norman, Kyungjin Ahn, and Brian W. O'Shea, ApJ, 833:84, 2016 -
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@@ -125,7 +125,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 9. First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations #### Kirk S. S. Barrow, John H. Wise, Michael L. Norman, Brian W. O'Shea, Hao Xu , MNRAS, 469:4863, 2017 -
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@@ -139,7 +139,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 10. First light – II. Emission line extinction, population III stars, and X-ray binaries #### Kirk S S Barrow, John H Wise, Aycin Aykutalp, Brian W O'Shea, Michael L Norman, Hao Xu, MNRAS, 474:2617, 2018 -
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@@ -153,7 +153,7 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ ### 11. The Growth of Black Holes from Population III Remnants in the Renaissance Simulations #### Britton Smith, John Regan, Turlough Downes, Michael Norman, Brian O'Shea, John Wise, MNRAS, submitted, 2018 -
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From c1ee8078793f45cd2e3092b85328d35f0211bf78 Mon Sep 17 00:00:00 2001 From: Madicken Munk Date: Tue, 10 Mar 2020 16:09:18 -0500 Subject: [PATCH 5/5] remove useless image links --- learn.md | 12 ------------ showcase.md | 11 ----------- 2 files changed, 23 deletions(-) diff --git a/learn.md b/learn.md index 85a3d37..f1a31c0 100644 --- a/learn.md +++ b/learn.md @@ -23,7 +23,6 @@ use supercomputers to study them, and what this site enables you to do. ## Then and now
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The Universe at t=13,800,000,000 yr. (NASA and Space Telescope Science Institute) @@ -38,7 +37,6 @@ galaxies”? And how do they differ from modern galaxies like the Milky Way? [learn more](https://en.wikipedia.org/wiki/Hubble_Ultra-Deep_Field)
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The Universe at t=380,000,000 yr. (ESA and Planck Collaboration) @@ -50,7 +48,6 @@ more ## Growing Galaxies
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Simplified diagram showing hierarchical assembly of galaxies starting from small fluctuations in the density distribution of the early universe. @@ -71,7 +68,6 @@ assembly of thousands of protogalaxies which are much smaller. ## Observing the First Galaxies
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Conceptual diagram showing how the Hubble Space Telescope looks back @@ -94,7 +90,6 @@ galaxies. ## Faint Red Blobs at the Edge of the Universe
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Composite of high redshift galaxies imaged by the Hubble Space Telescope. The galaxies appear red due to cosmological redshift. (Space Telescope Science Institute) @@ -123,7 +118,6 @@ to cover some basics. ## Supercomputers
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The Blue Waters Sustained Petascale Supercomputer at the University of Illinois, Urbana-Champaign. @@ -144,7 +138,6 @@ a total of 362,240 processing elements. [learn more](https://en.wikipedia.org/w ## Parallel computing
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Parallel computing subdivides the problem domain into many smaller domains, which are @@ -168,7 +161,6 @@ is done using domain decomposition, illustrated at right. [learn more](https://e ## Coping with an infinite universe
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Simulation of cosmic structure is performed in a cubic volume assuming periodic boundary conditions @@ -189,7 +181,6 @@ the box we are simulating. ## Coping with an expanding universe
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The expansion of the universe is removed from the simulation through the comoving coordinate transformation. @@ -207,7 +198,6 @@ exactly the rate of the expanding universe. We say we simulate a co-moving volum ## Initializing the simulation
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Matter fluctuations consistent with CMB measurements are used to initialize the @@ -227,7 +217,6 @@ we are able to adjust the amplitude accordingly, however the power spectrum rema ## Computing what happens next
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The matter fluctuations grow in amplitude, forming the characteristic cosmic web @@ -243,7 +232,6 @@ you want to simulate, and how finely resolved the simulation is. [learn more](ht ## What physical laws are programmed?
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Equations of cosmological hydrodynamics. diff --git a/showcase.md b/showcase.md index 69b63a0..0c8abac 100644 --- a/showcase.md +++ b/showcase.md @@ -22,7 +22,6 @@ A 47-minute science documentary directed by Tom Lucas. Available on [Amazon Prim #### Hao Xu, John H. Wise, and Michael L. Norman, ApJ, 773:83, 2013
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@@ -34,7 +33,6 @@ In [Xu et al. 2013](http://adsabs.harvard.edu/abs/2013ApJ...773...83X) the Rarep #### Hao Xu, Kyungjin Ahn, John H. Wise, Michael L. Norman, and Brian W. O’Shea, ApJ, 791:110, 2014
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@@ -47,7 +45,6 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ #### Pengfei Chen, John H. Wise, Michael L. Norman, Hao Xu, and Brian W. O’Shea, ApJ, 795:144, 2014
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@@ -126,7 +118,6 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ #### Kirk S. S. Barrow, John H. Wise, Michael L. Norman, Brian W. O'Shea, Hao Xu , MNRAS, 469:4863, 2017
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@@ -140,7 +131,6 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ #### Kirk S S Barrow, John H Wise, Aycin Aykutalp, Brian W O'Shea, Michael L Norman, Hao Xu, MNRAS, 474:2617, 2018
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@@ -154,7 +144,6 @@ If one assumes a fraction of Pop III stellar remnants high mass x-ray binaries [ #### Britton Smith, John Regan, Turlough Downes, Michael Norman, Brian O'Shea, John Wise, MNRAS, submitted, 2018
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