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Expand Up @@ -16,26 +16,61 @@ <h4 class="heading-heading">AGORA Simulations</h4>
<h4>Project summary</h4>
<p>
The
<a class="underline" target="_blank" rel="noopener" href="https://sites.google.com/site/santacruzcomparisonproject/"
>AGORA High-resolution Galaxy Simulations Comparison Project </a
> investigates galaxy formation with high-resolution simulations and compares the results across code platforms and with observations. The goal is to verify that the astrophysical assumptions are responsible for any success in galaxy simulations, not artifacts of particular numerical implementations. By guaranteeing reproducibility, we aim to improve numerical experiments as one of the most powerful tools in formulating theories of galaxy formation. This is a one-of-a-kind, inter-institutional effort by more than 160 participants from over 60 institutions worldwide. We welcome anybody who is interested in participating in the AGORA project, especially with new codes.
<a
class="underline"
target="_blank"
rel="noopener"
href="https://sites.google.com/site/santacruzcomparisonproject/"
>AGORA High-resolution Galaxy Simulations Comparison Project</a
>
investigates galaxy formation with high-resolution simulations and
compares the results across code platforms and with observations.
The goal is to verify that the astrophysical assumptions are
responsible for any success in galaxy simulations, not artifacts
of particular numerical implementations. By guaranteeing
reproducibility, we aim to improve numerical experiments as one of
the most powerful tools in formulating theories of galaxy
formation. This is a one-of-a-kind, inter-institutional effort by
more than 160 participants from over 60 institutions worldwide. We
welcome anybody who is interested in participating in the AGORA
project, especially with new codes.
</p>
<p>The AGORA infrastructure include common cosmological initial conditions (4 halo masses and 2 assembly histories generated using MUSIC), common isolated initial conditions (generated with MakeDisk), common astrophysics models (cooling and UV background implemented via the GRACKLE package), and a common analysis platform (yt toolkit), all publicly available to the community. Using the components assembled, the ongoing collaborative efforts aim to increase the realism of numerical experiments collectively, resulting in multiple publications in the next few years. </p>
<p>The data are available <a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/~chayward/agora_public_release/"
>here</a>.
<p>
The AGORA infrastructure include common cosmological initial
conditions (4 halo masses and 2 assembly histories generated using
MUSIC), common isolated initial conditions (generated with
MakeDisk), common astrophysics models (cooling and UV background
implemented via the GRACKLE package), and a common analysis
platform (yt toolkit), all publicly available to the community.
Using the components assembled, the ongoing collaborative efforts
aim to increase the realism of numerical experiments collectively,
resulting in multiple publications in the next few years.
</p>
<p>
The data are available
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/~chayward/agora_public_release/"
>here</a
>.
</p>
<p>For more information about the project, the simulation data, or the infrastructures assembled, please visit the <a
class="underline"
target="_blank"
rel="noopener"
href="https://sites.google.com/site/santacruzcomparisonproject/"
>AGORA homepage.</a>
<p>
For more information about the project, the simulation data, or
the infrastructures assembled, please visit the
<a
class="underline"
target="_blank"
rel="noopener"
href="https://sites.google.com/site/santacruzcomparisonproject/"
>AGORA homepage</a
>.
</p>
<p>
Any publication using these data should cite the relevant paper(s)
linked below:
</p>
<p>Any publication using these data should cite the relevant paper(s) linked below:</p>
<ul>
<li>
Paper I - AGORA rationale and dark matter-only comparison:
Expand All @@ -45,7 +80,7 @@ <h4>Project summary</h4>
rel="noopener"
href="https://ui.adsabs.harvard.edu/abs/2014ApJS..210...14K/abstract"
>Kim et al. (2014)</a
>
>
</li>
<li>
Paper II - isolated disk comparison:
Expand All @@ -55,17 +90,17 @@ <h4>Project summary</h4>
rel="noopener"
href="https://ui.adsabs.harvard.edu/abs/2016ApJ...833..202K/abstract"
>Kim et al. (2016)</a
>
>
</li>
<li>
Paper II public data release:
Paper II - public data release:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://arxiv.org/abs/2001.04354"
>Roca-Fabrega et al. (2020)</a
>
>
</li>
<li>
Paper III - cosmological comparison:
Expand All @@ -75,13 +110,231 @@ <h4>Project summary</h4>
rel="noopener"
href="https://ui.adsabs.harvard.edu/abs/2021ApJ...917...64R/abstract"
>Roca-Fabrega et al. (2021)</a
>
>
</li>
<li>
Paper IV - Cosmological comparison at Low redshift + merger
trees:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://arxiv.org/abs/2402.06202"
>Roca-Fabrega et al. (2024)</a
>
</li>
</ul>
<p>
The data from Paper II, III and IV are publicly available and can
be found
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/~chayward/agora_public_release/"
>here</a
>. All the CosmoRun data saved in more than 300 fine time steps,
will be available soon.
