Skip to content

Page formatting #7

New issue

Have a question about this project? Sign up for a free GitHub account to open an issue and contact its maintainers and the community.

Sign up for GitHub

By clicking “Sign up for GitHub”, you agree to our terms of service and privacy statement. We’ll occasionally send you account related emails.

Already on GitHub? Sign in to your account

Open
munkm wants to merge 5 commits into
base: master
Choose a base branch
from
Open

Page formatting #7

Show file tree
Hide file tree
Changes from all commits
Commits
Show all changes
5 commits
Select commit Hold shift + click to select a range
36ad580
update figure captions to be in a smaller font size
munkm Mar 10, 2020
e5f7b31
make image formatting consistent with other figures
munkm Mar 10, 2020
3f7c0ed
add line breaks to fix formatting issues from caption overflow
munkm Mar 10, 2020
9e3a742
add padding on left-aligned images so text is readable
munkm Mar 10, 2020
c1ee807
remove useless image links
munkm Mar 10, 2020
File filter

Filter by extension

Filter by extension
Conversations
Failed to load comments.
Loading
Jump to
Jump to file
Failed to load files.
Loading
Diff view
Diff view
3 changes: 2 additions & 1 deletion index.md
View file
Open in desktop
Original file line number Diff line number Diff line change
Expand Up @@ -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

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/ApJ_projection_all.PNG" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
Mass-weighted density projection of the (40 comoving Mpc)<sup>3</sup> survey volume, showing the locations of the
Rarepeak, Normal, and Void zoom-in regions.
</figcaption>
Expand Down
57 changes: 31 additions & 26 deletions learn.md
View file
Open in desktop
Original file line number Diff line number Diff line change
Expand Up @@ -23,9 +23,8 @@ use supercomputers to study them, and what this site enables you to do.
## Then and now

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig1.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
The Universe at t=13,800,000,000 yr. (NASA and Space Telescope Science Institute)
</figcaption>
</figure>
Expand All @@ -37,21 +36,20 @@ 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)

<figure style="display: table; float: left;">
<a href="somewhereelse">
<figure style="display: table; float: left; margin: 0 0 20px 20px">
<img src="images/fig2.png" width="250"></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size:12px;">
The Universe at t=380,000,000 yr. (ESA and Planck Collaboration)
<a href="https://en.wikipedia.org/wiki/Cosmic_microwave_background">learn
more</a>
</figcaption>
</figure>
[learn more](https://en.wikipedia.org/wiki/Cosmic_microwave_background)

## Growing Galaxies

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig3.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size:12px;">
Simplified diagram showing hierarchical assembly of galaxies starting from small fluctuations in the density distribution of the early universe.
(Australia Telescope National Facility)
</figcaption>
Expand All @@ -70,9 +68,8 @@ assembly of thousands of protogalaxies which are much smaller.
## Observing the First Galaxies

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig4.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
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)
Expand All @@ -93,9 +90,8 @@ galaxies.
## Faint Red Blobs at the Edge of the Universe

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig5.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
Composite of high redshift galaxies imaged by the Hubble Space Telescope. The galaxies appear red due to cosmological redshift. (Space Telescope Science Institute)
</figcaption>
</figure>
Expand All @@ -108,17 +104,22 @@ 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).
<br />
<br />
<br />
<br />
<br />

# How we use supercomputers to study the first galaxies

Before we delve into how we use supercomputers to study the first galaxies, we need
to cover some basics.

## Supercomputers

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig6.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
The Blue Waters Sustained Petascale Supercomputer at the University of Illinois, Urbana-Champaign.
(M. Norman, UCSD)
</figcaption>
Expand All @@ -129,12 +130,16 @@ 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)
<br />
<br />
<br />
<br />

## Parallel computing

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig7.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
Parallel computing subdivides the problem domain into many smaller domains, which are
calculated simulateneously on many processors of a supercomputer. (M. Norman, UCSD)
</figcaption>
Expand All @@ -148,12 +153,16 @@ 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)
<br />
<br />
<br />
<br />

## Coping with an infinite universe

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig8.jpg" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
Simulation of cosmic structure is performed in a cubic volume assuming periodic boundary conditions
in all 3 directions. (G. Bryan, Columbia & M. Norman, UCSD)
</figcaption>
Expand All @@ -172,9 +181,8 @@ the box we are simulating.
## Coping with an expanding universe

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig9.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
The expansion of the universe is removed from the simulation through the comoving coordinate transformation.
(M. Norman, UCSD)
</figcaption>
Expand All @@ -190,9 +198,8 @@ exactly the rate of the expanding universe. We say we simulate a co-moving volum

## Initializing the simulation
<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig10.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
Matter fluctuations consistent with CMB measurements are used to initialize the
cosmology simulation. (M. Norman, UCSD)
</figcaption>
Expand All @@ -210,9 +217,8 @@ we are able to adjust the amplitude accordingly, however the power spectrum rema

## Computing what happens next
<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig11.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
The matter fluctuations grow in amplitude, forming the characteristic cosmic web
large scale structure of the universe. (M. Norman, UCSD)
</figcaption>
Expand All @@ -226,9 +232,8 @@ you want to simulate, and how finely resolved the simulation is. [learn more](ht

## What physical laws are programmed?
<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/fig12.png" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
<figcaption style="display: table-caption; caption-side: bottom; font-size: 12px;">
Equations of cosmological hydrodynamics.
(M. Norman, UCSD)
</figcaption>
Expand Down
48 changes: 25 additions & 23 deletions showcase.md
View file
Open in desktop
Original file line number Diff line number Diff line change
Expand Up @@ -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

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/RSimg1.PNG" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
Expand All @@ -33,32 +32,32 @@ 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg2.PNG" width="320" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
</figure>

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.
<br /><br /><br /><br />
<br /><br /><br /><br />
<br /><br /><br /><br />

### 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

<figure style="display: table; float: right; margin: 0 0 20px 20px;">
<a href="somewhere">
<img src="images/RSimg3.PNG" width="320" style="float: right;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
</figure>

[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.
<br /><br /><br /><br />
<br /><br />

### 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg4.PNG" width="320" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
Expand All @@ -69,19 +68,20 @@ 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg5.PNG" width="320" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
</figure>10
</figure>

[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.
<br />
<br />

### 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg6.PNG" width="320" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
Expand All @@ -92,56 +92,58 @@ 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg7.PNG" width="320" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
</figure>

[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.
<br /><br />

### 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg8.PNG" width="320" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
</figure>

[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).
<br /><br /><br /><br />
<br /><br />

### 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg9.PNG" width="320" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
</figure>

[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.
<br /><br /><br /><br />
<br /><br />

### 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg10.PNG" width="240" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
</figure>

[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.
<br /><br /><br /><br />
<br /><br />

### 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

<figure style="display: table; float: left; margin: 0 0 20px 20px;">
<a href="somewhere">
<figure style="display: table; float: left; margin: 0 20px 20px 20px;">
<img src="images/RSimg11.PNG" width="240" style="float: left;"/></a>
<figcaption style="display: table-caption; caption-side: bottom;">
</figcaption>
Expand Down