</p>
<h5>Paper IV data structure</h5>
<p>
The Paper IV Data Release note with full information about how to
find and download the simulations snapshots and the metadata can
be found
<a
class="underline"
target="_blank"
rel="noopener"
href="https://arxiv.org/pdf/2408.00432"
>here</a
>. In the released data, we include 14 snapshots from each code at
the integer redshifts between 15 and 2, plus the ones at z=1 and
0, when available. You can find the snapshot number (included in
the snapshot filename) corresponding to each specific redshift in
the following table:
</p>
<img
src="/web/assets/agora-table.png"
style="display: block; max-width: 100%; width: 1200px"
/>
<ul>
<li>
i:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/ART-I/"
>ART-I</a
>
</li>
<li>
ii:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/ENZO/"
>ENZO</a
>
</li>
<li>
iii:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/RAMSES/"
>RAMSES</a
>
</li>
<li>
iv:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/CHANGA/SB/output/"
>CHANGA</a
>
</li>
<li>
v:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/CHANGA/nSB/output/"
>CHANGA-T</a
>
</li>
<li>
vi:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/GADGET3/"
>GADGET-3</a
>
</li>
<li>
vii:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/GEAR/"
>GEAR</a
>
</li>
<li>
viii:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/AREPO/"
>AREPO-T</a
>
</li>
<li>
ix:
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/∼chayward/agora_public_release/PaperIV/GIZMO/"
>GIZMO</a
>
</li>
</ul>
<p>The data from Paper II and III are publicly available and can be found <a class="underline" target="_blank" rel="noopener" href="https://users.flatironinstitute.org/~chayward/agora_public_release/" >here.</a> The CosmoRun data down to z=2, saved in fine time steps, will be available soon.</p>
<p>
Together with the snapshots data we also released several metadata
files. These files are located in the metadata folder you can find
<a
class="underline"
target="_blank"
rel="noopener"
href="https://users.flatironinstitute.org/~chayward/agora_public_release/PaperIV/Metadata/"
>here</a
>
and contains the following three files and a subfolder:
</p>

<ul>
<li>
centers_CODE_final_noID.txt: This file contains the centers of
the main halo inside the simulated cosmological box in physical
kiloparsecs. The data is structured as follows: redshift,
snapnum (see Table 2), [x,y,z].
</li>
<li>
Rvir_cent_CODE.txt: This file contains similar information to
the previous one but in a simpler format, including information
on the R200c. The data is structured as follows: redshift,
snapnum (see Table 2), x, y, z, R200c (in physical kpc).
</li>
<li>
Rvir_cent_others_CODE.txt: This file contains information about
many general properties of the central halo. The data is
structured as follows: redshift, snapnum (see Table 2), R200c
[kpc], M200c [M⊙], M⊙(R&lt;R200c) [M⊙], M⊙,gal(R&lt; 0.15R200c)
[M⊙], R1/2 [kpc], Mtot(R&lt;R1/2 ) [M⊙], Z⊙ [Z⊙], R1/2⊙,gal
[kpc], M⊙,gal(R&lt;R1/2⊙ ) [M⊙], Z⊙,gal [Z⊙].
</li>
<li>
MERGERTREES_ROCKSTAR: In this folder you will find a sub-folder
containing the merger for each one of the participant codes
<strong>except</strong> for the fiducial CHANGA
(CHANGA_3.5e51erg_SB), generated using rockstar (<a
class="underline"
target="_blank"
rel="noopener"
href="https://ui.adsabs.harvard.edu/abs/2013ApJ...762..109B/abstract"
>Behroozi et al. 2013a</a
>) and consistent-trees (<a
class="underline"
target="_blank"
rel="noopener"
href="https://ui.adsabs.harvard.edu/abs/2013ApJ...763...18B/abstract"
>Behroozi et al. 2013b</a
>). The files can be read and analysed using the
<a
class="underline"
target="_blank"
rel="noopener"
href="https://ytree.readthedocs.io/en/latest/"
>ytree</a
>
tool provided by the
<a
class="underline"
target="_blank"
rel="noopener"
href="https://yt-project.org/"
>yt</a
>
community.
</li>
</ul>
<p>
All metadata filenames include the name of the corresponding code
plus some small variations indicating its content.
</p>
<p>
WARNING: Because the CHANGA fiducial (CHANGA_3.5e51erg_SB) merger
trees are not yet available, we provide the CHANGA-T
(CHANGA_6.0e51erg_NSB) ones instead. Although this can give a
first guess of the center of all subhalos and of the central halo,
we recommend the users to make additional checks and to apply a
re-centering routine before using the data (e.g. centering at the
center of mass in a sphere centered at the center provided in the
merger tree catalog).
</p>
</div>
</div>
</div>
</div>
</div>
</div>
</div>
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